DRSP 1.1.1 Title Unbiased survey of submm galaxies: continuum survey at 1 mm Pi S.Guilloteau Time 80 hrs 1.1.1: Name -- Unbiased survey of submm galaxies -- -- Part 1 -- Authors: S.Guilloteau 2. Science goal: -- (Generic Science Scope from C.Carilli) -- The discovery of the IR background, and the SCUBA/MAMBO population of dusty, star forming galaxies at high redshift, has transformed our understanding of galaxy formation. It is now clear that a significant fraction (of order 50%) of star formation in the cosmos occurs in galaxies that are heavily obscured by dust, and that this fraction may rise with redshift, possibly corresponding to the formation of spheroidal galaxies in active starbursts. One highly uncertain aspect of the study of submm galaxies is their redshift distribution. Optical redshifts remain problematic for the majority of such sources, and can be misleading due to possible mis-identifications. -- (specific part) An important way to study the history of galaxy formation is to perform an unbiased redshift survey. We propose a unbiased, high sensitivity survey over a 4x4' area of the sky. This survey consists in a 4 main parts, and 2 or 3 complementary observations which are discussed in separate proposals: - Part 1) Continuum survey at 1 mm to reach 0.1 mJy point source sensitivity at the 5 sigma level. - Part 2) Combined line and continuum survey at 3 mm, down to 7.5 microJy at the 5 sigma level. - Part 3) Pointed continuum survey at 650 GHz towards sources detected in Part 1), down to 0.4 mJy at the 5 sigma level - Part 4) Line survey of the 210-275 GHz frequency band, down to 50 microJy for the 8 GHz bandwidth, with some angular resolution (0.4") in order to provide dynamical masses and lens corrections for the detectable sources. The fraction of sources found in Part 1 to be detected in Part 4 is unknown, but should be high (perhaps 50 -- 80 %). The complementary observations include: high resolution imaging to identify lenses and derive dynamical masses, and observations of other lines such as HCN or CI. This proposal covers Part 1). Continuum surveys made by large bolometer cameras will cover much wider fields of view, but will most likely be sensitivity limited to a level at least 5 to 10 times above the proposed ALMA survey. ALMA will explore a range of star formation rates much lower than those of currently detected sub-mm sources. With a proposed sensitivity level of 0.1 mJy, the survey should be able to find between 100 and 300 continuum sources, depending on the applicable cosmological model. 30 to 90 sources are expected to be brighter than 0.4 mJy. 3. Number of sources: 1 field of 4x4' 4. Coordinates: 4.1. Any 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 1" 5.2. Range of spatial scales/FOV: 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 7 -- 290 GHz 6.2. Lines and Frequencies Continuum only 6.3. Spectral Resolution (km/s) (coarse) 6.4. Bandwidth or spectral coverage: 8 GHz (for search) 7. Continuum flux density: 7.1. Typical value: 0.1 - 1 mJy 7.2. Continuum peak value: 2-5 mJy 7.3. Required continuum rms: 20 microJy 7.4. Dynamic range in image: < 100:1 8. Line intensity: 8.1. Typical value: 8.2. Required rms per channel: 8.3. Spectral dynamic range: 9. Polarization: no 10. Integration time per setting: Mosaic of 140 pointings, 30 minutes per pointing center. 11. Total integration time for program: Part 1): 80 hours ********************************************************************** Review Pierre Cox: this programme in four parts proposes to explore a 4x4 arcmin^2 field in order to study the submm galaxy population in both the dust and line emission. A few 100-300 sources will be detected providing a census of the population together with first indications on their properties (redshifts, infrared luminosities, gas excitation, and dynamical masses). The time estimates are correct and the overall strategy is robust. Note that in 1.1.2, the current CO detections of submm galaxies indicate that the CO fluxes are about 1-2 Jy km/s for 1.3 mm continuum flux densities of 1-3 mJy rather than the 5-10 mJy which are indicated and which correspond to the 850 microns flux densities. Also at the expected sensitivities, one could perhaps start to detect species other than CO such as HCN which is typically 10 times weaker than CO. -------------------------------------------------- Review v2.0: 1.1.1 We may have to require about 43 min integration per pointing center in order to achieve 20 microJy rms if we assume the number of antenna is 50. The total integration time for this program (1.1.1) will be 100 hours or so. Note that the selection of target 4'x4' field is a very essential issue for this program, considering the effect of ``cosmic variance''. ===================================================================================== DRSP 1.1.2 Title Unbiased survey of submm galaxies: combined line+cont at 3 mm Pi S.Guilloteau Time 256 hrs 1.1.2: Name -- Unbiased survey of submm galaxies -- -- Part 2 -- Authors: S.Guilloteau 2. Science goal: -- (Generic Science Scope from C.Carilli) -- The discovery of the IR background, and the SCUBA/MAMBO population of dusty, star forming galaxies at high redshift, has transformed our understanding of galaxy formation. It is now clear that a significant fraction (of order 50%) of star formation in the cosmos occurs in galaxies that are heavily obscured by dust, and that this fraction may rise with redshift, possibly corresponding to the formation of spheroidal galaxies in active starbursts. One highly uncertain aspect of the study of submm galaxies is their redshift distribution. Optical redshifts remain problematic for the majority of such sources, and can be misleading due to possible mis-identifications. -- (specific part) An important way to study the history of galaxy formation is to perform an unbiased redshift survey. We propose a unbiased, high sensitivity survey over a 4x4' area of the sky. This survey consists in a 4 main parts, and 2 or 3 complementary observations which are discussed in separate proposals: - Part 1) Continuum survey at 1 mm to reach 0.1 mJy point source sensitivity at the 5 sigma level. - Part 2) Combined line and continuum survey at 3 mm, down to 7.5 microJy at the 5 sigma level. - Part 3) Pointed continuum survey at 650 GHz towards sources detected in Part 1), down to 0.4 mJy at the 5 sigma level - Part 4) Line survey of the 210-275 GHz frequency band, down to 50 microJy for the 8 GHz bandwidth, with some angular resolution (0.4") in order to provide dynamical masses and lens corrections for the detectable sources. The fraction of sources found in Part 1 to be detected in Part 4 is unknown, but should be high (perhaps 50 -- 80 %). The complementary observations include: higher resolution imaging for better lens models, and better derivation of dynamical masses, and observations of other lines such as HCN or CI. This proposal covers Part 2). In Part 2), we propose to cover completely in space the same area as covered in Part 1), and in frequency the range 84 to 116 GHz. The frequency coverage can be done in 4 tunings of the Band 3 receivers, although the details depend on the final choice of receivers for Band 3. We propose to achieve a continuum sensitivity (averaged over the total 32 GHz) of 7.5 microJy at 5 sigma all over the 4x4' field. Such a field requires about 16 pointings (slightly less at 84 GHz, slightly more at 116 GHz). At 90 GHz, an integration time of 12 hours per pointing is required to reach this sensitivity level, leading to a total time of 8 days to perform the program. Given the degraded sensitivity at 84 GHz (receiver) and 115 GHz (atmospheric oxygen), Part 2 can be completed in about 10 days. With a typical spectral index of 2-3 for the dust emission between 3 mm and 1 mm, depending on the source redshift, sources detected in Part 1 at the 0.2 mJy level will have a 3 mm continuum flux between 8 and 23 microJy. The continuum sensitivity is thus sufficient to allow detection of all these sources at 3 mm as well, and to provide a first order information on the redshift by the determination of the spectral index. For a spectral resolution of 50 km/s, the corresponding line sensitivity is 70 microJy (taking into account the 4 times smaller integration time for each receiver tuning). For typical linewidths of 300 km/s, the integrated line flux sensitivity is thus 0.04 Jy.km/s (at 5 sigma). Current (as of July 2003) detection of CO in sub-mm galaxies indicate an integrated line flux at 3 mm of order 1 to 2 Jy.km/s for sources of about 5 to 10 mJy continuum flux at 1 mm. As for the 3 mm continuum, the 5 sigma sensitivity is sufficient to detect in CO all continuum sources detected above 0.2 mJy in Part 1). In detected sources, there will be at least one CO line for sources with z>2, and two for sources with z>6. The are two blind redshift regions: 0.4 -- 1, and 1.7 -- 2.0. The survey thus provides a good coverage of the star formation history for redshifts above 1. 3. Number of sources: 1 field of 4x4' 4. Coordinates: 4.1. Any 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 3" 5.2. Range of spatial scales/FOV: scales < 1", FOV 4x4' 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 -- 84 -- 116 GHz 6.2. Lines and Frequencies 4 tunings for complete band coverage 6.3. Spectral Resolution (km/s) 50 6.4. Bandwidth or spectral coverage: 8 GHz per tuning 7. Continuum flux density: 7.1. Typical value: 0.01 - 0.1 mJy 7.2. Continuum peak value: 0.2 mJy 7.3. Required continuum rms: 1.5 microJy 7.4. Dynamic range in image: < 100:1 8. Line intensity: 8.1. Typical value: 8.2. Required rms per channel: 14 microJy 8.3. Spectral dynamic range: < 30:1 9. Polarization: no 10. Integration time per setting: Mosaic of 16 pointings, 4 hours per pointing center and per tuning, 4 tunings. 11. Total integration time for program: Part 2): 256 hours ************************************************************************ Review Pierre Cox: this programme in four parts proposes to explore a 4x4 arcmin^2 field in order to study the submm galaxy population in both the dust and line emission. A few 100-300 sources will be detected providing a census of the population together with first indications on their properties (redshifts, infrared luminosities, gas excitation, and dynamical masses). The time estimates are correct and the overall strategy is robust. Note that in 1.1.2, the current CO detections of submm galaxies indicate that the CO fluxes are about 1-2 Jy km/s for 1.3 mm continuum flux densities of 1-3 mJy rather than the 5-10 mJy which are indicated and which correspond to the 850 microns flux densities. Also at the expected sensitivities, on could perhaps start to detect species other than CO such as HCN which is typically 10 times weaker than CO. -------------------------------------------------- Review v2.0: 1.1.2 Time estimation was checked. Note that "14 microJy" stated in 8.2. Required rms per channel seems to be 70 microJy. ===================================================================================== DRSP 1.1.3 Title Unbiased survey of submm galaxies: pointed cont. at 650 GHz Pi S.Guilloteau Time 150-450 hrs 1.1.3: Name -- Unbiased survey of submm galaxies -- -- Part 3 -- Authors: S.Guilloteau / C. Carilli -- (Generic Science Scope from C.Carilli) -- The discovery of the IR background, and the SCUBA/MAMBO population of dusty, star forming galaxies at high redshift, has transformed our understanding of galaxy formation. It is now clear that a significant fraction (of order 50%) of star formation in the cosmos occurs in galaxies that are heavily obscured by dust, and that this fraction may rise with redshift, possibly corresponding to the formation of spheroidal galaxies in active starbursts. One highly uncertain aspect of the study of submm galaxies is their redshift distribution. Optical redshifts remain problematic for the majority of such sources, and can be misleading due to possible mis-identifications. -- (specific part) An important way to study the history of galaxy formation is to perform an unbiased redshift survey. We propose a unbiased, high sensitivity survey over a 4x4' area of the sky. This survey consists in a 4 main parts, and 2 or 3 complementary observations which are discussed in separate proposals: - Part 1) Continuum survey at 1 mm to reach 0.1 mJy point source sensitivity at the 5 sigma level. - Part 2) Combined line and continuum survey at 3 mm, down to 7.5 microJy at the 5 sigma level. - Part 3) Pointed continuum survey at 650 GHz towards sources detected in Part 1), down to 0.4 mJy at the 5 sigma level - Part 4) Line survey of the 210-275 GHz frequency band, down to 50 microJy for the 8 GHz bandwidth, with some angular resolution (0.4") in order to provide dynamical masses and lens corrections for the detectable sources. The fraction of sources found in Part 1 to be detected in Part 4 is unknown, but should be high (perhaps 50 -- 80 %). The complementary observations include: high resolution imaging to identify lenses and derive dynamical masses, and observations of other lines such as HCN or CI. This proposal covers Part 3. In Part 3, we propose to observe at 670 GHz all sources detected in Part 1 down to a 5 sigma sensitivity of 0.55 mJy per beam. Such a sensitivity requires about 90 minutes per pointing. Since 100 to 300 sources are expected to be detected in Part 1, the total time for Part 3 is 6 to 18 days. With this sensitivity, the weakest sources detected in Part 1 will be detected in Part 3 if the spectral index of the emission is greater than 2. In Part 3, we shall thus easily detect the low redshift sources, while the faintest and highest redshift objects may not be visible at 670 GHz. 3. Number of sources: 100 to 300 4. Coordinates: 4.1. Any 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.5" 5.2. Range of spatial scales/FOV: scales < 1" 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 9 -- 670 GHz 6.2. Lines and Frequencies 670 GHz, continuum only 6.3. Spectral Resolution (km/s) 6.4. Bandwidth or spectral coverage: 8 GHz 7. Continuum flux density: 7.1. Typical value: 0.5 - 5 mJy 7.2. Continuum peak value: 10 mJy 7.3. Required continuum rms: 0.1 mJy 7.4. Dynamic range in image: < 50:1 8. Line intensity: 8.1. Typical value: 8.2. Required rms per channel: 8.3. Spectral dynamic range: 9. Polarization: no 10. Integration time per setting: 1.5 hours per pointing center 11. Total integration time for program: Part 3): 150 -- 450 hours *************************************************************************** Review Pierre Cox: this programme in four parts proposes to explore a 4x4 arcmin^2 field in order to study the submm galaxy population in both the dust and line emission. A few 100-300 sources will be detected providing a census of the population together with first indications on their properties (redshifts, infrared luminosities, gas excitation, and dynamical masses). The time estimates are correct and the overall strategy is robust. Note that in 1.1.2, the current CO detections of submm galaxies indicate that the CO fluxes are about 1-2 Jy km/s for 1.3 mm continuum flux densities of 1-3 mJy rather than the 5-10 mJy which are indicated and which correspond to the 850 microns flux densities. Also at the expected sensitivities, one could perhaps start to detect species other than CO such as HCN which is typically 10 times weaker than CO. -------------------------------------------------- Review v2.0: 1.1.3 To achieve a continuum sensitivity of 0.1 mJy rms, we may need 2.5 hours per pointing. The net integration time will be increased accordingly. ===================================================================================== DRSP 1.1.4 Title Unbiased survey of submm galaxies: line survey 210-275 GHz Pi S.Guilloteau Time 180 hrs 1.1.4: Name -- Unbiased survey of submm galaxies -- -- Part 4 -- Authors: S.Guilloteau 2. Science goal: -- (Generic Science Scope from C.Carilli) -- The discovery of the IR background, and the SCUBA/MAMBO population of dusty, star forming galaxies at high redshift, has transformed our understanding of galaxy formation. It is now clear that a significant fraction (of order 50%) of star formation in the cosmos occurs in galaxies that are heavily obscured by dust, and that this fraction may rise with redshift, possibly corresponding to the formation of spheroidal galaxies in active starbursts. One highly uncertain aspect of the study of submm galaxies is their redshift distribution. Optical redshifts remain problematic for the majority of such sources, and can be misleading due to possible mis-identifications. -- (specific part) An important way to study the history of galaxy formation is to perform an unbiased redshift survey. We propose a unbiased, high sensitivity survey over a 4x4' area of the sky. This survey consists in a 4 main parts, and 2 or 3 complementary observations which are discussed in separate proposals: - Part 1) Continuum survey at 1 mm to reach 0.1 mJy point source sensitivity at the 5 sigma level. - Part 2) Combined line and continuum survey at 3 mm, down to 7.5 microJy at the 5 sigma level. - Part 3) Pointed continuum survey at 650 GHz towards sources detected in Part 1), down to 0.4 mJy at the 5 sigma level - Part 4) Line survey of the 210-275 GHz frequency band, down to 50 microJy for the 8 GHz bandwidth, with some angular resolution (0.4") in order to provide dynamical masses and lens corrections for the detectable sources. The fraction of sources found in Part 1 to be detected in Part 4 is unknown, but should be high (perhaps 50 -- 80 %). The complementary observations include: high resolution imaging to identify lenses and derive dynamical masses, and observations of other lines such as HCN or CI. This proposal covers Part 4). In Part 4), we propose to cover completely in space the same area as covered in Part 1), and in frequency the range 210 to 274 GHz. The frequency coverage can be done in 8 tunings of the Band 6 receivers. We propose to achieve a continuum sensitivity (averaged over the total 64 GHz) of 50 microJy at 5 sigma all over the 4x4' field. Such a field requires about 90 pointings at each frequency tuning (70 at 210 GHz, 110 at 270 GHz). An integration time of 2 hours per pointing (all tunings included) is required to reach this sensitivity level, leading to a total time of 8 days to perform the program. The continuum part of this survey duplicates Part 1: all sources detected in Part 1 will be detected in Part 4. However, Part 4 also allows detection of the CO lines from the sources. Because of the overlap with Part 1, it is conceivable to perform Part 4 with some angular resolution. For this excercise, we assume an angular resolution of 0.4", already better than that of the best images obtained today (July 2003). The continuum brightness sensitivity corresponds to 1 mK (1 sigma) at this angular resolution. Statistics on the strength of the CO lines redshifted to such frequencies are still too scarce to predict a detection rate. The brightness sensitivity of the instrument is then 0.05 K (1 sigma) for 50 km/s resolution. This is well below the typical line strength of CO in nearby galaxies. Even accounting for additional beam dilution, we would thus expect a large number of detections. The highest redshift objects may escape detection, since the high J CO lines may no longer be significantly excited. Conducted as such, Part 4 would allow to obtain sizes of most (but probably not all) of the sources detected in Part 1, as well as dynamical masses for the brighter objects. Lensing correction for the brightest sources may also be possible, as the angular resolution will help in building a first order lens model for the brightest sources. 3. Number of sources: 4. Coordinates: 4.1. Any 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.4" 5.2. Range of spatial scales/FOV: scales < 1" , FOV 4x4' 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 6 -- 210 to 274 GHz 6.2. Lines and Frequencies 8 adjacent tunings 6.3. Spectral Resolution (km/s) 50 6.4. Bandwidth or spectral coverage: 8 GHz 7. Continuum flux density: 7.1. Typical value: 0.05 - 2 mJy 7.2. Continuum peak value: 4 mJy 7.3. Required continuum rms: 0.01 mJy 7.4. Dynamic range in image: < 100:1 8. Line intensity: 8.1. Typical value: 8.2. Required rms per channel: 8.3. Spectral dynamic range: 9. Polarization: no 10. Integration time per setting: 2 hours per pointing center, shared between 8 tunings, 90 pointings 11. Total integration time for program: Part 4): 180 hours ************************************************************************ Review Pierre Cox: this programme in four parts proposes to explore a 4x4 arcmin^2 field in order to study the submm galaxy population in both the dust and line emission. A few 100-300 sources will be detected providing a census of the population together with first indications on their properties (redshifts, infrared luminosities, gas excitation, and dynamical masses). The time estimates are correct and the overall strategy is robust. Note that in 1.1.2, the current CO detections of submm galaxies indicate that the CO fluxes are about 1-2 Jy km/s for 1.3 mm continuum flux densities of 1-3 mJy rather than the 5-10 mJy which are indicated and which correspond to the 850 microns flux densities. Also at the expected sensitivities, one could perhaps start to detect species other than CO such as HCN which is typically 10 times weaker than CO. -------------------------------------------------- Review v2.0: 1.1.4 Recent exciting reports on the detections of redshifted [CII] 158um emission suggest that this program will allow us to detect CII from many of sources, if there are any SMGs lying in the redshift range of 6 to 8. A minor revision on the time estimation. If 2 hours integration will be shared by 8 tunings (i.e., 900 sec for each setup), a line sensitivity (rms) of 0.5 mJy per 50 km/s channel (or 0.07 K for 0".4 resolution) will be achieved. About 2000 sec integration will be required to achieve 0.05 K rms, which is stated in the text. The total integration time for this program will be around 400 hours in this case. ===================================================================================== DRSP 1.1.5 Title Molecular line studies of submm galaxies --constraining dust obscured galaxy formation Pi C. Carilli Time 170 hrs 1.1.5: Name -- Molecular line studies of submm galaxies -- constraining dust obscured galaxy formation Authors: C. Carilli 2. Science goal: The discovery of the IR background, and the SCUBA/MAMBO population of dusty, star forming galaxies at high redshift, has transformed our understanding of galaxy formation. It is now clear that a significant fraction (of order 50%) of star formation in the cosmos occurs in galaxies that are heavily obscured by dust, and that this fraction may rise with redshift, possibly corresponding to the formation of spheroidal galaxies in active starbursts. One highly uncertain aspect of the study of submm galaxies is their redshift distribution. Optical redshifts remain problematic for the majority of such sources, and can be misleading due to possible mis-identifications. We propose a three part program -- (1) a 'blind' search for CO emission from a representative sample of submm galaxies to constrain their redshift distribution, (2) high resolution imaging of a sub-sample to determine the gas distribution and dynamics on sub-kpc scales and (ii) a search for HCN emission to search for dense gas directly associated with star formation. A representative sample of sources will be chosen from standard (sub)mm continuum surveys with large single dishes or by ALMA itself. Part 1: Redshift search -- I assume redshifts will be 'narrowed-down' via photometric techniques (optical and/or radio) to +/- 0.5 in dz, and that the typical source redshift is between 2 and 3. Using band 3 then requires 3 settings between 90 and 116 GHz to get the CO(3-2) line. This will take about 1hr per source (see below). A second search will then be required to look for higher/lower order transitions to confirm the redshift. This will take another hour. This second search will also give some indication of CO excitation conditions. I assume the characteristic line flux density is of order 1 mJy. Part 2: High resolution CO imaging -- I assume the characteristic source size is >= 1 kpc (0.2"), and intrinsic brightness temperature >= few K. Part 3: HCN emission is typically 10x fainter than CO. To get a 4 sigma detection will then take of order 10hrs/source. 3. Number of sources: 50 4. Coordinates: 4.1. Any 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: small configuration preferred - (1) and (3) A configuration for (2) 5.2. Range of spatial scales/FOV: 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 -- initial search, high res imaging, HCN search Band 6 -- 220 GHz follow-up for redshift verification 6.2. Lines and Frequencies CO, HCN at z=1 to 5, various transitions 6.3. Spectral Resolution (km/s) 100 km/s 6.4. Bandwidth or spectral coverage: 8 GHz (for search) 7. Continuum flux density: 7.1. Typical value: 1 mJy 7.2. Continuum peak value: 7.3. Required continuum rms: 7.4. Dynamic range in image: 8. Line intensity: 8.1. Typical value: 1 mJy -- CO(3-2), 0.1mJy -- HCN 8.2. Required rms per channel: 100 GHz -- 0.14 mJy (20min), 0.026mJy (10hrs) 220 GHz -- 0.2 mJy Imaging -- T_B = 0.25 K at 0.2" res in 1hr note: this corresponds to intrinsic T_B = 0.9 K (1sigma) at z=2.5 8.3. Spectral dynamic range: 9. Polarization: no 10. Integration time per setting: (1a) Search -- 1/3hr per setting x 3 settings x 50 srcs with band 3 = 50hr (1b) 1 hr/src for verification x 50 sources with band 3 or 6 = 50 hr (2) CO imaging -- 1hr/src x 20 srcs with band 3 = 20 hr (3) 10 hr/src for HCN search for 5 sources with band 3 = 50 hr 11. Total integration time for program: 170 ============================================================ Review Pierre Cox: This programme has essentially the same scientific goals has the previous programme, except that there is an explicit mention of HCN. So a slightly redundant. Not clear on what the selection of the 50 sources will be based, sources detected from bolometer surveys such as planned with APEX? The integration time is correct. Comment EvD: Keep this program in DRSP; no need to merge -------------------------------------------------- Review v2.0: 1.1.5 Redshift determination of optically dark SMGs using CO/CI/CII lines is one of the most important science objectives of the ALMA. Large samples of luminous southern SMGs will be provided by continuum camera mounted on APEX, ASTE, CCAT, and so on. Just a minor comment on the integration time; the required rms level (per channel) of 0.14 mJy and 0.026 mJy at 100 GHz will need 32 min and 16 hr, respectively, according to the current specification. It seems OK for 220 GHz estimation. The resultant total integration time is about 230 hours or so. Note that the 8 GHz band width of ALMA will enable us to observe both HCN and HCO+ lines simultaneously. They have comparable intensities and are indeed useful as tracers/diagnostics of dense ISM. ===================================================================================== DRSP 1.1.6 Title Ultradeep ALMA continuum survey Pi A. Blain Time 4120 hrs 1. Name of program and authors Ultradeep ALMA continuum survey Andrew Blain 2. One short paragraph with science goal(s) High-redshift dusty galaxies are known to be responsible for a reasonable fraction of the energy emitted by all galaxies over the history of the Universe. Only a large interferometer offers the opportunity to study more the brightest 10% of the population. In particular, ALMA has the capability to detect all other classes of distant galaxies detected at radio, optical and X-ray wavelengths to generate a unified picture of galaxy evolution. We propose: i) to cover the entire area of the GOODS-S field, to provide a link between different populations of galaxies selected at a range of wavelengths. ii) to probe deeper in the enclosed UDF region and in the separate HDFS field. iii) to make a small number of single images to the deepest possible level inside. Note that should not make blank field images shallower than about 0.15 mJy RMS, as these can be done using single-antenna telescopes, and interesting populations of optically-selected galaxies are known from stacking analyses to be detectable at this level. The number of detected sources, some with spectral line information will provide the first insight into the properties of sub-L* dusty galaxies at high redshifts, and to address their spatial and spectral relationships with the faintest galaxies detected at other wavelengths. The ultradeep fields could detect the very first dusty objects to form at any plausible redshifts up to 20, and certainly impose severe upper limits on the properties of the faintest, earliest metal-rich objects. 3. Number of sources (e.g., 1 deep field of 4'x4', 50 YSO's, 300 T Tauri stars with disks, ...; do NOT list individual sources or your "pet object", except in special cases like LMC, Cen A, HDFS) 1 deep field of 15'x10' (GOODS-S/UDF) 1 deeper sub-field of 3'x3' (UDF) 1 field of 2'x2' to the same depth as UDF (HDF-S) 1 field of 1.3' radius to the same depth as UDF (A370) 2 ultradeep+ single pointings: one in the UDF, and one in the most strongest magnified region of A370. 4. Coordinates: 4.1. Rough RA and DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 30 in Lupus) Indicate if there is significant clustering in a particular RA/DEC range (e.g., if objects in one particular RA range take 90% of the time) 03h 32m; -27 (GOODS) 22h 33m; -60 (HDF-S) 02h 23m; -01 (A370) Other deep fields could be possible, but these are the prime sites for deep surveys in the South. Other RA ranges can be filled by sparser observations of clusters of galaxies (see other proposals), which give ALMA a powerful boost using their gravitational lensing magnification. Also, COSMOS field at 10hr, -02deg is a good place to put a deep observation. At least one Ultradeep+ fields should be in the UDF to maximize multiwaveband coverage. 4.2. Moving target: yes/no (e.g. comet, planet, ...) No 4.3. Time critical: yes/no (e.g. SN, GRB, ...) No 4.4. Scheduling constraints: (optional) None 5. Spatial scales: 5.1. Angular resolution (arcsec): Angular resolution (arcsec): At least 0.1" to resolve galaxies 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) Moderate field mosaic to ensure smooth coverage; however, no targets are larger than a few arcsec. 5.3. Required pointing accuracy: (arcsec) 1", unless mosaic imposes greater requirement. 6. Observational setup 6.1. Single dish total power data: no/beneficial/required No Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no/beneficial/required No 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no/beneficial/required Possibly for increased depth if not required for other work 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no No 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9 6/7 7.2. Lines and Frequencies (GHz): (approximate; do _not_ go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify, e.g., "6 frequency settings in Band 3". Apply redshift correction yourself.) Top of band 6/bottom of band 7 - 280 GHz. Tunings at similar frequencies for all imaging, as 280-GHz is expected to lead to the detection of sources at the highest rate. May be sensible to shift tuning over several adjacent 8GHz ranges for imaging within each field to maximize the chances of serendipitous emission line detection. The decision on this should wait for a more concrete understanding of the range of emission properties of faint dusty galaxies, both to confirm the best frequency to search at, and the most efficient depth. 7.3. Spectral resolution (km/s): 300 km/s for serendipitous line detection 7.4. Bandwidth or spectral coverage (km/s or GHz): 8 GHz 8. Continuum flux density: 8.1. Typical value (Jy): (take average value of set of objects) (optional: provide range of fluxes for set of objects) Typical optical galaxies at 0.1mJy or less. Deep survey, so unknown 8.2. Required continuum rms (Jy or K): GOODS-S 0.02 mJy UDF/HDF-S/A370 0.004 mJy Ultradeep+ <0.001 mJy 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) No bright objects expected (brightest ~ 10mJy). 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) relative 10% 9. Line intensity: N/A 9.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10. Polarization: yes/no (optional) N/A 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): GOODS - 3800s per pointing, 1000 pointings = 1050 hours HDF-S - 96000s per pointing, 20 pointings = 530 hours A370 - 96000s per pointing, 20 pointings = 530 hours UDF - 96000s per pointing, 60 pointings = 1590 hours Ultradeep - a 0.001mJy RMS pointing takes 420 hours (single field assumed for total time calculation 12. Total integration time for program (hr): 4120 hours (long term can be used) 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): Should be an excellent first look at representative areas of sky using ALMA's deep imaging capability. Probably best to make a very deep subfield as early as possible to verify the system, produce headline science results, check the strategy by estimating the faint counts, and provide some objects at a wide range of fluxes for follow-up imaging at higher frequencies (in better weather?). The required atmospheric conditions will be determined by experience, but in principle, 280GHz observations could be done in the daytime and worse conditions, subject to the coherence being verfied to be acceptable under these conditions. Only ALMA can confirm the density of sources, but expect 20 sources per square arcmin at detection threshold of 0.1mJy and 80 per square arcmin at detection threshold of 0.02mJy: should get 3000 detections in GOODS-S field and 700 in UDF, matching reasonably well to the surface density of galaxies in the optical images. -------------------------------------------------- Review v2.0: 1.1.6 Sensitivity calculations were checked. In some of the proposed fields (close to the equator), we may have to check whether there are any nearby strong sources or not; if we go down to a microJy level; sidelobes from such a luminous (~ 10 - 100 mJy level) mm source could be problematic, although it is expected that the dynamic range will be high enough thanks to the huge number of antennas. ===================================================================================== DRSP 1.1.7 Title A deep search for line-emitting galaxies using ALMA Pi A. Blain Time 160 hrs 1. Name of program and authors A deep search for line-emitting galaxies using ALMA Andrew Blain 2. One short paragraph with science goal(s) So far, no galaxies have been discovered directly by their CO line emission. Only unusual catagories of distant galaxies: the brightest QSOs and most luminous dust-enshrouded galaxies have been detected. The properties of typical field galaxies in CO lines at even moderate redshifts is not currently known. ALMA has the sensitivity to search for their CO emission very efficiently, especially at longer wavelengths, where the fractional bandwidth is greatest. The 140-GHz band is likely to be most sensitive ultimately, but Band-3 can be used straightaway. Band-3 combines a wide primary beam, a large fractional bandwidth, availablility in the worst of observing conditions, and access to CO lines that have a high probability of excitation (CO(5-4) and lower) out to z=5. To a 5-sigma depth of 0.3mJy, a 300-km/s line can probably be detected every hour in a staring observation. Other CO lines can then be targetted in detected objects to confirm redshifts, and the continuum emission should be easy to detect alongside at higher frequencies. The equivalent widths of CO lines can be used to provide a redshift estimate from a single CO line. 3. Number of sources (e.g., 1 deep field of 4'x4', 50 YSO's, 300 T Tauri stars with disks, ...; do NOT list individual sources or your "pet object", except in special cases like LMC, Cen A, HDFS) Scans of fields covered in other deep surveys. Parts of sky very adaptable. 4. Coordinates: 4.1. Rough RA and DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 30 in Lupus) Indicate if there is significant clustering in a particular RA/DEC range (e.g., if objects in one particular RA range take 90% of the time) Could be widely spread. GOODS-S field at 02hr is an excellent candidate. Should target fields that have deep ALMA continuum imaging in preference to unobserved fields. 4.2. Moving target: yes/no (e.g. comet, planet, ...) No 4.3. Time critical: yes/no (e.g. SN, GRB, ...) No 4.4. Scheduling constraints: (optional) None 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" Modest for line detection 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) Single field 5.3. Required pointing accuracy: (arcsec) 1" 6. Observational setup 6.1. Single dish total power data: no/beneficial/required No Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no/beneficial/required No 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no/beneficial/required No 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no No 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9 Band 3 & 4: 4 tunings in each. If line detected then could cut bands to cover short - but likely not possible in real time. 7.2. Lines and Frequencies (GHz): (approximate; do _not_ go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify, e.g., "6 frequency settings in Band 3". Apply redshift correction yourself.) Redshifted CO(4-3)/CO(5-4). 4 settings in B3 and B4. 7.3. Spectral resolution (km/s): 300 7.4. Bandwidth or spectral coverage (km/s or GHz): 8GHz 8. Continuum flux density: 8.1. Typical value (Jy): (take average value of set of objects) (optional: provide range of fluxes for set of objects) Of order 0.1mJy 8.2. Required continuum rms (Jy or K): Of order 0.02mJy 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) Modest 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10% 9. Line intensity: 9.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) ~0.5 Jy km/s - in ~300 km/s line 9.2. Required rms per channel (K or Jy): 5-10-sigma, so 0.2mJy in 300 km/s 9.3. Spectral dynamic range: Modest 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10% 10. Polarization: yes/no (optional) No 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 360s per pointing, (~200 pointings at 90GHz to cover GOODS-S field) 12. Total integration time for program (hr): 200 pointings, 4 tunings, 2 bands, 8x200x360s = 57600s = 160 hours 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): Line surveys could be easily expanded/deepened. Expect about 2400 sources per square degree in a 24-GHz band at 5-sigma sensitivity of 0.3 Jy km/s, implies expect (150/3600)*2400 = 100 sources. The best strategy for line surveys is currently unclear, until the population of galaxies being probed is better quantified. Carrying out the survey at some of the settings, then reviewing and deciding whether to keep searching or follow up should bring down the total time by a factor of 2. The field will be contiguous, so calibrators and slewing will be quick and easy. Little retuning should be necessary until a substantial part of the field has been covered. Note that a z~1.2 redshift survey cannot be carried out any other way. -------------------------------------------------- Review v2.0: 1.1.7 Sensitivity calculation seems appropriate. ===================================================================================== DRSP 1.1.8 Title Follow-up observations of high-redshift submillimeter galaxies Pi A. Blain Time 5300 hrs 1. Name of program and authors Follow-up observations of high-redshift submillimeter galaxies Andrew Blain 2. One short paragraph with science goal(s) Since the first sensitive submm-wave surveys in 1997, a steadily increasing sample of high-redshift galaxies have been discovered, with 300-GHz flux densities of order 5mJy. There are currently about 600 of these galaxies known, and about 120 have redshifts mostly in the interval z=2-3. By the time ALMA operations begin, it is possible that 10,000 such galaxies may be known, with perhaps 1-2,000 redshifts. This depends on the success of single-antenna telescopes like JCMT/SCUBA-2, APEX and the 50-m LMT with wide-field bolometer array detectors. A handful have high-resolution mm-wave interferometer detections, showing emission resolved typically on the sub-arcsec scale, but there are so far no measurements close to the peak of the SED of these galaxies at about 100 microns. ALMA will provide multi-color spectral images of these galaxies longward of their SED peak to probe their astrophysics. Resolved images of these galaxies will provide valuable information about the relationship between optical and mm/submm morphology for the first time, providing details about the reprocessing of light in these galaxies, the temperature distribution of the dust, etc. Where redshifts are known, receiver tunings will be chosen to include CO lines in the ALMA bands if possible. 3. Number of sources (e.g., 1 deep field of 4'x4', 50 YSO's, 300 T Tauri stars with disks, ...; do NOT list individual sources or your "pet object", except in special cases like LMC, Cen A, HDFS) Of order 1000-2000 galaxies, spread over the sky. Many fields are currently in the North. Future fields will be equatorial, including COSMOS and follow-up of VLT-VIMOS redshift survey. This large number can be used to construct an accurate luminosity function, spanning the range of luminosities from typical galaxies to the most extreme systems, and rooting out the effects of gravitational lensing etc. However, some useful statistical information is available from a sample size as small as 300 targets, allowing a 10-bin luminosity function to be compiled. 4. Coordinates: 4.1. Rough RA and DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 30 in Lupus) Indicate if there is significant clustering in a particular RA/DEC range (e.g., if objects in one particular RA range take 90% of the time) Should be approximately uniform. 10hr equatorial field, 02hr southern fields are promising targets for APEX and LMT surveys accessible to ALMA. Could be bunching in the 02hr region, based on GOODS-S field. 4.2. Moving target: yes/no (e.g. comet, planet, ...) No 4.3. Time critical: yes/no (e.g. SN, GRB, ...) No 4.4. Scheduling constraints: (optional) Good weather required, 02hr and 10hr likely to most popular RA. 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.01"-1" 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) Single field in general, targeted at known object. 5.3. Required pointing accuracy: (arcsec) 1" 6. Observational setup 6.1. Single dish total power data: no/beneficial/required No Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no/beneficial/required No, unless standing idle for a bit more collecting area. 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no/beneficial/required Yes, if ACA used 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no No 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9 In principle all bands to provide excellent SED, but 3,6 and 9 should provide good continuum SED, with the best chance of detecting a CO line coming in 3, 4 & 6 where fractional bandwidth is greatest. Where CO/HCN will fall in band, at known redshift, want to observe there. 7.2. Lines and Frequencies (GHz): (approximate; do _not_ go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify, e.g., "6 frequency settings in Band 3". Apply redshift correction yourself.) Single setting in each band. Follow up may require more complex setups to hunt more unusual lines. 7.3. Spectral resolution (km/s): 100-300 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 8GHz, max continuum sensitivity. 8. Continuum flux density: 8.1. Typical value (Jy): (take average value of set of objects) (optional: provide range of fluxes for set of objects) For typical galaxy at z=2.5 or so: 90GHz ~0.08mJy 230GHz ~2mJy 350GHz ~5mJy 670GHz ~15mJy 8.2. Required continuum rms (Jy or K): Need to obtain high signal-to-noise resolved images to determine= detailed morphologies: implies at least 10-sigma detections: The most sensitive band in terms of signal to noise is Band 7, the highest resolution in any configuraion is expected in Band 9; therefore, the signal-to-noise ratio targets in these bands should be the greatest. 90GHz 5microJy 230GHz 0.05mJy 350GHz 0.05mJy 670GHz 0.1mJy 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) Small. 100-1000 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) Absolute 10%, relative band-to-band would like 5% for accurate SEDs. 9. Line intensity: Difficult to be sure, but in Band 3 there is a good chance that CO(3-2) can be detected for most sources, revealing internal dynamics and relative distributions of gas, dust and stars. 9.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) Few mJy over 300 km/s channel 9.2. Required rms per channel (K or Jy): See above, but set by continuum 9.3. Spectral dynamic range: N/A 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10. Polarization: yes/no (optional) No 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 90GHz 100min 230GHz 6min (at 280GHz only 10min for better S/N). 350GHz 367min 670GHz 167min => 640 minutes each 12. Total integration time for program (hr): 500 sources (estimated, most likely with redshifts) => 5300 hours total 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): Note that there are a wide variety of other point source targets for ALMA: optically-selected high-redshift Lyman-break galaxies (with ~0.1mJy at 350GHz); near-infrared-selected ERO galaxies (some of which are several mJy at 350GHz); galaxies detected by SIRTF (maybe 10,000,000 in the catalog). A key extra sample of galaxies are those detected by Planck Surveyor. There are likely to be several thousand of these (see additional proposal). I include an extra Planck Surveyor proposal, and I know there are high-redshift QSO proposals. I can certainly foresee at least comparable amounts of time being required to survey the field. One option to reduce time greatly would be to make a single survey at 230 GHz or 280 GHz first, and then to sift the results for follow up. This could reduce the time required by a factor of 10. -------------------------------------------------- Review v2.0: 1.1.8 I fully agree with the author's proposal; making a single band survey at 280 GHz first (500 sources * 10min for 0.05 mJy rms, i.e., 83 hrs), given the huge amount of requested time. Note that the sensitivity of 0.05 mJy rms at 350 GHz will be accomplished by about 30 min integration, not 367 min. Thus, proposed observations will require (100+6+30+167min) * 500 sources = 2500 hrs in total. ===================================================================================== DRSP 1.1.9 Title Dust in normal Lyman Break Galaxies Pi M. Sawicki Time 80 hrs 1. Name of program and authors Title: Dust in normal Lyman Break Galaxies. Author: Marcin Sawicki, marcin.sawicki@nrc.ca 2. One short paragraph with science goal(s) Star-formation rates and other properties of z~3 Lyman Break Galaxies (LBGs) remain only poorly constrained because of the poorly-understood starlight-absorbing interstellar dust that they contain. To properly understand the impact of dust, these objects must be observed in the rest-frame far-IR. Until now, however, normal LBGs were out of reach at these wavelengths and only one typical (but gravitationally lensed) LBG, MS1512-cB58, has been detected with SCUBA. We will use ALMA to obtain spatially unresolved continuum flux densities of 20 normal LBGs at 900 and 450um and use these data in combination with rest-frame optical, UV, and near-IR observations (in hand from HST and SIRTF) to map out the LBG spectral energy distributions over a wavelength range that spans dust both in absorption and in emission. These observations will allow us to constrain the properties of dust in emission such as its mass and temperature. 3. Number of sources: 20 4. Coordinates: 4.1. Rough RA and DEC all 20 in Southern GOODS field approximately at: R.A. = 03:32:27 Dec. = -27:48:31 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution (arcsec): ANY 5.2. Range of spatial scales/FOV (arcsec): individual point sources - one per field 5.3. Single dish total power data: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Bands 7 and 9 6.2. Lines and Frequencies (GHz): continuum 6.3. Spectral resolution (km/s): N/A 6.4. Bandwidth or spectral coverage (km/s or GHz): N/A 7. Continuum flux density: 7.1. Typical value (Jy): 0.1 mJy at 900um and 1 mJy at 450 um, based on SCUBA 850um flux density of the lensed LBG MS1512-cB58. Observations should continue until a reasonable detection is made (see #12 below) 7.2. Required continuum rms (Jy or K): 0.01 mJy in Band 7 0.1 mJy in Band 9 7.3. Dynamic range within image: 7 8. Line intensity: 8.1. Typical value (K or Jy): N/A 8.2. Required rms per channel (K or Jy): N/A 8.3. Spectral dynamic range: N/A 9. Polarization: no 9.1. Required Stokes N/A 9.2. Total polarized flux density (Jy) N/A 9.3. Required polarization rms and/or dynamic range N/A 9.4. Polarization fidelity N/A 10. Integration time for each observing mode/receiver setting (hr): Band 7 continuum: 20 x 3.25 hr Band 9 continuum: 20 x 1.75 hr 11. Total integration time for program (hr): 80 hrs 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) Each target should be observed until a S/N=10 is reached, but for at least a total of 2 hrs and for not more than 7 hrs. ********************************************************************* Review Pierre Cox: This programme proposes to search the thermal dust continuum emission of 20 Lyman Break Galaxies at the highest frequencies (Bands 7 and 9). Clearly important science. It is not clear why a signal-to-noise ratio of 10 is requested for a detection experiment. Aiming for say s/n of 5-6 would reduce the observing time significantly. Comment EvD: keep programme as is, since it does not require much time overall; reduced S/N could be compensated by increased number of sources -------------------------------------------------- Review v2.0: 1.1.9 Achieving a sensitivity of 0.01 mJy rms at 900 um band is somewhat a time consuming business for a simple detection purpose, as suggested by previous reviewers; it will already require about 8 hours integration per source at 300 GHz (1000 um) band (more integration time for shorter wavelengths, such as 880 um). Cross-correlation between ACA and 12-m array antennas will be beneficial; especially for band 9 observations. ===================================================================================== DRSP 1.1.10 Title Follow-up observations of Spitzer selected galaxies Pi A. Blain Time 560 1. Name of program and authors Follow-up observations of Spitzer selected galaxies Andrew Blain 2. One short paragraph with science goal(s) The Spitzer Space Telescope has provided an effective first look into a representative volume of luminous galaxies with far-infrared emission in the Universe at redshift z~1, typically lower than those of submm-selected galaxies. However, Spitzer provides a short-wavelength (most sensitive out to 23 microns) and unresolved view of the apparent disk galaxies that dominate the luminosity function at this redshifts. Optical redshifts and morphologies are available for many examples, but this combination of information does not provide insight into where the dust-enshrouded star formation is concentrated, and thus into the astrophysical processes - tides, collisions, gravitational collapse -- that are responsible, ALMA provides a unique facility to rapidly image the stryuctures within these galaxies that are required too understand their emission. About 60 square degrees has been surveyed to useful depth using Spitzer, more than half accessible from the South. Spitzer colors, oprical-Spitzer colors and some redshifts are available, and can be used to select a subsample of Spitzer-selected galaxis that span the full range of properties of the galaxy sample, which is likely to involve the formation of the majority of disk stars in the Universe today. There are something like 100000 cataloged galaxies in the final Spitzer fields. Only ALMA can pinpoint the most active regions of these galaxies, and provide information about the mechanisms triggering their luminosity. 3. Number of sources (e.g., 1 deep field of 4'x4', 50 YSO's, 300 T Tauri stars with disks, ...; do NOT list individual sources or your "pet object", except in special cases like LMC, Cen A, HDFS) Of order up to 50000 galaxies, spread over the sky. In equatorial COSMOS field, GOODS-S, HDF-S and Southerly SWIRE fields. This large number can be used to construct an extremely accurate luminosity function, revealing the internal structure of star formation and AGN emission in galaxies spanning the range of luminosities from typical galaxies to the most extreme systems. However, some useful statistical information is available from a sample size as small as a few 1000 targets, allowing a 10-bin luminosity function to be compiled as a function of several Spitzer color classes. 4. Coordinates: 4.1. Rough RA and DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 30 in Lupus) Indicate if there is significant clustering in a particular RA/DEC range (e.g., if objects in one particular RA range take 90% of the time) Should be approximately uniform around the year. 4.2. Moving target: yes/no (e.g. comet, planet, ...) No 4.3. Time critical: yes/no (e.g. SN, GRB, ...) No 4.4. Scheduling constraints: (optional) Good weather required. 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.01"-1" 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) Single field in general, targeted at known object. 5.3. Required pointing accuracy: (arcsec) 1" 6. Observational setup 6.1. Single dish total power data: no/beneficial/required No Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no/beneficial/required No, unless standing idle for a bit more collecting area. 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no/beneficial/required Yes, if ACA used 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no No 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9 In principle all bands to provide excellent SED, but 3,6 and 9 should provide good continuum SED, with the best chance of detecting a CO line coming in band 3 & 4 where fractional bandwidth is greatest, and sensitive to CO(2-1) for 1 404s each 12. Total integration time for program (hr): 5000 sources (estimated, most likely with redshifts) => 560 hours total 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): -------------------------------------------------- Review v2.0: 1.1.10 Clearly, SED determination of SST selected galaxies using ALMA is an important science case. Time estimations for 90, 230, and 670 GHz bands seem OK. At 350 GHz band, about 16 sec integration per pointing will be sufficient to achieve the required rms sensitivity of 0.5 mJy, so 180 sec each. This results in the total integration time for 5000 sources of 250 hrs. Relaxing of 670 GHz sensitivity requirement will also reduce the total integration time significantly; about 45 sec will achieve the rms sensitivity of 1.5 mJy (still S/N of ~100, seems to be enough). The total time will be then (60+4+16+45)*5000 = 174 hrs, for example. Is it essential to observe both 230 and 350 GHz in terms of SED measurements? More observing bands are better for SED, of course, but it may be possible to reduce the number of observing bands. For instance, about 6 sec integration at around 280 GHz will also achieve a sensitivity of 0.5 mJy rms, and these 3 bands, i.e., 90, 280, and 670 GHz bands observations will be made just (60+6+100)*5000 = 231 hrs or so. (just 20 hrs saving, though) ===================================================================================== DRSP 1.2.1 Title Weak lensing using ALMA Pi A. Blain Time 100 hrs 1. Name of program and authors Weak lensing using ALMA Andrew Blain 2. One short paragraph with science goal(s) Gravitational lensing by large-scale structure in the Universe produces systematic distortions in the shapes of galaxies at moderate and high redshifts (by about 0.1-1% for z>0.2). These distortions can be used to map the distribution of dark matter along the line of sight to the lensed object. Currently, this effect is detected statistically with samples of over 10,000 galaxies detected in optical survey fields at least 10 square arcmin in extent. Although ALMA will have exquisite spatial resolution, it will not be able to cover large enough fields to match this work. The ALMA archive would allow this science to be pieced together in field observed for other deep science investigations. There is however, a possible unique niche for ALMA to study weak lensing, along with the astrophysics of gas emission from galaxies at moderate redshifts. By imaging disk galaxies that are close to each other on the sky (separated by an arcmin or less), and by measuring their rotation fields very accurately the distortion can perhaps be detected (Blain 2002 ApJ 570 L54). The most promising way to probe this should be to detect the CO(3-2) line from z~0.5, at which there should be a significant amount of excited gas present, and yet the distance is such that the galaxy is neither too small nor too faint. z~0.5 line-emitting galaxies may also be important for galaxy evolution science. This project may be possible in parallel. 3. Number of sources (e.g., 1 deep field of 4'x4', 50 YSO's, 300 T Tauri stars with disks, ...; do NOT list individual sources or your "pet object", except in special cases like LMC, Cen A, HDFS) 1 trial pair of z~0.5 spiral galaxies separated by up to about 1 arcmin on sky (perhaps pre-selected from a deep ALMA survey region). Program could be extended, combining examples in an interconnected web to build up a map of the distortion 1 arcmin at a time. 4. Coordinates: 4.1. Rough RA and DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 30 in Lupus) Indicate if there is significant clustering in a particular RA/DEC range (e.g., if objects in one particular RA range take 90% of the time) Could be anywhere near ALMA latitude in dec. 4.2. Moving target: yes/no (e.g. comet, planet, ...) No 4.3. Time critical: yes/no (e.g. SN, GRB, ...) No 4.4. Scheduling constraints: (optional) None 5. Spatial scales: 5.1. Angular resolution (arcsec): Angular resolution (arcsec): 0.03-0.1" at 230 GHz. Best possible resolution is essential to resolve the rotation curve 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 0.03"=10". Pair of single fields. 5.3. Required pointing accuracy: (arcsec) 1 6. Observational setup 6.1. Single dish total power data: no/beneficial/required No Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) N/A 6.2. Stand-alone ACA: no/beneficial/required No 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no/beneficial/required Possibly, as it would help sensitivity a little, which is required to be excellent; but, owing to lack of mosaicking, it'll have no benefit for imaging quality. 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no No. Sensitivity crucial. 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9 6 7.2. Lines and Frequencies (GHz): (approximate; do _not_ go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify, e.g., "6 frequency settings in Band 3". Apply redshift correction yourself.) CO(3-2) redshifted to 230GHz 7.3. Spectral resolution (km/s): 7.4. Bandwidth or spectral coverage (km/s or GHz): 1-2 km/s 8. Continuum flux density: 8.1. Typical value (Jy): (take average value of set of objects) (optional: provide range of fluxes for set of objects) 0.1mJy 8.2. Required continuum rms (Jy or K): N/A - line observation 8.3. Dynamic range within image: Not a problem. Bright nearby objects will be avoided (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10% 9. Line intensity: 9.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) 0.4 Jy km/s integrated over 300 km/s, i.e 1.3 mJy line flux. Point by point probably a 10 km/s wide line. 9.2. Required rms per channel (K or Jy): Approx. 0.13mJy to give 100-sigma on whole line. 9.3. Spectral dynamic range: Modest - 100. 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10%. 10. Polarization: yes/no (optional) No 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 0.13 mJy. RMS in 2 km/s channel in 1 hr is 0.93 mJy, so 51 hours. 2 pointings, 100 hours. Corresponding brightness sensitivity is 1.2 K at 0.05" resolution. 12. Total integration time for program (hr): 100 hrs on a carefully considered target pair of z~0.5 galaxies 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): ===================================================================================== DRSP 1.2.2 Title A ultradeep galaxy survey through clusters using ALMA Pi A. Blain Time 1740 hrs 1. Name of program and authors A ultradeep galaxy survey through clusters using ALMA Andrew Blain 2. One short paragraph with science goal(s) Clusters of galaxies are the most massive gravitationally relaxed systems in the Universe, and the most powerful gravitational lenses. Depending on the brightness distribution of faint background galaxies, the surface density of their lensed images to a chosen flux density limit can be increased by several times by a foreground cluster. Furthermore, the magnification, by up to several 10's, allows galaxies to be probed in more detail than possible without the magnification. In order to determine the properties of the population of galaxies at fainter levels than currently possible, benefiting from the gravitational lensing, the typically ring-like 1-arcmin radius `critical line' structures along which the greatest magnifications will be found will be mapped, involving of order 20 pointings per cluster. An additional speculative investigation could image the central core of the clusters to the same deep depth. If the potential of the cluster is sufficiently is sufficienty steep at the center: corresponding to a volume density of mass that depends on radius as the -1.5 power or steeper, then de-magnified images of all the background galaxies within the = approx. 1 arcmin radius of the critical lines can be imaged within a few arcsec of the core of the cluster. ALMA's exquisite resolution can be used to detect all of these objects in a single additional pointing per cluster (Blain 2002 MNRAS 330 219). Hence, the cluster images would have a `bullseye' structure. The location of the fields within the clusters will be chosen carefully based on the best models of the potential of the clusters available in 2012 from optical, X-ray and Sunyaev-Zeldovich (SZ) effect observations. It is likely that it would be productive to include the same targets in a 90-GHz band-3 line survey, which could produce SZ effect images alongside. 3. Number of sources (e.g., 1 deep field of 4'x4', 50 YSO's, 300 T Tauri stars with disks, ...; do NOT list individual sources or your "pet object", except in special cases like LMC, Cen A, HDFS) 4. Coordinates: 4.1. Rough RA and DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 30 in Lupus) Indicate if there is significant clustering in a particular RA/DEC range (e.g., if objects in one particular RA range take 90% of the time) Up to 20 rich clusters at approximately z=0.2-1.2. Spread around the sky, but mainly equatorial (based on the most complete cluster surveys having been followed up by large telescopes in the North). 4.2. Moving target: yes/no (e.g. comet, planet, ...) No 4.3. Time critical: yes/no (e.g. SN, GRB, ...) No 4.4. Scheduling constraints: (optional) None 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.1" 5.2. Range of spatial scales/FOV (arcsec): 0.1-5" (optional: indicate whether single-field, small mosaic, wide-field mosaic...) Small mosaic. 20 fields at 280 GHz round critical lines in band-6/7 7 fields at 90GHz in a hexagonal pack to cover whole region. 5.3. Required pointing accuracy: (arcsec) 1" 6. Observational setup 6.1. Single dish total power data: no/beneficial/required No Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no/beneficial/required Yes, if SZ sought. 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no/beneficial/required Yes, as coherent spatial emission from lensed arcs could extend over most of the primary beam, and can see atmospheric effects on SZ/lensing signal in real time. 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no No. 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9 Edge of band 6/7: faint continuum surveys most promising at these frequencies. Band-3: line surveys most promising here, and SZ effect 7.2. Lines and Frequencies (GHz): (approximate; do _not_ go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify, e.g., "6 frequency settings in Band 3". Apply redshift correction yourself.) Continuum in band 6/7 single tuning. 3 line tunings in band 3. 7.3. Spectral resolution (km/s): 50-300 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 8GHz 8. Continuum flux density: 8.1. Typical value (Jy): (take average value of set of objects) (optional: provide range of fluxes for set of objects) Typical optical galaxies at 0.1mJy or less. Deep survey, so unknown. SZ effect a few 100 mJy integrated over the cluster. 8.2. Required continuum rms (Jy or K): 0.01 mJy - band 6/7 - to reach much deeper than any current survey: detection limit is about 40 times deeper than current record. 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) Brightest continuum sources 20mJy. 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10% 9. Line intensity: 9.1. Typical value (K or Jy): Set by continuum conditions above (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10. Polarization: yes/no (optional) No 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): Continuum rms at 280GHz is 0.02 mJy per hour => > 4 hour per pointing, 80 hours per cluster. For SZ at 90GHz, rms is 0.97mK per hour, so need about 1 hour per pointing, 7 hours per cluster 12. Total integration time for program (hr): 20 clusters (x87hr)= 1740 hours. Note that there are of order 20 suitable clusters, but that the time available could be cut to fit the available resource. The 1740 hour total gives the maximum amount of time that could be spent on this type of deep field observation. 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): Could be reduced in length, going for fewer objects. Otherwise, can be a long-term survey spread over 5 years or more. In DRSP1, a total of 500 hours was considered reasonable. Herschel & JWST will certainly cover ~30 clusters in a reasonable time (5 years). Hence, a reasonable number of targets for DSRP2 could be 5-6, for a similar total time. There is a potential long-term market for about 30 targets. ===================================================================================== DRSP 1.2.3 Title Follow-up observations of very bright Planck Surveyor sources Pi A. Blain Time 500 hrs 1. Name of program and authors Follow-up observations of very bright Planck Surveyor sources Andrew Blain 2. One short paragraph with science goal(s) There is no all-sky submm survey. IRAS, and the forthcoming Akari & WISE surveys, have mapped large areas of the sky, but at longer wavelengths the brightest examples of the submm galaxy population have not been cataloged. This should change after 2009 when the Planck Surveyor satellite surveys the whole sky at 850, 500 and 350 microns at 5-arcmin resolution, detecting objects as faint as several 100mJy. It is unclear how deep the survey catalog will go, but it is likely that at least 10,000 sources will be detected. These will be a mix of relatively low-redshift, low-luminosity sources and the most luminous galaxies in the Universe. 10% of them could be gravitationally lensed by at least a factor of 2 by foreground galaxies. These objects will be bright and easy to study by ALMA. This proposal assesses the time required to locate, image and study these galaxies, revealing the astrophysics in the most extreme objects known. In parallel, a wide-field, shallow imaging survey of order 70 square degrees will be made. 3. Number of sources (e.g., 1 deep field of 4'x4', 50 YSO's, 300 T Tauri stars with disks, ...; do NOT list individual sources or your "pet object", except in special cases like LMC, Cen A, HDFS) Of order 20,000 galaxies over the whole sky, about 30% eclipsed by the Milky Way, and 40% inaccessible from the ALMA site. So up to 10,000 targets. A small minority may already be located in FIRST radio survey, minimizing need for an ALMA OTF map to locate them. Depending on the availability of single-dish bolometer arrays to locate the targets accurately enough for single pointings with ALMA, there could be significant time savings. 4. Coordinates: 4.1. Rough RA and DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 30 in Lupus) Indicate if there is significant clustering in a particular RA/DEC range (e.g., if objects in one particular RA range take 90% of the time) Should be approximately uniform (except the Milky Way region) No clustering, but avoiding 04-09hr. 4.2. Moving target: yes/no (e.g. comet, planet, ...) No 4.3. Time critical: yes/no (e.g. SN, GRB, ...) No 4.4. Scheduling constraints: (optional) None specific, but follow-up deep imaging requires multi-band and good weather, so probably not during lower 50% of weather. 5. Spatial scales: 5.1. Angular resolution (arcsec): Angular resolution (arcsec): 0.01"-1" 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 5' field mosaic (if no radio or bolometer array/WISE/Akari position) and then a single deep field when object located. 5.3. Required pointing accuracy: (arcsec) 1", or so. Galaxies should be bright and easy to register at other wavelengths once discovered using ALMA. 6. Observational setup 6.1. Single dish total power data: no/beneficial/required No Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) N/A 6.2. Stand-alone ACA: no/beneficial/required No 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no/beneficial/required No Marginal sensitivity increase slightly useful, but no demand from imaging quality. 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no Probably not, alhough the 5-arcmin mosaic to locate the target could use subarrays at the expense of longer integration times. 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9 Band 6 to scan the field for a detection - most rapid, due to a combination of expected SED, primary beam area and source SED. The SED can be estimated from Planck bands, along with ASTRO-E upper limits/ detections. Follow up imaging in at least 4 well-spaced bands, to determine color distributions, and accurate SEDs. Three tunings in band-3 to search 24GHz for CO lines: detect redshifts for ~30% of sources. If a line is detected, then use appropriate other bands to detect different transitions - likely to be only one additional observation. 7.2. Lines and Frequencies (GHz): (approximate; do _not_ go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify, e.g., "6 frequency settings in Band 3". Apply redshift correction yourself.) 230-GHz imaging in band-6 for mosaic. 7.3. Spectral resolution (km/s): 300 7.4. Bandwidth or spectral coverage (km/s or GHz): 8 GHz. (Full range) 8. Continuum flux density: 8.1. Typical value (Jy): (take average value of set of objects) (optional: provide range of fluxes for set of objects) For typical galaxy SED at moderate redshift: 90GHz 1 mJy 230GHz 50 mJy 350GHz 100 mJy 670GHz 300 mJy There is a tail of brighter candidates 8.2. Required continuum rms (Jy or K): Search at 230GHz - need rms 5mJy or less. Imaging at other wavelengths - need good quality image: 90GHz 0.05mJy 230GHz 1mJy 350GHz 2mJy 670GHz 2mJy 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) Small. 100. All single bright objects 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10% should be fine. No repeatability. Minimize overheads in survey. 9. Line intensity: Uncertain, should be detectable, but redshifts not known - should be easy to search band 3 for CO emission in a matter of seconds. 9.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) N/A ~1 Jy over 300 km/s channel in band 3. 9.2. Required rms per channel (K or Jy): N/A - set by continuum 9.3. Spectral dynamic range: N/A - small. Single strong line on weak continuum. 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10%, no repeatability. 10. Polarization: yes/no (optional) Might be possible for bright objects in follow-up imaging to search for signs of AGN. 10.1. Required Stokes parameters: Just 2 10.2. Total polarized flux density (Jy): ~1-10% of continuum possible. In lowest band 1 0.1mJy 10.3. Required polarization rms and/or dynamic range: 3% 10.4. Polarization fidelity: Not an issue 10.5. Required calibration accuracy: For detection only 11. Integration time for each observing mode/receiver setting (hr): 230GHz - 30 images to cover 5-arcmin pixel - each 5mJy RMS (0.04s)=1.2s (scan overheads dominate) Imaging on target - 90GHz - 58s (x3 tunings) 230GHz - 1s 350GHz - 1s 670GHz - 25s ~3 minutes each. Will be dominated by overheads for slewing/scanning etc... deeper imaging of detected sources possible. Accurate assessment of overheads is currently tough. Number of targets may need to cut back hard, but the potential target list is up to 10,000. 12. Total integration time for program (hr): 10,000 sources (estimated) = up to 500 hours (overheads crucial). 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): OTF mosaic required to minimize time losses in initial search. Other parts require grouping by frequency range, all sources together, to minimize overheads too. Probably both `hot' bands simultaneously at 1 target, if 15s swap required. Retuning in band 3 to be done in single visit. Source list may be culled in favor of brighter sources after initial OTF map to locate source. OTF map role may be filled by a bolometer array survey at the Planck catalog positions. ===================================================================================== DRSP 1.2.4 Title A submm study of strong gravitational lenses Pi T. Wiklind Time 230 hrs 1. Name of program and authors A submm study of strong gravitational lenses Wiklind T. 2. One short paragraph with science goal(s) Strong gravitational lensing offers the possibility to indirectly image the gravitational potential of individual galaxies. Presently this is done using background AGNs, viewed either at optical/NIR wavelengths, or at radio wavelengths. The former case leads to point-like images and, hence, with few constraints on the shape of the lensing potential. The latter case often leads to partially resolved images of the background source. However, the intrinsic shape of the radio loud AGN remains unknown and effectively reduces the number of constraints that can be set on the lens. Dust continuum emission offers an advantage over both optical and radio wavelengths; it has a finite and resolvable distribution and its intrinsic shape, although unknown, is likely to be simple compared to radio jets. With present day instrumentation, it is not possible to reach the low flux levels associated with the extended dust emission, nor to reach the angular resolution needed. Another constraint on the shape of the lensing potential can be obtained from the relative flux ratios of two or more images of the same source point. However, this constraint is rarely usable due to different amount of obscuration along different line of sights in the case of optical imaging, and due to only partially resolved images at radio wavelengths. Observing at submm wavelengths alleviates the obscuration problem, and if sufficient angular resolution can be achieved, the images will be resolved to the extent that flux ratios will provide an additional constraint when solving for the lensing potential. Two projects are proposed: 1) Imaging of known gravitationally lensed radio loud AGNs with the aim of determining accurate positions and relative flux ratios of the lensed components. Lenses can be selected from optical and/or radio surveys. Typical flux levels are in the mJy range. Angular scales are 0.1 - 3 arcsec Number of sources ~ 10 2) High fidelity imaging of gravitational lenses, selected from optical and/or radio surveys, in order to image the lensed components of the host galaxy. Another source of targets is background galaxies strongly lensed by intervening cluster members. The aim is to constrain the total gravitational potential of the lens by resolving the images, determining the shape and location of the Einstein ring caused when parts of the host galaxy passes through the cusp. Typical flux levels are 25 microJy and up Angular scales are 0.1" - 1" Number of sources ~ 5 In addition, observations of CO lines in emission can be used to both determine the physical and chemical status of the gas in the background source and to constrain the lens modeling. However, this aspect of gravitational lensing will not be covered in this proposal as the instrumental parameters needs to be defined specifically for each individual case. Another issue will be searching for new gravitational lenses. Here one can target high redshift AGNs, which are not known to be lensed. The larger extent of the dust emission region could mean that the dust emission consists of multiple components while the AGN remains single, albeit magnified. This aspect is not covered in this proposal, as it will be a 'side product' of other surveys, in particular those concerning weak lensing. A short note on flux density estimates: The actual flux densities from 'typical' high redshift galaxies is essentially unknown at the present. An estimate of the observed flux in a 16 GHz wide band centered on 345 GHz of an unresolved galaxy with a FIR luminosity of 1E10 L_sun (integrated over 10-3000 micron) is : Dust temp z=2 z=4 z=6 K ----------------------------------------------------- 30 35 microJy 33 microJy 22 microJy 50 8 9 10 ----------------------------------------------------- The luminosity and flux density have been estimated using a modified blackbody curve B_nu(T_d) (1 - exp(-tau_nu), where tau_nu = (\nu/\nu_0)**b. The parameter b is set to 1.5 and \nu_0 to 10 microns. Parts of the emission will be magnified with factors >10, while other parts will experience magnification factors much smaller ~2. Hence, ALMA can easily detect unresolved lens components in this particular case, but will run into problems when resolving the emission. An exact time estimate is therefore not possible at the present, and needs to be done on a case-to-case basis. The FIR luminosity chosen for this example may be a conservative estimate for typical targets. It may also prove favorable to use band 9, both from an angular resolution point of view and for an increased sensitivity (basically for any type of dust SED). With this note in mind, the suggested programme is only preliminary and a final decision should await actual receiver performance details. The time estimate has been done in a very conservative manner. 3. Number of sources (e.g., 1 deep field of 4'x4', 50 YSO's, 300 T Tauri stars with disks, ...; do NOT list individual sources or your "pet object", except in special cases like LMC, Cen A, HDFS) 10 radio loud strongly gravitational lensed sources 2 strongly gravitationally lensed AGNs, both radio loud and radio quiet (possibly more sources if time estimate is over-conservative; see below). 4. Coordinates: 4.1. Rough RA and DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 30 in Lupus) Source list can be selected such that there is a desired spread in RA and DEC. Indicate if there is significant clustering in a particular RA/DEC range (e.g. if objects in one particular RA range take 90% of the time) NO 4.2. Moving target: yes/no (e.g. comet, planet, ...) NO 4.3. Time critical: yes/no (e.g. SN, GRB, ...) NO 5. Spatial scales: 5.1. Angular resolution (arcsec): Ranging from 0.1" to ~3" (see observing strategy below) 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) Single field per source 5.3. Single dish total power data: yes/no NO 5.4. ACA: yes/no NO 5.5. Subarrays: yes/no NO 6. Frequencies: 6.1. Receiver band: Band 3, 6, 7, or 9 Band 7 6.2. Lines and Frequencies (GHz): (approximate; do NOT go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify e.g. "6 frequency settings in Band 3". Apply redshift correction yourself) Band 7, continuum observation 6.3. Spectral resolution (km/s): None 6.4. Bandwidth or spectral coverage (km/s or GHz): Band 7, 16 GHz 7. Continuum flux density: 7.1. Typical value (Jy): (take average value of set of objects) (optional: provide range of fluxes for set of objects) 30 microJy - several mJy (due to magnification and resolved images). 7.2. Required continuum rms (Jy or K): 1) 25 microJy (radio loud AGNs) 2) 6 microJy (high fidelity imaging) 7.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether e.g. weak objects next to bright objects) ~50-100 8. Line intensity: 8.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) No 8.2. Required rms per channel (K or Jy): No 8.3. Spectral dynamic range: No 9. Polarization: yes/no (optional) No 9.1. Required Stokes total intensity only 9.2. Total polarized flux density (Jy) N/A 9.3. Required polarization rms and/or dynamic range N/A 9.4. Polarization fidelity N/A 10. Integration time for each observing mode/receiver setting (hr): 1) Imaging of gravitationally lensed radio loud AGns: estimated rms needed ~50 (correct to 25 EvD) microJy, requiring ~ 0.25 hours per source. For an angular resolution of 0.1", this increases to ~25 hours. Not all lenses are likely to need 0.1" resolution. An estimate is therefore 10x0.25 + 3x25 = 100 hours. (this time estimate can be decreased significantly if a sufficient number of stronger radio loud lensed AGNs become available prior to 2011). 2) High fidelity imaging of lensed AGNs (not necessarily radio loud): estimated rms needed 10 microJy, requiring ~6 hours per source at an angular resolution of 1". At 0.3" the time increases to ~60 hours per source. With 2 sources in total the time amounts to ~130 hours. (If the flux densities are stronger, the same amount of time should/could be used to reach the target angular resolution of 0.1"). 11. Total integration time for program (hr): 230 hours + over-head 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) Targets can be selected from known gravitational lenses. The number of available targets is likely to be significantly larger at the time when ALMA is fully operational than what is the case now. This will likely mean that targets can be chosen that have a FIR luminosity greater than the nominal (and conservative 1.E10 L_sun used here). This will decrease the estimated integration time considerably. Review Chris Carilli: he says he needs an rms of 50 uJy for radio loud AGN in continuum with band 7, and that this will take 0.25hrs. but I get an rms of 25 uJy in 0.25 hrs. in another place in proposal he says 25 uJy, so I guess 50 was just a typo. Comment Ewine: typo corrected to 25 uJy -------------------------------------------------- Review v2.0: 1.2.4 A submm study of strong gravitational lenses (Wiklind) Not revised since DRSP 1.1. Similar to 1.2.2. Scientifically OK, no need for ACA or ACA/12m array cross-correlation. Back then 230 h + overhead, probably similar now. ===================================================================================== DRSP 1.2.5 Title Dust in gravitationally lensed Lyman Break Galaxies Pi M. Sawicki Time 94.2 hrs 1. Name of program and authors Title: Dust in gravitationally lensed Lyman Break Galaxies. Author: Marcin Sawicki, marcin.sawicki@nrc.ca 2. One short paragraph with science goal(s) Star-formation rates and other properties of z~3 Lyman Break Galaxies (LBGs) remain only poorly constrained because of the presence of starlight-absorbing interstellar dust which can only be properly understood by combining rest-far-IR data with rest-frame optical and UV observations. Normal LBGs are expected to be too faint at sub-mm wavelengths to yield anything but integrated fluxes even with ALMA. Therefore, to gain understanding of the spatial distribution of dust and star formation in LBGs, we propose to observe three gravitationally lensed LBGs, whose fluxes are magnified by factors of 10-30. These observations, to be carried out at 450 and 900 um, will provide information about the spatial distribution of dust in LBGs that will be directly comparable to rest-frame UV and optical HST observations of these objects. These observations will allow us to study each of these gravitational arcs with ~25-100 spatial resolution elements having a S/N=10 per spatial resolution element. 3. Number of sources: 3 4. Coordinates: 4.1. Rough RA and DEC RA(2000) Dec(2000) MS1512-cB58 15:14:22.2 +36:36:24 Cl1053-arc 10:53:47.2 +57:35:10 A2218-arc 16:35:49.3 +66:13:07 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.1 5.2. Range of spatial scales/FOV (arcsec): individual point sources - one per field 5.3. Single dish total power data: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Bands 7 and 9 6.2. Lines and Frequencies (GHz): continuum 6.3. Spectral resolution (km/s): N/A 6.4. Bandwidth or spectral coverage (km/s or GHz): N/A 7. Continuum flux density: 7.1. Typical value (Jy): Total flux density per object 1-4 mJy at 900um 10-40 mJy at 450um 7.2. Required continuum rms (Jy or K): 0.004 mJy in Band 7 0.04 mJy in Band 9 7.3. Dynamic range within image: 7 8. Line intensity: 8.1. Typical value (K or Jy): N/A 8.2. Required rms per channel (K or Jy): N/A 8.3. Spectral dynamic range: N/A 9. Polarization: no 9.1. Required Stokes N/A 9.2. Total polarized flux density (Jy) N/A 9.3. Required polarization rms and/or dynamic range N/A 9.4. Polarization fidelity N/A 10. Integration time for each observing mode/receiver setting (hr): Band 7 continuum: 3x20.3 hr Band 9 continuum: 3x11.1 hr 11. Total integration time for program (hr): 94.2 hrs 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) Review Chris Carilli: OK, integration times checked -------------------------------------------------- Review v2.0: 1.2.5 Dust in gravitationally lensed Lyman Break Galaxies (Sawicki) Not revised since DRSP 1.1. No further comment, no need for ACA or ACA/12m array cross-correlation. ===================================================================================== DRSP 1.3.1 Title Spectral line survey in high-z molecular absorption systems Pi T. Wiklind Time 240.3 hrs 1. Name of program and authors Spectral line survey in high-z molecular absorption systems Wiklind T., Combes F. 2. One short paragraph with science goal(s) Molecular line absorption in front of a radio continuum source is a very powerful technique to detect even small quantities of interstellar molecules in external galaxies. It is also complementary to the emission technique: it samples molecules in low excitation state, that would never have been detected in emission. For galaxies at large distances, molecular absorption lines offer the only way to observe rare molecular species. This has been proven through the detection of many molecular species (about 20) at redshifts z=0.25-0.89, using pre-ALMA instrumentation. The sensitivity is largely determined by the strength of the background continuum source, meaning that a large collecting area is the main issue (the sources themselves remain point sources even at high angular resolution). The completion of ALMA makes it possible to make a spectral line survey to an unprecedented level of the molecular interstellar medium in distant galaxies. We propose to carry on a complete molecular line survey (using the available frequency bands) towards 3 remarkable sources at different redshifts, in order to probe the interstellar chemistry and its evolution. Many different molecular species, such as CCH, C3H2, HOC+, SiC, deuterated species etc. are expected to be detected. A complete spectral line survey will allow a detailed comparison of the interstellar chemistry of these three distant sources with that of the Milky Way ISM. In addition, the survey will include several molecular lines which for Milky Way gas are not possible to observe from the ground; such as the ground transition of LiH and water vapor, as well as the elusive molecular oxygen. Noise rms limits have been chosen such that over most of the available frequencies, absorption lines with depth of <1% of the continuum flux can be detected at 5sigma. Over some frequency intervals and for the stronger sources, this limit can be set as low as 0.15% (while lowering the velocity resolution), without excessive exposure times. This corresponds to column densities of CO and HCO+ of 910E12 and 1E10, respectively. It is possible that the density of lines will be large, possibly limiting the detections of individual lines through confusion over certain frequency intervals. We propose to do a systematic survey in the 7 priority bands Band 3: 86 GHz - 116 GHz Band 4: 125 GHz - 163 GHz Band 5: 163 GHz - 211 GHz (6 antennas) Band 6: 211 GHz - 275 GHz Band 7: 275 GHz - 370 GHz Band 8: 385 GHz - 500 GHz Band 9: 602 GHz - 720 GHz for 3 absorption systems already observed with IRAM and SEST, and visible from Chajnantor: PKS1830-211 (z=0.89) PKS1413+135 (z=0.25) CenA (z=0) 3. Number of sources (e.g., 1 deep field of 4'x4', 50 YSO's, 300 T Tauri stars with disks, ...; do NOT list individual sources or your "pet object", except in special cases like LMC, Cen A, HDFS) 3 sources PKS1830-211, PKS1413+135 and CenA (note that PKS1830-211 gives two sight lines through the intervening galaxy, separated by ~6 kpc). 4. Coordinates: 4.1. Rough RA and DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 30 in Lupus) Indicate if there is significant clustering in a particular RA/DEC range (e.g., if objects in one particular RA range take 90% of the time) 1830-211, 1413+135, 1325-43 4.2. Moving target: yes/no (e.g. comet, planet, ...) No 4.3. Time critical: yes/no (e.g. SN, GRB, ...) No 4.4. Scheduling constraints: (optional) No 5. Spatial scales: 5.1. Angular resolution (arcsec): 1 arcsec 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 5.3. Required pointing accuracy: (arcsec) 2-5" (depending on frequency) 6. Observational setup 6.1. Single dish total power data: no/beneficial/required NO Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) Nutator 6.2. Stand-alone ACA: no/beneficial/required No 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no/beneficial/required No 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no No 7. Frequencies: ALL 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9 ALL 7.2. Lines and Frequencies (GHz): (approximate; do _not_ go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify, e.g., "6 frequency settings in Band 3". Apply redshift correction yourself.) This is a line survey. We will cover the entire extent of each band falling within atmospheric windows of sufficient transparency. 7.3. Spectral resolution (km/s): 1-4 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): Band 3: bandwidth 2 GHz Band 4: bandwidth 2 GHz Band 5: bandwidth 1 GHz (6 antennas) Band 6: bandwidth 1 GHz Band 7: bandwidth 0.5 GHz Bnad 8: bandwidth 0.5 GHz Band 9: bandwidth 0.5 GHz 8. Continuum flux density: Fluxes at 90GHz. The continuum flux at higher frequencies is estimated assuming a spectral index of 0.7: S_nu = S_90 * (\nu/90)^-0.7 PKS1413: S_90 = 0.2 Jy PKS1830: S_90 = 2,0 Jy Cen A : S_90 = 6.0 Jy 8.1. Typical value (Jy): PKS1413 PKS1830 Cen A Band 3 0.20 2.00 6.00 Band 4 0.15 1.47 4.40 Band 5 0.12 1.20 3.60 Band 6 0.10 1.00 2.99 Band 7 0.08 0.82 2.46 Band 8 0.07 0.66 1.97 Band 9 0.05 0.50 1.49 (take average value of set of objects) (optional: provide range of fluxes for set of objects) 8.2. Required continuum rms (Jy or K): The limitation to the S/N is defined as the channel noise rms required to detect an absorption line of a given depth. The depth is defined as percentage of the continuum flux density. The ultimate aim is to detect absorptions line at 1% of the continuum level at 5 sigma. For one source (PKS1413) lines are narrow and the required velocity resolution is 1 km/s. 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) No imaging 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 9. Line intensity: 9.1. Typical value (K or Jy): See 8.2 (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): See 8.2 9.3. Spectral dynamic range: 100-500 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 5% relative ( 1-3% / 5% / 10% / n/a ) 1-3% 10. Polarization: yes/no (optional) No 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): The integration times have been calculated using the actual line flux density (from the ALMA integration time estimator), the required absorption line depth (1-10%), velocity resolution (1-5 km/s) and S/N ratio (3-5). This is calculated for each tuning and then summed for each band and source. Some bands contain atmospheric lines which will increase the system temperature. We have excised those regions which increase the integeation times by a factor more than 2 compared to other regions of the same band. The final observation will have a sensitivity of 1% at 5 sigma for 1 kms/s for approximately 80% of the complete frequency coverage. The remaining 20% have a lower sigma (3) and/or lower line sensitivity (5%) and/or lower velocity resoltuion (up to 5 km/s). A remaining uncertainty in the exposure time estimate is the available correlator configurations. This defines the number of tunings needed to cover a given band. We have assumed conservative bandwidths (see 7.4). Also, time for tuning is not included in the time estimate. PKS1413 PKS1830 Cen A Band 3 6.0 1.5 1.0 Band 4 14.4 3.6 1.0 Band 5 -- 6.3 8.0 Band 6 19.2 10.8 5.9 Band 7 42.8 3.8 16.2 Band 8 36.0 9.7 8.7 Band 9 -- 28.2 17.2 Total 118.4 63.9 58.0 12. Total integration time for program (hr): 240.3 + overhead 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): This is a molecular line line survey. The observations are self-calibrated using the central continuum source. The pointing accuracy needs to be than 5". Very good weather conditions are only required for high frequency observations. A homogeneous sensitivity is necessary in order to allow a comparative abundances study of weak lines. The estimated time can be decreased by lowering the target sensitivity or only choosing PKS1830-211 and Cen A as targets. However, given the uniqueness of this data set, we would prompt for a significant time allocation. -------------------------------------------------- Review v2.0: quasarexgal_1 = 1.3.1 Spectral line survey in high-z molecular absorption systems Wiklind T., Combes F. Very interesting project. Could it in fact be carried out at _any_ angular resolution? This would make it quite flexibly scheduled - more of an operational question than anything having to do with science. ===================================================================================== DRSP 1.3.2 Title A deep search for new molecular absorption line systems Pi T. Wiklind Time 260 hrs 1. Name of program and authors A deep search for new molecular absorption line systems Wiklind T., Combes F. 2. One short paragraph with science goal(s) Observations of molecular absorption lines offer the only way to obtain detailed information of the physical and chemical parameters of the molecular interstellar medium in distant galaxies. The sensitivity is essentially only given by the strength of the background continuum source, independent of the distance. Four molecular absorption line systems at redshifts between z=0.25-0.89 have previously been detected using single dish telescope, and allowed a detailed study of the astrochemistry of these systems, including molecular species never before observed from the ground. In addition, since molecular absorption is biased towards diffuse and therefore excitationally cold gas, the observations have made it possible to measure the temperature of the Cosmic Microwave Background radiation at the redshift of the absorber. In order to make a comparative study of the chemical and physical status of the molecular gas at earlier epochs it is necessary to increase the number of known systems. Molecular absorption line systems are rare, about 100 times less common than damped Lyman-alpha systems. They are also difficult to detect since continuum fluxes of the background sources are relatively weak at mm/submm wavelenghts. Also, the mere presence of obscuration means that redshift information is lacking. This was the case for one of the known absorption systems and it was detected by the technique of frequency scanning, looking for absorption of high-opacity molecules such as CO and HCO+ (actually, the line first detected in this case turned out to be a HNC(2-1) line). By observing the frequency range 86-116 and 226-260 GHz, the entire redshift space is covered for CO and HCO+ lines. These are the lines with the highest opacities. In this project we propose a search for molecular absorption towards 60 selected radio loud AGNs with mm continuum fluxes greater than 50mJy. The targets will be prioritized according to a few criteria which enhances the probability for the presence of obscuration; such as gravitational lensing (small impact parameter to the lens), suppressed soft X-ray flux, optically weak and indications of reddening. Since we want to discover absorption systems with unknown redshift, we will search for absorption over the entire redshift range using the technique of frequency scanning. Noise rms limits have been chosen such that band 3, which covers z=0-0.34 and z>0.54, where absorption lines with depth of 5% of the continuum flux can be detected at 5sigma. In band 4, covering z=0.09-2.69, and in particular the z=0.34-0.54 gap in band 3, the limits have been set to 5% at 5sigma as well. To enable a larger number of sources to have complete redshift coverage, these detection limits could be raised to 10% at 5sigma. With the velocity resolution given below, these limits corresponds to column densities of CO and HCO+ of 710E14 and 8E11 cm-2, respectively. 3. Number of sources (e.g., 1 deep field of 4'x4', 50 YSO's, 300 T Tauri stars with disks, ...; do NOT list individual sources or your "pet object", except in special cases like LMC, Cen A, HDFS) 50 flat spectrum radio continuum sources 4. Coordinates: Source list can be selected such that there is any desired spread in RA and DEC. 4.1. Rough RA and DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 30 in Lupus) Indicate if there is significant clustering in a particular RA/DEC range (e.g., if objects in one particular RA range take 90% of the time) 4.2. Moving target: yes/no (e.g. comet, planet, ...) NO 4.3. Time critical: yes/no (e.g. SN, GRB, ...) NO 4.4. Scheduling constraints: (optional) NO 5. Spatial scales: 5.1. Angular resolution (arcsec): All targets are point sources for which the angular resolution does not really matter. 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 5.3. Required pointing accuracy: (arcsec) 5" 6. Observational setup 6.1. Single dish total power data: no/beneficial/required NO Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) Nutator 6.2. Stand-alone ACA: no/beneficial/required NO 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no/beneficial/required NO 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no NO (possible for stronger sources, but not considered here) 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9 3 + 4 7.2. Lines and Frequencies (GHz): (approximate; do _not_ go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify, e.g., "6 frequency settings in Band 3". Apply redshift correction yourself.) The aim is redshifted CO and HCO+ lines. By using the entire frequency range of band 3 (86-116 GHz) and band 4 (125-162 GHz), the entire redshift range is covered. 7.3. Spectral resolution (km/s): 5 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): Band 3: 2x1 GHz = 2 GHz Band 4: 2x1 GHz = 2 GHz 8. Continuum flux density: 8.1. Typical value (Jy): 5 sources with fluxes 50 - 100 mJy 20 sources with fluxes 100 - 200 mJy 35 sources with fluxes >200 mJy (take average value of set of objects) (optional: provide range of fluxes for set of objects) 8.2. Required continuum rms (Jy or K): We aim at being able to detect an absorption at 5sigma at 5% of the continuum level in band 3 and band 4. The sources are assumed to have 50mJy, 100mJy and 200mJy at 90GHz, with a spectral index S_nu \propto S_nu^-0.7 (see ALMA Memo #543). The required exposure time has been calculated for each tuning for band 3 and 4, where the continuum rms is defined as the limit in percentage of the source continuum flux where an absorption line with a depth of 5% of the continuum can be detected at 5sigma. 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) n/a 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 10% repeatability ( 1-3% / 5% / 10% / n/a ) 5% relative ( 1-3% / 5% / 10% / n/a ) 5% 9. Line intensity: 9.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) See 8.2 9.2. Required rms per channel (K or Jy): See 8.2 9.3. Spectral dynamic range: 100 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10. Polarization: yes/no (optional) No 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): Band 3 50mJy at 90GHz : 2.2 hours + overhead 100mJy : 1.7 hours + overhead 200mJy : 1.9 hours + overhead Band 4 50mJy at 90GHz : 4.2 hours + overhead 100mJy : 2.9 hours + overhead 200mJy : 2.9 hours + overhead 12. Total integration time for program (hr): 260 hours + overhead (10 sources at 50mJy, 20 sources at 100mJy 20 sources at 200mJy) This estimate is based on a bandwidth of 2GHz. If 4GHz is available, with the required velocity resolution, the exposure times will be significantly lower (almost factor 2). 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): The targets will be radio loud AGNs with one or more of the following indications of possible obscuration along the line of sight (either intervening or intrinsic) (i) optically weak or blank field, (ii) indication of reddening, (iii) gravitationally lensed, (iv) suppressed soft X-ray flux, (v) observed galaxy along the line of sight. The observations are self-calibrated using the background continuum source. The pointing accuracy needs to be than 5". -------------------------------------------------- Review v2.0: quasarexgal_2 = 1.3.2. A deep search for new molecular absorption line systems Wiklind T., Combes F. Ok. ===================================================================================== DRSP 1.4.1 Title Imaging galaxy cluster mergers via the Sunyaev-Zel'dovich effect Pi K. Yamada Time 400 hrs 1. Name of program and authors Imaging galaxy cluster mergers via the Sunyaev-Zel'dovich effect K. Yamada, N. Okabe, T. Kitayama, M. Hattori 2. One short paragraph with science goal(s) We aim to reveal detailed structures around the merger sites and the shock fronts in galaxy clusters via deep mapping observations of the Sunyaev-Zel'dovich effect (SZE). The SZE provides a direct probe of thermal pressure in the intracluster medium, complementary to the X-ray observations which probes the emission measure. The SZE is also a unique tool for detecting the gas shock-heated to above 10 keV, for which current X-ray spectrometers lose sensitivity. With the spatial resolution of ALMA (2" at 90 GHz), we will be able to resolve the substructures down to 10 kpc at z=0.3. These measurements will be particularly useful in understanding the dynamical nature of the mergers and their links to the thermal evolution of galaxy clusters. 3. Number of sources : 5 clusters with signatures of violent mergers and shock heating 4. Coordinates: 4.1. Rough RA and DEC : (13h, -10d), (06h, -50d), (20h, -60d), (02h, -40d), (16h, -10d) 4.2. Moving target: no 4.3. Time critical: no 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution (arcsec): 2 arcsec (9 kpc at z=0.3) 5.2. Range of spatial scales/FOV (arcsec): 180 arcsec (800 kpc at z=0.3) diameter. Wide-field mosaic is necessary; e.g., 19 and 7 pointings in a hexagonal orientation for 12m and 7m antennas, respectively. 5.3. Required pointing accuracy (arcsec): 1 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: nutator switch or the on-the-fly mapping 6.2. Stand-alone ACA: yes 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: required 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3 7.2. Lines and Frequencies (GHz): 90 GHz 7.3. Spectral resolution (km/s): 7.4. Bandwidth or spectral coverage (km/s or GHz): 8. Continuum flux density: 8.1. Typical value (Jy): 0.02-0.06 mJy/ (2" beam) 8.2. Required continuum rms (Jy or K): 0.004 mJy/ (2" beam) 8.3. Dynamic range within image: 10-100. 8.4. Calibration requirements: absolute (5%) repeatability (5%) relative (5%) 9. Line intensity: no 9.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): 9.3. Spectral dynamic range: 9.4. Calibration requirements: 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 20 hours per source for the ACA-baseline_ALMA cross-correlation, and additional 60 hours per source for the stand-alone ACA 12. Total integration time for program (hr): 100 hours for the ACA-baseline_ALMA cross-correlation, and 300 hours for the stand alone ACA 13. Comments on observing strategy : Major advantages of using Band 3 for the SZE observation are that the level of foreground/background contamination is expected to be minimal and the FOV is still adequate for covering compact (sub)clusters. In order to map the larger area and increase the number of feasible targets, Band 1 will be more suitable. We have checked that there are very few known luminous (>10mJy) source at 90GHz in our target fields. It may nevertheless be the case that there exist yet unknown or variable sources in the fields. Detailed simulations will be helpful to clarify to what extent such sources can be removed using the long baseline data. An absolute calibration accuracy of 5% will be desirable and at least 10% will be necessary for performing detailed combined analysis with high sensitivity X-ray data to explore the physical status of the intracluster medium. ===================================================================================== DRSP 1.4.2 Title Sunyaev-Zeldovich Effect of Galaxy Clusters at High Redshift Pi N. Sugiyama Time 400 hrs 1. Name of program and authors Name: Sunyaev-Zeldovich Effect of Galaxy Clusters at High Redshift Authors: Naoshi Sugiyama, Naoki Yoshida, Tetsuo Hasegawa 2. One short paragraph with science goal(s) Observing the fine structure of clusters of galaxies probes formation history of the clusters. High-resolution observations of the thermal Sunyaev-Zel'dovich effect (SZE) can be an ideal and unique tool for this purpose. With 10 arc-second resolution, we can resolve merging proto-clusters whose sizes are approximately 100kpc. ALMA can also detect the kinematic SZE which is caused by streaming motion of galaxy clusters. Although the expected signal is smaller than the thermal SZE, merging clusters could imprint a peculiar dipole pattern that can be easily identified. Multi-frequency observations are essential. 3. Number of sources 1' deep field; about a few high-z clusters per FOV. (Selected based on optical/X-ray cluster catalogue. Not necessary to specify a peculiar object.) 4. Coordinates: 4.1. Rough RA and DEC (uniformly distributed over the sky) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution (arcsec): 1-2 5.2. Range of spatial scales/FOV (arcsec): 60" mosaic 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3, 6 (220 GHz is essential to remove foreground/background) 6.2. Lines and Frequencies (GHz): 90 and 220 GHz 6.3. Spectral resolution (km/s): not required 6.4. Bandwidth or spectral coverage (km/s or GHz): 8 GHz x dual pol 7. Continuum flux density: 7.1. Typical value (Jy): 0.01-0.1 mJy/(1" beam) 7.2. Required continuum rms (Jy or K): 0.002 mJy/(1" beam) 7.3. Dynamic range within image: 5 - 50 8. Line intensity: 8.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) 8.2. Required rms per channel (K or Jy): 8.3. Spectral dynamic range: 8.4. Calibration requirements: absolute (5%) repeatability (5%) relative (5%) 9. Line intensity: no 9.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): 9.3. Spectral dynamic range: 9.4. Calibration requirements: 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): (for band 3) 30 hours (per pointing) for the ACA-baseline_ALMA cross-correlation, and additional 90 hours for the stand-alone ACA 12. Total integration time for program (hr): 500 hours (ACA-baseline_ALMA cross-correlation) 1500 hours (ACA stand alone) 13. Comments on observing strategy : -------------------------------------------------- Review v2.0: 1.4.2 The requested rms level is 2 micro Jy (for both band 3 and 6, presumably; please indicate explicitly). The authors estimate that integration time of 30 hours per pointing for band 3 observations with ACA and 12-m array cross correlations, yet much shorter integration is OK for band 3, and slightly longer integration seems to be needed for band 6. Please check together with the justification of the total requested integration time. The authors request an absolute calibration accuracy of 5 %. I am wondering if there is a clear reason to justify this calibration accuracy. I understand the *relative* accuracy between band 3 and 6 is essential for this project, but the requirement for *absolute* one is somewhat unclear. In the band 6 observations, we may also detect significant numbers of SMGs toward high-z clusters of galaxies; strategy for careful removal of them will be an issue. ===================================================================================== DRSP 1.5.1 Title Imaging Molecular material in the vicinity of an AGN Pi E. Schinnerer Time 64 hrs 1. Name of program and authors 1.5.1: Name -- Imaging Molecular material in the vicinity of an AGN Authors: E. Schinnerer 2. Science goal: Molecular gas has been detected within a radius of 10pc of a Seyfert nucleus (correspinding to 0.12'' at a distance of 17 Mpc). Here we propose to map the CO(2-1) line emission at 0.06" resolution in a sample of 2 nearby AGN in order to resolve their nuclear molecular reservoir. Finding more molecular gas within a few pc of the BH is essential to understand the actual process of feeding the AGN. These data will also allow us to test dynamical models of the gas flow which include the presence of BH. Ultimately, this method will allow measuring BH masses using the molecular line emission due to the high spectral resolution provided by ALMA. 3. Number of sources: 2 4. Coordinates: 4.1. N1068, N1097 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.06" 5.2. Range of spatial scales/FOV: 0.06" to 25" 5.3. Required pointing accuracy: ~ 1" 6. Observational setup 6.1. Single dish total power data: no 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 6 -- 220 GHz in Configuration AB 7.2. Lines and Frequencies (GHz): CO(2-1) @ 230 GHz 7.3. Spectral resolution (km/s): 5 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): ~ 1200 km/s 8. Continuum flux density: 8.1. Typical value (Jy): 8.2. Required continuum rms (Jy or K): 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) 8.4. Calibration requirements: absolute ( 5% ) repeatability ( 5% ) relative ( 5% ) 9. Line intensity: 9.1. Typical value (K or Jy): <= 1 mJy/beam at 230 GHz 9.2. Required rms per channel (K or Jy): 0.2 mJy/beam 9.3. Spectral dynamic range: 5 - 10 9.4. Calibration requirements: absolute ( 5% ) repeatability ( 5% ) relative ( 5% ) 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 2 track (+/- 4hr) at 230 x 2 sources x 2 configurations 12. Total integration time for program (hr): 64 hr 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): ----------------------------------------------------------------------------- Revised version of drsp1_1.5.1.txt. *************************************************************************** Comments: revised to go to 0.06" resolution --> The requested resolution is already 0.06", abstract has been clarified The abstract proposes to map CO(2-1) line emission in 6 AGN, but the proposal seems to be for two sources only. That seems sufficient. --> Abstract corrected to 2 sources. proposal looks ok ************************************************************************* Previous comments: Review Jean Turner: Science case is good; the behavior of molecular gas near AGN is of great interest for many reasons, kinematics, star formation triggering, AGN fueling. This will certainly be something done early on by ALMA. The high resolution is justified. Scope is reasonable: one can learn much from studies of a single nearby system. This is high resolution for CO(2-1). While 0.02" is justified by the sizescales of the source -- this corresponds to 1-2 pc at these distances -- there is not a lot of power in this beam. 20K gas will be detectable only at 3 sigma. Possibilities: higher J CO lines, since one might expect warm gas in these regions, and lower resolution. The Doppler shifting will give you the resolution better than the beam if you have the signal to noise; in theory 0.1" at 20:1 signal to noise would give you roughly equivalent Doppler positional information to .02", and the 1 sigma sensitivity would be 0.24 K rather than 6K. Could do CO(3-2) also. ==>recommend 0.1" resolution Also, dust continuum will be very useful for tracing gas distribution. Integration time in the proposal checks out, but see comments above regarding beamsize. Reply Schinnerer: I changed the required resolution to 0.06" (~ 5pc at 17Mpc distance). Spatially resolving the nuclear molecular gas reservoir around an AGN is important, especially with respect of a possible flaring of the molecular gas layer in z-direction, or a complicated structure (e.g. warping of the molecular disk). This information cannot easily be recovered from the Doppler positional information alone. A resolution of 0.06" will still allow to (at least) partially resolve a possible central reservoir of molecular gas with a diameter of ~ 20pc while providing a 1 sigma line sensitivity of about 1.34 K. This sensitivity should be sufficient to detect warmer molecular clouds (T => 20 K) close to the AGN with reasonable S/N of ~ 10. This appears to be a good compromise between sensitivity and resolution requirements. I agree that higher J-transitions might be a good alternative. However, since there are no good estimates yet for CO(3-2) line intensities close to an AGN, time estimates based on CO(2-1) appear more reliable at the moment. ===================================================================================== DRSP 1.5.2 Title Circumnuclear Starburst Rings: From Gas to Stars Pi E. Schinnerer Time 80 hrs 1. Name of program and authors 1.5.2: Name -- Circumnuclear Starburst Rings: From Gas to Stars Authors: E. Schinnerer 2. Science goal: We will perform a high-resolution imaging (5-10pc) study of the molecular gas, including individual GMC complexes, in a sample of nearby (D ~ 17 Mpc) spiral galaxies containing circumnuclear starburst rings which are generally associated with large-scale stellar bars. These rings have typical diameters of about 1 kpc and are the sites of massive star clusters similar to those observed in merging systems. Comparison to high-resolution optical and NIR imaging data as well as radio continuum data will allow us to study the process of star formation from the gas phase via HII regions to 'fossil' star clusters. This comprehensive data set will allow us to access the process of star formation in an environment with short dynamical timescales. In addition, the gas kinematics and distribution will be compared to dynamical models for the gas flow in such circumnuclear rings. For a direct comparison to the models it is essential that the entire gas content is observed to test whether the assumption of continuity in the models is valid. This study has also direct consequences for possible feeding mechanisms of nuclear BH or star clusters. 3. Number of sources: 10 4. Coordinates: 4.1. Virgo cluster targets plus others 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.05" 5.2. Range of spatial scales/FOV (arcsec): 0.05" to 15" 5.3. Required pointing accuracy: ~ 1" 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: on-the-fly mapping 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: required 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 6 -- 230 GHz in Configuration ABCD 7.2. Lines and Frequencies (GHz): CO(2-1) @ 230 GHz 7.3. Spectral resolution (km/s): 2-3 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): ~ (800 - 1000) km/s 8. Continuum flux density: 8.1. Typical value (Jy): < 0.5 mJy/beam at 230 GHz 8.2. Required continuum rms (Jy or K): 8.3. Dynamic range within image: 8.4. Calibration requirements: absolute ( n/a ) repeatability ( n/a ) relative ( n/a ) 9. Line intensity: 9.1. Typical value (K or Jy): <= 60 mJy/beam at 230 GHz 9.2. Required rms per channel (K or Jy): 0.6 mJy/beam 9.3. Spectral dynamic range: 5 - 100 9.4. Calibration requirements: absolute ( 5% ) repeatability ( 5% ) relative ( 1-3% ) 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 1 track (+/- 1hr) at 230 x 10 sources x 4 configurations 12. Total integration time for program (hr): 80 hr 13. Comments on observing strategy : (optional) Tracing the gas flow in the centers of galaxies depends critically on measuring the distribution of the entire (molecular) gas. Thus short spacings are essential to probe diffuse extended material. ----------------------------------------------------------------------------- Revised version of drsp1_1.5.2.txt. The science goal has been up-dated and slightly modified thus some of the previous comments might not be relevant anymore. ************************************************************************* Comments: science goal.. surely the distance is 17 Mpc.. not kpc --> Corrected the science goal seems now to partially overlap with 1.5.1.. study of the gas flow feeding the back hole. However the emphasis is on the study of the formation of star clusters in starburst rings. This is definitely very interesting. --> Indeed, the emphasis of this project is on the onset, the continuation and possible determination of star formation in small rings around galactic nuclei. While the star formation might interact with the feeding of a (putative) black hole, it is not clear at all how and when in time, thus the science questions posed here are clearly distinct from 1.5.1. The number of sources proposed is 10. I don't understand why 10.. 1 could already be very interesting. Any number between 1 and 10 could be ok too. --> The geometry of starburst rings depends heavily on the shape of bar (strong, weak) as well as the gravitational potential of the bulge (early vs. late Hubble type). In addition, starburst rings have diameters ranging from a few 10pc to several 100pc and some galaxies host even two nuclear rings within their inner kiloparsec. Thus in order to be able to identify mechanisms for star formation that are similar in all types of starburst rings and to isolate the environmental effects a sample of 10 galaxies appears to be the bare minimum for some statistical analysis. estimated time is ok ************************************************************************* Previous comments: Review Jean Turner: Starburst rings are good targets, not well understood, and neither is SSC formation. Putting CO together with high resolution optical and near-IR imaging can provide useful circumstantial evidence for how star formation proceeds. Number of targets is somewhat arbitrary but about right; could reduce the time request to half and still have enough galaxies to discern patterns. Technical aspects. There will not be much power on the smallest angular scales, I don't think you will gain much in these galaxies below ~0.08-0.1" (1K). However, this is a multiconfiguration proposal, so that would perhaps mean one configuration's worth of data, and you never know, there could be hot spots. So this is okay. This project does not really need ACA or single dish since the focus is GMCs. 230 GHz is good for GMCs and for the primary beam, since the starburst rings are ~10-15" in size (1 kpc). Higher frequency CO lines may not show up due to excitation, and will have smaller primary beams. Integration time is reasonable. ===================================================================================== DRSP 1.5.3 Title Nuclear Dense Gas in Active Galaxies Pi E. Schinnerer Time 256 hrs 1. Name of program and authors 1.5.3: Name -- Nuclear Dense Gas in Active Galaxies Authors: E. Schinnerer, S. Garcia-Burillo 2. Science goal: The polar molecule HCN is commonly used as a tracer of dense molecular gas. The correlation between the HCN luminosity and the far-infrared (FIR) luminosity is found to be tighter than the well-known correlation between the CO luminosity and the FIR luminosity, and more importantly, the HCN-FIR correlation remains linear to high FIR luminosity, unlike the CO-FIR correlation, which 'saturates' at high FIR luminosity. Since HCN is a dense gas tracer, likely associated with active star forming regions, the linear HCN-FIR correlation suggests that the FIR luminosity originates from star formation rather than AGN activity in IR luminous galaxies. However, the HCN to CO intensity ratio varies substantially among luminous galaxies, which may indicate variation of the star formation efficiency (= star formation rate/total molecular gas mass) as a function of IR luminosity. The excitation conditions for HCN can be met either in star forming regions, or in gas close to the nuclei of galaxies, where AGN may heat the gas and dust. Recently, the HCN to HCO+ ratio has been suggested as a good discriminator between excitation due to an AGN (X-ray dominated regions; collisional excitation) or due to star formation (IR pumping; non-collisional excitation). Therefore, we propose to simultaneously image HCN and HCO+ (their first 4 transitions) in a representative sample of starburst and AGN galaxies to identify the excitation source of both HCN and HCO+ and to test whether their ratios can indeed be used as discriminator indepedent of transition. Note that in the case of high-J transitions of both HCN and HCO+ IR pumping might indeed play a vital role. In addition, high angular resolution is vital to spatially resolve possible nuclear star forming regions and the AGN itself. A good understanding of the excitation conditions of HCN and HCO+ are also paramount for the interpretation of observations of dense molecular gas in galaxies at high redshifts (z > 4) which will be routinely done with ALMA using high-J transitions. 3. Number of sources: 4 4. Coordinates: 4.1. active galaxies at ~10 - 20 Mpc distance: 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.1" 5.2. Range of spatial scales/FOV (arcsec): 0.1" to 15" 5.3. Required pointing accuracy: ~ 0.5" 6. Observational setup 6.1. Single dish total power data: no 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: 3,5,6,7 7.2. Lines and Frequencies (GHz): HCN/HCO+(1-0),(2-1),(3-2),(4-3): 88, 178, 266, 356 GHz multi-line 2 lines per setting per band 7.3. Spectral resolution (km/s): 20 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): ~ 1200 km/s per line; total bandwidth ~ 1.5-2 GHz (depends on line separation) 8. Continuum flux density: 8.1. Typical value (Jy): < 0.5 mJy/beam at 230 GHz 8.2. Required continuum rms (Jy or K): 8.3. Dynamic range within image: 8.4. Calibration requirements: absolute ( n/a ) repeatability ( n/a ) relative ( n/a ) 9. Line intensity: 9.1. Typical value (K or Jy): ~ 0.9 mJy/beam at 266 GHz 9.2. Required rms per channel (K or Jy): 0.15 mJy/beam 9.3. Spectral dynamic range: >5 9.4. Calibration requirements: absolute ( 5% ) repeatability ( 5% ) relative ( 5% ) 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): 1 track (+/- 4hr) at 266 x 4 sources x 2 configurations x 4 frequency set-ups The assumption is that the line intensity and rms noise do roughly scale with frequency. 12. Total integration time for program (hr): 256 hr 13. Comments on observing strategy : (optional) ----------------------------------------------------------------------------- Revised version of drsp1_1.5.3.txt. The science goal has been up-dated and slightly modified thus some of the previous comments might not be relevant anymore. ************************************************************************* Comments: proposes to simultaneously image HCN and HCO+ in 5 transitions in a representative sample of AGn and starburst.. consisting of 4 sources. The proposal only discusses 4 transitions --> The abstract has been corrected to 4 transitions. I don't see why two sources, one AGN and one starburst would not be enough. this is a huge amount of time. --> Given that the HCN/HCO+ lines are of high interest in high redshift sources understanding their chemistry in local well defined counterparts is paramount. Given the fact that at the resolution ALMA will achieve source properties are basically unknown, a sample of having 2 AGN and 2 pure starbursts seems the best way to avoid misinterpretation of results in case one source might turn out to host both AGN and starburst. Also, this will help to sample a possible wider range in nuclear properties such as the ionization strength of the AGN and the age and SFR rate of nuclear starbursts. ************************************************************************* Previous comments: Review Jean Turner: HCN is an interesting molecule for starbursts. One issue is the one that Phil Solomon has pointed out, that HCN is better correlated with Lir than CO. This is worth pursuing with high spatial resolution. HCN could well trace the star formation much better than CO (and presumably these galaxies would all already have comparable CO maps). However, it seems to me premature to do 10 sources. HCN could be confusing. Especially in exotic objects, with a lot of mid-IR emission. With the high spatial resolution one can isolate the AGN to some degree and perhaps simplify the problem to learn interesting things about dense gas and HCN in these two different categories of systems. This project will be done by ALMA. I think the dust continuum will be exceedingly useful in helping out with where the gas is (this would potentially require band 3 to weed out the free-free contribution) Scope: I think this is an awful lot of time to devote to HCN. At the moment it is unclear how much one might learn, with potential excitation issues, particularly in AGN, but anywhere there is strong mid-IR emission. Ewine will know better about the mid-IR pumping of HCN. If there are SSCs forming, there is VERY strong and localized mid-IR. Ditto AGN. Two galaxies carefully chosen galaxies would be sufficient to reveal unusual HCN properties. Technical: High resolution is needed to separate AGN; however, too high is not good for molecules. They propose 0.1", this is a reasonable compromise. Integration time is fine per galaxy. Total time for project should be cut, to possibly 2 sources instead of 10, for a total of 32 hrs. Comment Ewine: Both collisions and mid-IR pumping can indeed affect the HCN excitation in these hot cores. Two sources seems too few to me to test any relation, so I propose to cut to 6 sources = 96 hrs ===================================================================================== DRSP 1.5.4 Title Excitation Conditions of Nuclear GMCs Pi E. Schinnerer Time 75 hrs 1. Name of program and authors 1.5.5: Name -- Excitation Conditions of Nuclear GMCs Authors: E. Schinnerer, D.S. Meier 2. Science goals: Massive star formation as well as the presence of an active galactic nucleus (AGN) can impact the excitation conditions for CO line emission from the centers of galaxies. Therefore the derived molecular gas mass can be vastly overestimated, thus leading to wrong estimates about the star formation efficiency and the amount of gas available for future star formation events. Using multiple 12co transitions (1-0, 2-1, 3-2, 4-3, 6-5) allows the direct measurement of the temperature and density of individual molecular cloud complexes as well as the more extended diffuse gas via Large Velocity Gradient (LVG) analysis. The comparison of properties between the GMCs and the diffuse gas will provide important insight into the life cycle of molecular gas in the centers of galaxies. The high angular resolution is essential to resolve the gas into individual GMCs (avoiding blending) as well as for the separation of the diffuse component from the GMCs. Finally this dataset will provide local gas excitation templates for high z galaxies, where it is these high excitation lines that lay within the ALMA bands 3. Number of sources: 5 4. Coordinates: 4.1. all over sky, in 5 - 20 Mpc distance 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.2" 5.2. Range of spatial scales/FOV (arcsec): 0.2" - 20" single-field, small mosaic (at higher frequencies) 5.3. Required pointing accuracy: ` 0.5" (for pointing at high frequencies) 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: frequency switch; position switch; on-the-fly mapping; 6.2. Stand-alone ACA: required 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: required 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3, 6, 7, 8, 9 7.2. Lines and Frequencies (GHz): CO(1-0), CO(2-1), CO(3-2), CO(4-3), CO(6-5) 7.3. Spectral resolution (km/s): 5 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): ~ 1200 km/s 8. Continuum flux density: 8.1. Typical value (Jy): 8.2. Required continuum rms (Jy or K): 8.3. Dynamic range within image: 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 9. Line intensity: 9.1. Typical value (K or Jy): 10 mJy at 115 GHz (~ 300 mJy at 691 GHz) 9.2. Required rms per channel (K or Jy): 0.5 mJy at 115 GHz (6 mJy at 691 GHz) 9.3. Spectral dynamic range: 5 - 100 9.4. Calibration requirements: absolute ( 1-3% ) repeatability ( 1-3% ) relative ( 1-3% ) 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): 30min - 1hr per band per configuration per source 12. Total integration time for program (hr): 75 hr 13. Comments on observing strategy : short spacing information is crucial to derive accurate line ratios ----------------------------------------------------------------------------- ************************************************************************* Comments: I don't understand why this project needs the 7m x 12m cross correlations, but not standalone ACA. I would naively think that the ACA beaselines (+ total power) would deal quite well with the shorter spacings, while the few extra baselines we get by recording the 7m x 12m correlations would not increase the sensitivity by very large amounts. R.: It was my understanding that baselines between 7m antennas would be included as well. I have added the requirement for ACA stand-along observations. I agree that the best sampling possible of the uv plane is critical for this project. ===================================================================================== DRSP 1.5.5 Title Physical Condition for the Gas in Galactic Centers Pi E. Schinnerer Time 240 hrs 1. Name of program and authors 1.5.6: Name -- Physical Condition for the Gas in Galactic Centers Authors: E. Schinnerer, D.S. Meier 2. Science goal: Molecular gas is abundant in the central kiloparsec of nearby star forming galaxies. Generally, it is believed that large-scale structures such as stellar bars and/or spiral arms cause this pile-up of gas in the galactic centers which might then be transformed into stars. However, it is not clear what physical conditions are responsible for the excitation of the molecular gas seen in its 12co(1-0) line emission. By combining observations of molecules such as, e.g., HCN, CS, HCO+, CH3OH, HNC, CCH, N2H+, SiO, and HC3N one can probe if the physical environment is dominated by kinematic shocks (due to stellar bars causing the gas to move inward), embedded star formation (still invisible in the optical to NIR wavelengths) or photon dominated regions (caused by already developed HII regions). Gaining insight into the actual physical state of the molecular gas is of great importance as the star forming process in the galactic centers must proceed under very different conditions compared to the disk: the interstellar radiation field becomes stronger while the dynamical timescales become much shorter (< 1e7 yr). Angular resolution on the GMCs scale is paramount to avoid confusion between the molecular cloud complexes and the more diffuse extended gas. The high spectral resolution is required to resolve shock fronts that are expected to be present in barred galaxies. 3. Number of sources: ~ 5 nearby (barred) starburst galaxies 4. Coordinates: 4.1. random over sky, out to ~ 10-15 Mpc 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.05" 5.2. Range of spatial scales/FOV (arcsec): 0.05" --> 20" single-field 5.3. Required pointing accuracy: 0.5" 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: on-the-fly mapping 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: required 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3 7.2. Lines and Frequencies (GHz): multi-line 3 frequency settings in Band 3 7.3. Spectral resolution (km/s): 5 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): ~ 600 km/s per line with a maximum bandwidth of 8 GHz for most multiplexing freedom 8. Continuum flux density: 8.1. Typical value (Jy): 8.2. Required continuum rms (Jy or K): 8.3. Dynamic range within image: 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 9. Line intensity: 9.1. Typical value (K or Jy): 1.25 - 2.5 mJy 9.2. Required rms per channel (K or Jy): 0.1 mJy 9.3. Spectral dynamic range: 5 - 30 9.4. Calibration requirements: absolute ( 5% ) repeatability ( 5% ) relative ( 5% ) 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): 1 track (+/- 2hr) x 5 sources x 4 configurations x 3 frequency settings 12. Total integration time for program (hr): 240 hr 13. Comments on observing strategy : Short spacings are important for good imaging fidelity as well as to trace the distribution of the various molecules probing different physical conditions such as photon dominated regions, shocks and cold dense clouds. ----------------------------------------------------------------------------- ************************************************************************* Comments: this proposal requires cross correlations of 7m ACA and 12 m baseline-ALMA short spacings are indeed very important for this project they propose to do 5 sources without any justification for that number. R.: Given our experience from local nearby galactic nuclei, it is clear that the ongoing and/or recent star formation history in the centers will likely have an impact of the molecular gas properties in form of consumption of gas, ionization, mechanical impact etc. In addition, the exact bar properties (only a large-scale or a nuclear bar, double barred, strong bar vs. oval, etc.) will also shape the dynamical and physical properties of the molecular gas. Thus it is paramount to have a large enough sample to discriminate general trends from unusual but very localized conditions. Huge amount of time, but very interesting science.. ===================================================================================== DRSP 1.6.1 Title High resolution imaging of radio hot spots Pi C. Carilli Time 32 hrs 1.6.1: Name -- High resolution imaging of radio hot spots Authors: C. Carilli 2. Science goal: We will perform high resolution imaging at 100, 220, and 650 GHz of the radio hot spots, and jets, of the archtype powerful radio galaxies Cygnus A and Pictor A. These data, combined with VLA images at 8, 22, and 43 GHz, will provide the definitive test of particle acceleration and loss mechanisms in the hot spots (=terminal jet shocks) of powerful radio galaxies. The required sensitivities and dynamic ranges are extrapolated from existing 43 GHz images based on reasonable physical models for first order Fermi acceleration, and synchrotron radiative losses, at terminal jet shocks (Carilli et al. 1999, AJ 118, 2581; Perley et al. 1997, A&A, 328, 12). In particular, the 650 GHz imaging is in the critical range where an exponential cut-off is expected due to radiative losses during the finite shock crossing time of the electrons. These observations will delineate in detail the regions of most active particle acceleration, and can be used to determine hot spot magnetic field strengths and relativistic particle energy densities, independent of minimum energy assumptions. Observations of the inner jets will constrain particle acceleration processes along the jet, thought to occur in oblique (weak) shocks within the jets. Resolution must be matched to that of the VLA observations = 0.2". 3. Number of sources: 2 4. Coordinates: 4.1. 1957+4035, 0518-4548 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.2" 5.2. Range of spatial scales/FOV: 0.2" to 8" 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 -- 100 GHz in Configuration A Band 6 -- 220 GHz in Configuration B/C Band 9 -- 650 GHz in Configuration D 6.2. Lines and Frequencies 6.3. Spectral Resolution (km/s) 6.4. Bandwidth or spectral coverage: standard continuum 7. Continuum flux density: 7.1. Typical value: >= 1 mJy/beam at 100 GHz >= 0.5 mJy/beam at 250 GHz >= 0.1 mJy/beam at 650 GHz 7.2. Continuum peak value: Hot spots: 45 mJy/bm at 100 GHz 26 mJy/beam at 250 GHz 15 mJy/beam at 650 GHz Cores: 0.5 to 1 Jy 7.3. Required continuum rms: 0.01 mJy/bm at 100 GHz 0.02 mJy/beam at 250 GHz 0.06 mJy/beam at 650 GHz 7.4. Dynamic range in image: 5000 8. Line intensity: 8.1. Typical value: 8.2. Required rms per channel: 8.3. Spectral dynamic range: 9. Polarization: yes 10. Integration time per setting: due to small PB, each track will cycle through 3 pointing positions = 2 hot spots + core. 1 track (+/- 2hr) at 100 x 2 sources 1 track (+/- 2hr) at 250 x 2 sources 2 track (+/- 2hr) at 650 x 2 sources 11. Total integration time for program: 32 hr ********************************************************************** Review Jean Turner: This multifrequency study of prototypical radio galaxies is well justified, the sources are classic, and there is good motivation for going to high (650 GHz) frequency where break in spectrum is anticipated. Scope is also good; these are two sources in which a detailed, multiwavelength and concentrated study can be very productive. Technical aspects are fine, resolution to match VLA. Integration times are okay, agree with proposal, but are a little arbitrary. Could use more time at 650 GHz relative to 100 GHz, but total request is about right for this project. -------------------------------------------------- Review v2.0: 1.6.1 High resolution imaging of radio hot spots (Carilli) Not revised since DRSP 1.1. Nothing needs to be added to the review back then, no severe impact through reduction to 50 antennas, no need for ACA. ===================================================================================== DRSP 1.6.2 Title High resolution imaging of X-ray hot spots in radio Pi C. Carilli Time 16 hrs 1.6.2: Name -- High resolution imaging of X-ray hot spots in radio jets Authors: C. Carilli 2. Science goal: We will perform high resolution imaging at 100 and 350 GHz of the X-ray detected hot spots in the jets of the archtype jet sources M87 and 3C273. X-ray detected jet knots provide the most severe constraints on particle acceleration and emission mechanisms within radio jets, with radiative lifetimes that can be measured in years. The spectral properties of these hot spots are well constrained at cm, and optical to Xray wavelengths. The proposed observations will provide the key link between the cm and optical/Xray regime, and hence provide critical constraints on emission mechanisms (eg. synchrotron or inverse compton) for the Xrays, as well as constraints on particle acceleration mechanisms in the jets (see review by Harris 2003, astroph 0302097). Resolution must be matched to that of the Chandra and the VLA observations (0.5"). 3. Number of sources: 2 4. Coordinates: 4.1. 1229+0203, 1230+1223 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.2" 5.2. Range of spatial scales/FOV: 0.5" to 15" 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 -- 100 GHz in Configuration B Band 7 -- 350 GHz in Configuration D 6.2. Lines and Frequencies 6.3. Spectral Resolution (km/s) 6.4. Bandwidth or spectral coverage: standard continuum 7. Continuum flux density: 7.1. Typical value: 7.2. Continuum peak value: Cores: 5 to 10 Jy 7.3. Required continuum rms: 1 mJy/bm at 100 GHz 1 mJy/bm at 350 GHz 7.4. Dynamic range in image: 10000 8. Line intensity: 8.1. Typical value: 8.2. Required rms per channel: 8.3. Spectral dynamic range: 9. Polarization: yes 10. Integration time per setting: 1 track (+/- 2hr) at 100 x 2 sources 1 track (+/- 2hr) at 350 x 2 sources 11. Total integration time for program: 16 hr ********************************************************************** Review Jean Turner: Submillimeter observations provide important spectral link between optical-Xray and radio for hot spots. Good project, amount of time about right to devote to this (modest). Technical: angular resolution to match VLA and Chandra. Required sensitivity not explained here. To achieve this level of sensitivity, given the concentration of flux in these sources, requires a high dynamic range of 10,000:1. Integration time seems to be driven by uv-coverage and dynamic range rather than sensitivity. -------------------------------------------------- Review v2.0: 1.6.2 High resolution imaging of X-ray hot spots in radio jets (Carilli) Not revised since DRSP 1.1. Nothing needs to be added to the review back then, no severe impact through reduction to 50 antennas, no need for ACA. ===================================================================================== DRSP 1.6.3 Title Imaging the molecular gas in high redshift FIR-luminous Pi C. Carilli Time 60 hrs 1.6.3: Name -- Imaging the molecular gas in high redshift FIR-luminous QSOs Authors: C. Carilli 2. Science goal: We propose high resolution (0.2") imaging of the CO emission from high redshift (z=4 to 6.4) QSOs. Studies of high redshift QSOs have shown that about 30% of the sources are luminous FIR sources, corresponding to thermal emission from warm dust, with dust masses >= 1e8 M_sun (eg. Omont et al. 2003, A&A 398, 857; Carilli et al. 2002 ApJ 555, 625). In all cases studied with adequate sensitivity (and redshift accuracy), CO emission has also been detected, with typical line peak flux densities for the 5-4 transition (redshifted to band 3 of ALMA) >= 2 mJy. Various lines of argument suggest that the dominant dust heating mechanism is star formation, implying star formation rates of order 1e3 M_sun/year, although the AGN could also contribute to the dust heating. The coexistence of massive starbursts and major accretion events onto supermassive black holes, is consistent with the idea of coeval SMBH-galaxy formation at high redshift, as suggested by the close correlation between black hole mass and bulge mass seen in nearby spheroidal galaxies. Imaging the CO emission provides the only means of determining the dynamical mass of the host galaxy, and also provides information on the nature and physical conditions of the earliest galaxies. In particular, determining the distribution of the molecular gas and dust relative to the AGN could help to constrain the dust heating mechanism, as well as reveal complex/multiple sources, as might be expected in for hierarchical structure formation. We will observe a representative sample of 5 sources using band 3 in A configuration (0.17" resolution). The typical sizes inferred for the CO emitting regions are between 0.2 and 2". Assuming a characteristic size of order 1" implies a typical expected surface brightness of about 0.1 mJy/beam for a 50 km/s channel. 3. Number of sources: 5 4. Coordinates: 4.1. Choose equatorial sources from SDSS/DPSS, selected as FIR-luminous QSOs from single-dish bolometer surveys (eg. next generation MAMBO/SCUBA), and detected in CO emission using LMT or GBT (or small configuration ALMA survey). 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.17" 5.2. Range of spatial scales/FOV: 0.17" to 4" 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 -- 100 GHz in Configuration A 6.2. Lines and Frequencies 6.3. Spectral Resolution (km/s) 50 km/s 6.4. Bandwidth or spectral coverage: 8 GHz (for continuum sensitivity) with 512 spectral channels/polarization 7. Continuum flux density: 7.1. Typical value: 1 mJy 7.2. Continuum peak value: 7.3. Required continuum rms: 0.002 mJy/beam 7.4. Dynamic range in image: 8. Line intensity: 8.1. Typical value: 0.1 mJy/beam/channel 8.2. Required rms per channel: 0.035 mJy/beam/channel 8.3. Spectral dynamic range: 9. Polarization: no 10. Integration time per setting: 5 sources at 2x6 hrs per source 11. Total integration time for program: 60 hr Notes: could be included in 1.1 or 1.5. A parallel program could be to search for CO emission from high z QSOs, but this could also be done with LMT/GBT. The unique aspect of ALMA is the high resolution imaging. For some sources it might be possible to do multiple transitions (eg. 5-4 and 6-5) within band 3 simultaneously, thereby allowing for study of excitation gradients. ************************************************************************ Review Jean Turner: An area which is very popular right now, and in which not very much is known. 60 hours is not much time, given how much there is to be learned here; even a detection gives a lot of information about the early universe. The total time for this project could easily be increased given the present interest in these galaxies. ALMA is better suited to this study than the LMT because of the high resolution. Technical: angular resolution is appropriate. 12 hours per source is actually not much time for these sources. They're weak. However at the moment this is somewhat arbitrary. (It's actually difficult to judge this proposal for that reason, not much is known now and it's all pretty arbitrary) Integrations: checked and numbers about right. See 1) about total increase in time. I'm guessing ALMA will spend a LOT more time on this area, given recent experience at OVRO. Comment Ewine: some of these sources will likely also be covered in section 1.1. Since there will be many of these types of programs, it is good to have some duplicates with slightly different strategies. Increase sample here to 10 sources => 120 hr assuming 12 hr/source -------------------------------------------------- Review v2.0: 1.6.5 Imaging the molecular gas in high redshift FOR-luminous QSOs (Carilli) Not revised since DRSP 1.1. Nothing needs to be added to the review back then, no severe impact through reduction to 50 antennas, no need for ACA. I agree that this is a quite hot topic right now, and even though a lot of progress has been made, particularly with PdB, since the last review, the topic will most likely not be exhausted when ALMA comes on line, we'll see a lot more proposals like that, for a larger sample, and possibly also for higher resolution. ===================================================================================== DRSP 1.6.4 Title Search for flat spectrum mm-loud AGN Pi C. Carilli Time 20 hrs 1.6.4: Name -- Search for flat spectrum mm-loud AGN Authors: C. Carilli 2. Science goal: We will search for flat spectrum, mm-loud AGN. The search can be piggy-backed on the standard pre-observation calibrator searches using band 3 during normal observations. A follow-up snapshot survey (1 min/source) will then be done at 220 GHz of 1000 candidate sources, and at 22 GHz with VLA, to determine the cm to (sub)mm spectra of the sources. The search could reveal new population of faint blazars, IDVs, HFPs, and other types of known sources at more than 10 times deeper levels that is currently possible (and at higher frequencies; Corray et al. 1998 AJ 115, 1388; Dellacasa et al. 2001, A&A Supp), as well as possibly reveal new classes of sources, such as very young radio jets. These can then be studied further at X- and Gamma-rays, as well as using mm-VLBI, and standard monitoring programs. 3. Number of sources: 1000 4. Coordinates: 4.1. Any 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: any (small configuration preferred at 220 GHz) 5.2. Range of spatial scales/FOV: any 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 -- piggy-back on standard calibrator pre-observation search program Band 6 -- 220 GHz follow-up 6.2. Lines and Frequencies 6.3. Spectral Resolution (km/s) 6.4. Bandwidth or spectral coverage: full 7. Continuum flux density: 7.1. Typical value: 10 mJy 7.2. Continuum peak value: 7.3. Required continuum rms: 100 GHz -- standard sensitivity for calibrator search 220 GHz -- 0.1 mJy 7.4. Dynamic range in image: 1e3 8. Line intensity: 8.1. Typical value: 8.2. Required rms per channel: 8.3. Spectral dynamic range: 9. Polarization: yes 10. Integration time per setting: 1000 sources at 1min/source at 220 GHz 11. Total integration time for program: 20 hr ************************************************************************* Review Jean Turner: Science case and scope is very good. Will use initial observations for calibrators at 3mm in piggyback mode (no cost) to search for candidates for mm-loud AGN, and this project is the followup. Potential to reveal new populations of AGN. Strategy technically and scientifically sound. Integration time is correct. This project is defined by the parameters of the search, i.e., the amount of time available. Based on current crop of mm calibrators, which number at least 50-100 with fluxes of 0.3 Jy and above, they are very likely to find interesting populations of sources with their rms of 0.1 mJy/beam in 1 minute. -------------------------------------------------- Review v2.0: 1.6.7 Search for flat spectrum mm-loud AGN (Carilli) Not revised since DRSP 1.1. Nothing needs to be added to the review back then, no severe impact through reduction to 50 antennas, no need for ACA. ===================================================================================== DRSP 1.7.1 Title The GMC Scale Chemical Anatomy of Nearby Galaxies Pi D. Meier Time 144 hrs 1. Name: The GMC Scale Chemical Anatomy of Nearby Galaxies D. Meier, J. Turner 2. One short paragraph with science goal(s): Little is known about the chemistry applicable on scales larger than a few parsecs, for example over galactic-scale structures such as spiral arms. Chemical surveys of nearby galaxies are important for understanding this large-scale chemistry. Beyond providing physical conditions and abundances for molecular clouds in specific galaxies, it will also provide insights into interesting astrochemical questions, such as what is the cosmic ray rate versus galactocentric distance? What is the ionization fraction at different galactocentric distances? Does the chemical structure of the ISM differ significantly between regions where the clouds are expected to be young (eg. nuclei, spiral arms) versus those not (eg. outer galaxy, interarm regions) and if so can this be used to ``clock'' the chemical ages of molecular clouds across the galaxy? Over what physical scale do bars, spiral arms, AGNs, and massive star forming regions (AKA "starbursts") influence the chemistry and physics of their surroundings? Can we see the chemical signature of shocks associated with galaxy dynamics? Must grain surface processing be invoked to explain the rich, molecular complexity seen, particularly in the center of galaxies, or can normal ion-molecule chemistry in especially dense or warm gas suffice? What is the molecular complexity reached in diffuse clouds and what constraint does this impose on basic chemical formation pathways? Comparisons with the study of astrochemistry in the LMC and SMC should also provide important clues on the dependence of molecular abundances to abundances of the atomic pools. 3. Number of sources: 3: 1 AGN (Centarus A, Circinus --class galaxy) 1 Starburst (NGC 253, N4945 --class galaxy) 1 "Normal Spiral" (M 83 --class galaxy) 4. Coordinates: 4.1. Distributed Across the Sky 4.2. Moving target: no 4.3. Time critical: no 1 MM BAND Line Survey: --------------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" = 10-30 pc 5.2. Range of spatial scales/FOV (arcsec): 6 pointing distributed in galactocentric radius. 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 6 6.2. Lines and Frequencies (GHz): 4 x (1 GHz*8 basebands) = 32 GHz distributed across 218 - 270 GHz 6.3. Spectral resolution (km/s): 5 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 8 GHz (as wideband as possible) 8. Line intensity: 8.1. Typical value (K or Jy): 0.03 - 10 K 8.2. Required rms per channel (K or Jy): 0.01 K 8.3. Spectral dynamic range: 3 - 1000 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): 2 hrs per receiver setting per pointing per galaxy 11. Total integration time for program (hr): (6 pnts * 4 corr. set. * 3 gals.) * 2 hrs = 144 hrs =~ 10% of sub-theme 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) Three galaxies will be selected at distances of ~5 Mpc. One AGN (eg. NGC 4945, Centarus A -like galaxy), one starburst (eg. NGC 253, N4945 -like galaxy) and one "normal" spiral (eg. M83 -like galaxy) will be selected in order to assess the impacts of starbursts, AGNs and bars/spiral arms on the chemistry. Six pointings will be distributed across each galaxy, one nuclear, one inner disk, and one outer disk (~solar radius) and three others distributed to sample particularly interesting regions (eg. spiral arms, bar ends, massive star forming regions). Four 1 GHz x 8 baseband correlator configurations will be distributed throughout Band 6 (218 - 270 GHz), making sure to catch important molecular transitions. Based on the sensitivity achieved in 2 hrs, it is conservatively estimated to be possible to detect all transitions 2 K and brighter in the Nummelin et al. 1998 Sgr B2 survey (given similar chemistries). This equates to ~100 molecular transitions over the 32 total GHz of bandwidth. Deep 1 mm continuum observations will also be obtained for free, providing measurements of N(H_2) to derive fractional abundances. Moreover, the wide bandwidth of spectral line observations will provide an opportunity to assess the line contamination of the continuum data. *************************************************************************** Review Chris Carilli: OK -------------------------------------------------- Review v2.0: The GMC scale... Meier & Turner This line survey proposal on specific local galaxies is a must-do, but modest program. Choosing to make discrete pointings in only 3 targets is reasonable. It would be interesting to get the authors' estimate of whether they're holding down the time request at the expense of getting better sampling. It would also be interesting to know what additional science results could come from coordinating targets, fields and analysis with localgal_3 `Calibrating the I_CO...' Is the ACA needed if the fields are not within a primary beam of each other? ===================================================================================== DRSP 1.7.2 Title The Molecular ISM in Low Surface Brightness Galaxies Pi Turner Time 96 hrs 1. Name: The Molecular ISM in Low Surface Brightness Galaxies --Turner et al. 2. One short paragraph with science goal(s): LSB are low surface brightness, low star formation, metal-poor galaxies which make up the most ubiquitous class of galaxies in the universe. Suppressed star formation in LSBs must stem from different physical conditions of the ISM. Detection of molecular gas in these galaxies are at the current limit of technology (O'Neil et al. 2003). Are LSBs weak in CO because they have very little molecular gas or because CO fails to trace H_2 in the low metallicity galaxies? Does the molecular ISM follow the light distribution as is HSB galaxies? Is the interstellar pressure large enough to maintain a multi-phase ISM? Can GMCs exist in such low surface density (yet rotationally massive) LSB disks, and if so are they gravitationally bound? If the molecular ISM is present and significantly clumped like in HSBs, the very low interstellar radiation field (ISRF) implies that CO photodissociation is irrelevant and that CO's weakness likely stems from molecular gas being very cold. If the ISM is not clumped then the molecular gas must be warm, very diffuse and stable against collapse. Determinations of the structure and physical conditions in LSBs will aid in separating the two possibilities. Studies of local LSBs may also provide insights into the nature of Lyman-alpha absorbers at high-z, given their apparent similarity. Moreover, the very low ISRF in LSBs will provide a complimentary dataset to local, low metallicity star forming galaxies for constraining the effects of UV photons on CO at low metallicity. Finally, constraints of the NFW cold dark matter density profiles may be obtained for these dark matter dominated galaxies. 3. Number of sources: 10, A sample distributed between massive LSB disks and small LSB dwarfs. 4. Coordinates: 4.1. distributed across the sky. 4.2. Moving target: no 4.3. Time critical: no CO J=1-0 imaging: ---------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" (50 - 100 pc @ 10 - 20 Mpc) 5.2. Range of spatial scales/FOV (arcsec): single pointing 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 6.2. Lines and Frequencies (GHz): 12CO(1-0), 114.7 GHz (20 Mpc and Ho=70) 6.3. Spectral resolution (km/s): 5 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 500 km/s max 7. Continuum flux density: 7.1. Typical value: 0.05 mJy 7.2. Continuum peak value: 0.05 mJy 7.3. Required continuum rms: 0.004 mJy 7.4. Dynamic range in image: 12 8. Line intensity: 8.1. Typical value (K or Jy): 5 mJy 8.2. Required rms per channel (K or Jy): 0.4 mJy 8.3. Spectral dynamic range: 12 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): 5 hrs per galaxy CO J=3-2 imaging: ---------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" (50 - 100 pc @ 10 - 20 Mpc) 5.2. Range of spatial scales/FOV (arcsec): small mosaic (~4 pointing) 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 7 6.2. Lines and Frequencies (GHz): 12CO(3-2), 344.2 GHz (20 Mpc and Ho=70) 6.3. Spectral resolution (km/s): 5 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 300 km/s max 7. Continuum flux density: 7.1. Typical value: 0.2 mJy 7.2. Continuum peak value: 0.8 mJy 7.3. Required continuum rms: 0.05 mJy 7.4. Dynamic range in image: 15 8. Line intensity: 8.1. Typical value (K or Jy): 45 mJy 8.2. Required rms per channel (K or Jy): 1.9 mJy 8.3. Spectral dynamic range: 24 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): 0.25 hr per pointing per galaxy 13CO J=3-2 imaging: ---------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" (50 - 100 pc @ 10 - 20 Mpc) 5.2. Range of spatial scales/FOV (arcsec): 1 field (towards brightest GMCs in the 4 brightest sources) 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 7 6.2. Lines and Frequencies (GHz): 13CO(3-2), 329.0 GHz (20 Mpc and Ho=70) 6.3. Spectral resolution (km/s): 5 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 300 km/s max 7. Continuum flux density: 7.1. Typical value: 1 mJy 7.2. Continuum peak value: 1 mJy 7.3. Required continuum rms: 0.009 mJy 7.4. Dynamic range in image: 100 8. Line intensity: 8.1. Typical value (K or Jy): 6 mJy 8.2. Required rms per channel (K or Jy): 0.6 mJy 8.3. Spectral dynamic range: 10 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): 9 hrs per galaxy 11. Total integration time for program (hr): (5 + 1)*10 + 9*4 = 96 hrs = ~7 % of sub-theme. 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) Sensitivity calculations for the CO(1-0) line emission are based on 1/4 the intensity of the brightest LSBs detected in O'Neil et al. 2003. Sensitivities for the three brightest galaxies is assumed to be equal to the brightest galaxies in the O'Neil et al. 2003 survey. Targets will be chosen at distances between 10 - 20 Mpc, as a compromise between sensitivity, areal coverage and maintaining resolution close to the individual GMC scale. 12CO(1-0) will be used to map the ISM over the central 3-6 Kpc (10 - 20 Mpc). 12CO(3-2) will be observed towards the detections as a minimum establishment of gas excitation. Towards the three brightest sources an attempt to detect 13CO(2-1) will be included for constraints on gas density and/or the CO isotopic ratio. 3mm continuum for tracing free-free emission associated with star formation will be obtained for free, simultaneously with the 12CO(1-0) data. In the 5 hrs per galaxy at 115 GHz, a 115 GHz continuum rms of 0.004 mJy or the ionizing flux of a few O7V stars. Likewise 0.8 mm continuum for tracing cool dust associated with the molecular gas will be obtained for free, simultaneously with the 12CO(3-2) and 13CO(3-2) data. In the 0.25 hrs per galaxy at 345 GHz, a 345 GHz continuum rms of 0.05 mJy or GMCs with M(H_2)>~3x10^5 Mo (at 10 Mpc) will be detected. Towards the four brightest sources the deep continuum observation simultaneous with 13CO(3-2) will provide 330 GHz continuum rms of 0.009 mJy or GMCs with M(H_2)>~5x10^4 Mo (at 10 Mpc) of dust will be detected. **************************************************************** Review Chris Carilli: OK -------------------------------------------------- Review v2.0: The molecular ISM in LSB... Turner et al. The substantial change in DRSP2 is to modify the expected continuum level down in these targets. In contrast with the other proposals sharing some/all investigators, maybe LSBs are getting more coverage as a class of galaxy? (This is intended as an encouragement to up-size the other programs more than to down-size this one). Is the ACA going to be much help for single pointings? ===================================================================================== DRSP 1.7.3 Title Calibrating the I_CO to N(H_2) Conversion Factor in Nearby Galaxies Pi D. Meier Time 140 hrs 1. Name: Calibrating the I_CO to N(H_2) Conversion Factor in Nearby Galaxies --D. Meier, J. Turner et al. 2. One short paragraph with science goal(s): Directly or indirectly, the uncertainties in the validity of the conversion factor between I_co and N(H_2) (Xco) limits precision determinations of the molecular universe. Detailed spatially resolved observations of GMCs in galaxies other than our own are vital to investigations of the reliability of CO as a mass tracer under varying influences. Does Xco depend on the dynamics of the region, that is, are virialized GMCs a requirement for the applicability of Xco? Under virial conditions it is predicted that Xco depends on n^0.5/T. Is this relation observed and if so how much data must be observed in order to establish H_2 densities and temperatures accurately enough to correct the standard value? Is Xco dependent on observed sizescale as would be expected if internal cloud structure changes with size? Is Xco a function of galactocentric distance? Does Xco obtained in lower metallicity outer disks of spirals overlap Xco determined in similar metallicity dwarfs? Finally, since it is known that the higher J transitions of 12CO are susceptible to photospheric effects, can one directly establish a 12CO(2-1) or 12CO(3-2) "conversion factors", which will be more suitably to high redshift observations, and in general, the high sensitivity "workhorse" ALMA bands? We undertake a study of the lowest three CO lines in different isotopomers to model the CO behavior in the clouds in three different environments, nine lines in total with dust continuum, following Meier et al. 2001, ApJ, 551. 3. Number of sources: 3 nearby galaxies 4. Coordinates: 4.1. Possible targets M83 SBc galaxy, gas-rich, starburst nucleus 13:37, -30 NGC1068 02:42, 00 Circinus 14:13, -65 N6822 19:44, -15 4.2. Moving target: no 4.3. Time critical: no CO J=1-0 imaging: ----------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" 5.2. Range of spatial scales/FOV (arcsec): 10 distributed fields across each galaxy 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 6.2. Lines and Frequencies (GHz): 12CO(1-0) at 115 GHz 6.3. Spectral resolution (km/s): 3 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 8. Line intensity: 8.1. Typical value (K or Jy): 10 K 8.2. Required rms per channel (K or Jy): 0.05 K 8.3. Spectral dynamic range: 200 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): 2 hr per field per galaxy (observed simultaneously with 13CO(1-0) and C18O(1-0)) 13CO J=1-0 imaging: ----------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" 5.2. Range of spatial scales/FOV (arcsec): 10 distributed fields across each galaxy 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 6.2. Lines and Frequencies (GHz): 13CO(1-0) at 110.2 GHz 6.3. Spectral resolution (km/s): 3 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 300 km/s max 8. Line intensity: 8.1. Typical value (K or Jy): 1.2 K 8.2. Required rms per channel (K or Jy): 0.04 K 8.3. Spectral dynamic range: 30 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): 2 hr per field per galaxy (observed simultaneously with 12CO(1-0) and C18O(1-0)) C18O J=1-0 imaging: ----------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" 5.2. Range of spatial scales/FOV (arcsec): 10 distributed fields across each galaxy 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 6.2. Lines and Frequencies (GHz): C18O(1-0) at 109.7 GHz 6.3. Spectral resolution (km/s): 3 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 300 km/s max 7. Continuum flux density: 7.1. Typical value: 0.1 mJy 7.2. Continuum peak value: 1 mJy 7.3. Required continuum rms: 0.006 mJy 7.4. Dynamic range in image: 17 8. Line intensity: 8.1. Typical value (K or Jy): 0.3 K 8.2. Required rms per channel (K or Jy): 0.04 K 8.3. Spectral dynamic range: 8 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): 2 hr per field per galaxy (observed simultaneously with 12CO(1-0) and 13CO(1-0)) 12CO J=2-1 imaging: ----------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.5" 5.2. Range of spatial scales/FOV (arcsec): 15 distributed fields across each galaxy 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 6 6.2. Lines and Frequencies (GHz): 12CO(2-1) at 230 GHz 6.3. Spectral resolution (km/s): 3 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 300 km/s max 8. Line intensity: 8.1. Typical value (K or Jy): 12 K 8.2. Required rms per channel (K or Jy): 0.02 K 8.3. Spectral dynamic range: 60 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): 45 minutes per field per galaxy 13CO J=2-1 imaging: ----------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" 5.2. Range of spatial scales/FOV (arcsec): 15 distributed fields across each galaxy 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 6 6.2. Lines and Frequencies (GHz): 13CO(2-1) at 220.4 GHz 6.3. Spectral resolution (km/s): 3 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 300 km/s max 8. Line intensity: 8.1. Typical value (K or Jy): 1.6 K 8.2. Required rms per channel (K or Jy): 0.02 K 8.3. Spectral dynamic range: 80 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): 45 minutes per field per galaxy (simultaneous with C18O(2-1)) C18O J=2-1 imaging: ----------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" 5.2. Range of spatial scales/FOV (arcsec): 15 distributed fields across each galaxy 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 6 6.2. Lines and Frequencies (GHz): C18O(2-1) at 219 GHz 6.3. Spectral resolution (km/s): 3 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 300 km/s max 7. Continuum flux density: 7.1. Typical value: 0.15 mJy 7.2. Continuum peak value: 2 mJy 7.3. Required continuum rms: 0.013 mJy 7.4. Dynamic range in image: 390 8. Line intensity: 8.1. Typical value (K or Jy): 0.4 K 8.2. Required rms per channel (K or Jy): 0.02 K 8.3. Spectral dynamic range: 20 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): 45 minutes per field per galaxy (simultaneous with 13CO(2-1)) 12CO J=3-2 imaging: ----------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.5" 5.2. Range of spatial scales/FOV (arcsec): 20 distributed fields across each galaxy 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 7 6.2. Lines and Frequencies (GHz): 12CO(3-2) at 345 GHz 6.3. Spectral resolution (km/s): 3 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 300 km/s max 8. Line intensity: 8.1. Typical value (K or Jy): 10 K 8.2. Required rms per channel (K or Jy): 0.2 K 8.3. Spectral dynamic range: 50 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): 3 minutes per field per galaxy 13CO J=3-2 imaging: ----------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" 5.2. Range of spatial scales/FOV (arcsec): 20 distributed fields across each galaxy 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 7 6.2. Lines and Frequencies (GHz): 13CO(3-2) at 330.6 GHz 6.3. Spectral resolution (km/s): 3 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 300 km/s max 8. Line intensity: 8.1. Typical value (K or Jy): 1.2 K 8.2. Required rms per channel (K or Jy): 0.02 K 8.3. Spectral dynamic range: 34 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): 45 min per field per galaxy (simultaneous with C18O(3-2)) C18O J=3-2 imaging: ----------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" 5.2. Range of spatial scales/FOV (arcsec): 20 distributed fields across each galaxy 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 7 6.2. Lines and Frequencies (GHz): C18O(3-2) at 329 GHz 6.3. Spectral resolution (km/s): 3 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 300 km/s max 7. Continuum flux density: 7.1. Typical value: 0.3 mJy 7.2. Continuum peak value: 3 mJy 7.3. Required continuum rms: 0.062 mJy 7.4. Dynamic range in image: 50 8. Line intensity: 8.1. Typical value (K or Jy): 0.3 K 8.2. Required rms per channel (K or Jy): 0.02 K 8.3. Spectral dynamic range: 15 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): 45 min per field per galaxy (simultaneous with 13CO(3-2)) 11. Total integration time for program (hr): ( 10 fields * (2 hr per field) +15 fields * (.5 hr per field) +20 fields * (.45 hr per field) ) * 3 galaxies = 140 hrs ~= 10% of sub-theme time 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) Three spiral galaxies will be selected from across the Hubble sequence. Targets will be chosen at distances of ~5 Mpc, as a compromise between areal coverage and resolution necessary to resolve individual GMC scale (0.5" = 12 pc @ 5 Mpc). Ten fields distributed across different galactocentric radii in each galaxy. 15 and 20 fields distributed over the regions observed in CO(1-0) will also be observed. 12CO(1-0), 13CO(1-0) and C18O(1-0) will be observed simultaneously, while each of 13CO(2-1) and C18O(2-1), and 13CO(3-2) and C18O(3-2) will be observed simultaneously. The three lowest J transitions of the three most abundant isotopomers will be used to determine the gas physical conditions robustly. Having 13CO and C18O transitions will aid in determining CO opacities as well as locating potential sites of isotope abundance anomalies. C18O emission will undoubtedly be optically thin in all clouds providing a good N(H_2) for comparison with Ico. The observing times are driven by the weakest lines, which are the C18O lines, since the CO, 13CO, and C18O lines will be observed simultaneously. 45 minutes are necessary to get >10:1 signal to noise in these lines for typical line intensities expected. In Band 3 we cannot achieve these sensitivities, but with integrations of 2 hours, we are within a factor of 2, and can detect the expected signals from C18O(1-0). (The longer integrations at Band 3 are somewhat compensated for with the bigger primary beam) The number of fields per galaxy is based on preliminary maps made at CO(1-0) and followed up at CO(2-1) and CO(3-2); we assume that there is a nonunity filling factor (true outside the nuclear region) and so one does not need to map 4x the area at Band 6, and 9x the area at Band 7. We will need matching beams at the 3 Bands. 3mm continuum, 1 mm continuum and 0.8mm continuum will be observed simultaneously with the deep isotopic line integrations. 3mm continuum will trace free-free emission associated with star formation. The sensitivity achieved at 110 GHz is equivalent to the ionizing flux of one O7V star. Dust masses will be traced with the 220 GHz and 329 GHz continuum emission. The deep integrations will allow the detection of GMCs down to M(H_2)>~2x10^4 Mo (at 5 Mpc). Observations of 3 mm, 1mm and 0.8mm continuum provides good constraints on the SED in mm/submm for reliable separation of free-free and thermal dust emission. *********************************************************************** Review Chris Carilli: OK. I get sensitivity in 1 hr at 3 km/s res at 330 GHz at 1'' res of 0.02 K. they quote a required value of 0.035, so perhaps they need a little less time? Jean Turner: Chris is right; however, to get good sensitivity for the C18O(1-0) line we actually need 2 hours rather than the 1 given in the original DSRP, and even then the rms at Band 3 is a factor of 2 higher than the other bands. I've modified the DSRP with new integration times, 2 hours at Band 3, and 45 minutes per position for Bands 6 and 7. The total comes, coincidentally, to 140 hrs (I did not plan this! It's how it worked out), which is the original value. I've also included a note as to how we chose the observing times/sensitivities for these matched line observations in Section 12. If one wants to trim time, I would suggest trimming positions rather than observing time per line. -------------------------------------------------- Review v2.0: Calibrating the I_CO... Meier, Turner et al. Seems to be a carefully argued program. Again, a less modest proposal might be justified? Will the ACA be necessary? Any gain in analysing the results on a target from `The GMC scale...' proposal localgal_1? Note also that there's a similar kind of thing from Tatematsu et al. (Was 1.7.3). ===================================================================================== DRSP 1.7.4 Title Structure of the ISM in irregular galaxies Pi C. Wilson Time 180 hrs 1. Name: Structure of the ISM in irregular galaxies C. Wilson et al. 2. One short paragraph with science goal(s) The structure of the ISM in low metallicity dwarf galaxies. Are the molecular clouds smaller as well as less luminous in CO? Do they have small CO cores surrounded by larger H2 envelopes? Are the physical properties (density, temperature) very different from gas at solar metallicities? What is the dust to gas ratio at lower metallicities? What effect does the presence of a starburst have on the ISM structure at low metallicity? Besides understanding nearby dwarf galaxies, the answers to these questions could be important for interpreting ALMA observations of high-redshift galaxies with reduced metallicities. 3. Number of sources 10, about half starburst and half non-starburst 4. Coordinates: 4.1. all over the sky (probably) 4.2. Moving target: no 4.3. Time critical: no CO J=1-0 imaging: ---------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.4" (20 pc at 10 Mpc) 5.2. Range of spatial scales/FOV (arcsec): single field (55") 5.3. Required pointing accuracy: 1" 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: nutator or OTF 6.2. Stand-alone ACA: required 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3 7.2. Lines and Frequencies (GHz): CO 115.0 GHz (redshifted for 10 Mpc and Ho = 75) 7.3. Spectral resolution (km/s): 2 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 300 km/s max 9. Line intensity: 9.1. Typical value (K or Jy): 1-4 K 9.2. Required rms per channel (K or Jy): 0.25 K 9.3. Spectral dynamic range: 20 9.4. Calibration requirements: absolute 10% repeatability 3% relative 3% 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): 7.3 hr per galaxy CO 3-2 imaging: --------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" 5.2. Range of spatial scales/FOV (arcsec): medium mosaic (19 fields) 5.3. Required pointing accuracy: 1" 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: OTF 6.2. Stand-alone ACA: required 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 7 7.2. Lines and Frequencies (GHz): CO 3-2 345 GHz (redshifted for 10 Mpc and Ho = 75) 7.3. Spectral resolution (km/s): 2 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 300 km/s max 9. Line intensity: 9.1. Typical value (K or Jy): 0.5-2 K 9.2. Required rms per channel (K or Jy): 0.1 K 9.3. Spectral dynamic range: 20 9.4. Calibration requirements: absolute 10% repeatability 3% relative 3% 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): 90 sec hr x 19 fields = 0.5 hours per galaxy 13CO 1-0 imaging: ----------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" 5.2. Range of spatial scales/FOV (arcsec): single field 5.3. Required pointing accuracy: 1" 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: nutator 6.2. Stand-alone ACA: required 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3 7.2. Lines and Frequencies (GHz): 13CO 3-2 110 (redshifted for 10 Mpc and Ho = 75) 7.3. Spectral resolution (km/s): 2 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 300 km/s max 9. Line intensity: 9.1. Typical value (K or Jy): 0.1-0.4 K 9.2. Required rms per channel (K or Jy): 0.025 K 9.3. Spectral dynamic range: 20 9.4. Calibration requirements: absolute 10% repeatability 3% relative 3% 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): 10 hr per galaxy 12. Total integration time for program (hr): 10 x (7.3 + 10 + 0.5 ) = 180 hours 13. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) Have chosen 3 CO lines as a minimum estimate of what is needed to constrain gas density and temperature in any way. Will pick targets that are reasonably close, because gain in resolution and sensitivity, but not so close that we have to mosaic at 115 GHz. 10 Mpc seems like a reasonable estimate for a typical distance. In some cases we might chose to image a piece of a galaxy rather than the whole thing. Get 110 GHz continuum sensitivity of 0.0025 mJy or 0.25 mK and 345 continuum sensitivity of 0.20 mJy or 2.1 mK for free. At 345 GHz, this is equivalent to about 1e5 Msun (1 sigma) of gas and dust within 1" at a distance of 10 pc (30 Msun/pc^2), so will only detect the biggest clouds. Should also do 12CO J=1-0 simultaneously with 13CO J=1-0 to get better sensitivity to large extended structures; doesn't remove the need for higher resolution 12CO J=1-0 imaging in its own right ... -------------------------------------------------- Review v2.0: Structure of ISM in Irr galaxies Wilson et al. Seems fine. Maybe 10 is rather more Irr galaxies than normal galaxies covered in other proposals, but given the diversity of Irr galaxies, and potential relevance to high-redshifts it's all justified. Maybe covering a fraction of the targets contiguously rather than sampling might yield more impressive early results (he speculated idly)? ===================================================================================== DRSP 1.7.5 Title Low Frequency Survey of Free-Free Emission in Nearby Starburst Galaxies Pi J. Turner Time 43 hrs 1. Low Frequency Survey of Free-Free Emission in Nearby Starburst Galaxies J. Turner et al. 2. The goal is to measure and locate free-free emission from HII regions in starbursts in nearby galaxies. The images will reveal the youngest massive star-forming regions that are optically obscured within starburst complexes. Since free-free emission at cm-wavelengths is confused with synchrotron up to 2cm, and emission from compact HII regions is still rising into the millimeter, ALMA mm continuum fluxes are more useful measures of the free-free flux than are VLA fluxes (e.g., Meier et al. 2002). Comparison with high resolution Halpha and optical multicolor HST images (which give ages for the visible star clusters) will tell us about the spatial evolution of star formation within starbursts. In the closest of the galaxies, we can trace the internal stucture of individual HII regions, of particular interest for the formation of SSCs. Comparison with SIRTF and ALMA observations of gas and dust will allow the determination of the contributions of the young HII regions to the total star formation budget, and an estimate of star formation efficiency. The submillimeter continuum fluxes will be measured in a spectral region relatively free of synchrotron and dust confusion at 3 and 1mm, at 0.15" resolution, comparable to the sizes of the HII regions themselves. A small mosaic is required to cover typical starburst regions, which are a few hundred parsecs in size. Mapping at both 3 and 1 mm allows separation of dust emission from the free-free emission. 3. Number of sources: 16 4. Coordinates: 4.1 NGC253 00:47, -25:17 NGC1365 03:31, -36:21 Circinus 14:13, -65:20 NGC4945 13:05, -49:28 M83 13:37, -29:52 NGC5253 13:40, -31:38 IIZw40 05:55, +03:23 He 2-10 08:36, -26:24 NGC1808 05:08, -37:30 NGC3256 10:27, -43:54 NGC1097 02:46, -30:16 NGC660 01:43, +13:38 NGC1068 02:40, -00:13 NGC3521 11:05, -00:02 NGC3627 11:20, +12:59 NGC3628 11:20, +13:35 4.2 Moving target: no 4.3 Time critical: no 5. Spatial scales: 5.1 Angular resolution: 0.15" (to match sizes of HII regions =~1-3 pc) 5.2 Range of spatial scales/FOV: 2'x2' fields: require point mosaics. OTF mapping can be used if efficient for the size. 1500x1500 beam images. 5.3 Single dish: yes 5.4 ACA: yes 5.5 Subarrays: no 6. Frequencies: 6.1 Receiver band: Bands 3 and 6 6.2 Continuum 6.3 Spectral resolution N/A 6.4 Spectral coverage N/A 7. Continuum flux density 7.1 Typical value 0 7.2 Continuum peak value: 20 mJy 7.3 Required continuum rms: 0.05 mJy/beam 7.4 Dynamic range in image: 400:1 maximum 8. Line Intensity N/A 9. Polarization N/A 10. Integration time per setting: 2 minutes per setting at 1mm, 1 minute at 3mm, 64 settings (2'x2' mosaic) at 1mm, 32 settings at 3mm, in each field, total of 16 fields. Total integration time, without calibration, 43 hours w/o calib, slew, rampup. ************************************************************************** Review Chris Carilli: OK. -------------------------------------------------- Review v2.0: Low-frequency survey of free-free... Turner et al. The proposal reads well, and seems sound. I suggest updating `SIRTF' to `Spitzer'. What role would eVLA have? I guess working at 7mm it would help the separation of free-free and dust further? Since it's now more concrete than it was when DRSP1 was done, maybe a sentence about it could be added? Would adding (high-frequency/isotopic?) CO maps of the same regions reveal anything useful about the dynamics in the starburst regions? ===================================================================================== DRSP 1.7.6 Title Study of Gas Masses and Star Formation Efficiencies in Nearby Galaxies Pi J. Turner Time 120 hrs 1. Study of Gas Masses and Star Formation Efficiencies in Nearby Galaxies J. Turner et al. 2. We will map CO (2-1) emission at 1.5" resolution in a representative sample of nearby gas-rich (spiral and irregular) star-forming galaxies. The goal is to do a detailed study of gas and its relation to star formation. With CO gas masses, we can determine star formation efficiencies on sizescales of 30-60 pc, using ground-based Halpha images, radio continuum, and SIRTF photometry. We choose CO (2-1) instead of the (1-0) transition to obtain simultaneous 1mm continuum measurements, which provides another constraint on gas mass. We have chosen a representative range of Hubble types, galaxies with and without starbursts; most of the galaxies have SIRTF GTO programs for fIR photometry. We will map a 10'x10' region in each of the galaxies; this will cover most of the galaxy at 20-50 pc resolution. 3. Number of sources: 4 4. Coordinates: 4.1 NGC1097 (interacting and strongly barred galaxy; 8' diameter) 02h46m19.0s -30d16m30s M83 (starburst core, normal barred spiral; 12' diameter) 13h37m00.9s -29d51m57s NGC5253 (dwarf E/S0 galaxy; efficient starburst; 5'x2') 13h39m55.9s -31d38m24s NGC4945 (large spiral; 20'x4') 13h05m27.5s -49d28m06s 4.2 Moving target: no 4.3 Time critical: no 5. Spatial scales: 5.1 Angular resolution: 1.5" 5.2 Range of spatial scales/FOV: ~10' fields: require 40^2=1600 point mosaics for each, OTF mapping (some galaxies will have rectangular maps along their disks) Images contain 400x400 beams. 5.3 Single dish: yes 5.4 ACA: yes 5.5 Subarrays: no 6. Frequencies: 6.1 Receiver band: Band 6 6.2 Continuum 6.3 Spectral resolution 4 km/s 6.4 Spectral coverage 600 km/s 7. Continuum flux density 7.1 Typical value 0 7.2 Continuum peak value: 50 mJy 7.3 Required continuum rms: 0.1 mJy/beam 7.4 Dynamic range in image: 500:1 8. Line Intensity 8.1 Typical value: 0.5 K (up to 20K) 8.2 Required rms value per channel: 0.05 K 8.3 Spectral dynamic range: 400:1 9. Polarization N/A 10. Integration time per setting: 1 minute per Nyquist setting, 1600 settings within a 10'x10' region, mosaic/OTF mode. Total integration time, without calibration, 1600 minutes = 27 hrs/galaxy. 4 galaxies x 30 hours = 120 hours about 5 days w/o calibration, slew, rampup. *********************************************************************** Review Chris Carilli: OK, but possibly overestimates required time by factor 2 since this is a mosaic. The sensitivity they quote is per 1min pointing, but the pointings overlap. However, program is only 120 hrs total, so leave as-is. -------------------------------------------------- Review v2.0: Study of gas masses and star-formation efficiencies... Turner et al. Again `SIRTF' updates desirable. In light of SINGS being more and more complete, should this modify the target choice? Is there again any chance for synergistic interpretation and target matching with other Turner et al. continuum/line surveys? Here mosaicking suggests ACA is essential component. ===================================================================================== DRSP 1.7.7 Title Gas Content and Dynamics of Elliptical Galaxies Pi C. Wilson Time 12 hrs 1. Gas Content and Dynamics of Elliptical Galaxies C. Wilson, K. Tatematsu, N. Nakai 2. In elliptical galaxies, the kinematics of the stars can be studied with optical observations. Many ellipticals contain some molecular gas, but the details of the gas content and kinematics are only known for a few galaxies. What are the properties of molecular gas in elliptical galaxies? Is it organized into similar structures as spirals (i.e. GMCs, mass function, etc.) What does molecular gas do when there isn't very much of it and there is little or no active star formation? Is there general evidence that the molecular gas in elliptical galaxies comes from mergers (major or minor)? Peak CO 2-1 line strengths in single dish survey from Lees et al. (1991) are in the range of 10-40 mK, so we will need good sensitivity. 3. Number of sources: 20 in initial survey, follow-up on 6 brightest and/or most interesting sources 4. Coordinates: 4.1. all over the sky, avoiding galactic plane 4.2. Moving target: no 4.3. Time critical: no 4.4. Scheduling constraints: no CO J=1-0 imaging: ---------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 3" 5.2. Range of spatial scales/FOV (arcsec): 60" 5.3 Required pointing accuracy: 1" 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: nutator or OTF 6.2. Stand-alone ACA: required 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3 7.2. Lines and Frequencies (GHz): 114 GHz 7.3. Spectral resolution (km/s): 10 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 1000 km/s 9. Line intensity: 9.1. Typical value (K or Jy): 20-80 mK 9.2. Required rms per channel (K or Jy): 5 mK 9.3. Spectral dynamic range: 5-20 9.4. Calibration requirements: absolute 10% repeatability 3% relative 3% 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): 1 hours per galaxy = 20 hours Followup in CO 2-1 and 3-2 on 6 interesting/bright galaxies: CO J=2-1 imaging: ---------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 1.2 5.2. Range of spatial scales/FOV (arcsec): 2 fields within 1' CO 1-0 map 5.3. Required pointing accuracy: 1" 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: nutator or OTF 6.2. Stand-alone ACA: required 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 6 7.2. Lines and Frequencies (GHz): 228 GHz 7.3. Spectral resolution (km/s): 10 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 1000 km/s 9. Line intensity: 9.1. Typical value (K or Jy): 25-100 mK 9.2. Required rms per channel (K or Jy): 6 mK 9.3. Spectral dynamic range: 5-20 9.4. Calibration requirements: absolute 10% repeatability 3% relative 3% 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): 2 hours per field x 2 fields per galaxy = 24 hours CO J=3-2 imaging: ---------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 1.0 5.2. Range of spatial scales/FOV (arcsec): 20" 5.3. Required pointing accuracy: 1" 6. Observational setup 6.1. Single dish total power data: no 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 7 7.2. Lines and Frequencies (GHz): 342 GHz (CO 3-2) 7.3. Spectral resolution (km/s): 10 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 1000 km/s 9. Line intensity: 9.1. Typical value (K or Jy): 25-100 mK 9.2. Required rms per channel (K or Jy): 6 mK 9.3. Spectral dynamic range: 5-20 9.4. Calibration requirements: absolute 10% repeatability 3% relative 3% 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): 2 hours per field x 1 field per galaxy = 12 hours 12. Total integration time for program (hr): 56 hours 13. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) -------------------------------------------------- Review v2.0: Gas Content and dynamics of elliptical galaxies Wilson et al. There's a relatively modest request to address an important and unique question. It also seems to avoid being too modest to meet a time cap. Since DRSP1 have there been developments in other areas that allow either more precise target selection, or render some of the power of ALMA less unique? I'm thinking of SAURON IFU optical work, and the possibility of a SEQUOIA array working on the LMT to make an early detection? ===================================================================================== DRSP 1.7.8 Title Gas densities and dynamics in central regions Pi N. Nakai Time 99 hrs 1. Name: Gas densities and dynamics in central regions Tatematsu, K., Nakai, N., et al. 2. One short paragraph with science goal(s) Fueling AGNs and nuclear activity on the sub-kpc scale. (May overlap with another sub-theme.) Study the gas morphology, dynamics, physical properties in nuclear regions of active galaxies (Seyferts, liners, AGN) and "apparent" normal galaxies. Example is the study by Schinnerer et al. in NGC 1068. How may active galaxies have severely warped inner disks? Can we see mini-spirals inside the Inner Lindblad Resonance that might feed the AGN? Can we detect a molecular torus very close in to the central engine? Do double-barred galaxies have a role to play in nuclear activity? Do all galaxies have massive black holes? 3. Number of sources 15, about half AGN and half non-AGN 4. Coordinates: 4.1. all over the sky (probably) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.05" (2.4 pc at 10 Mpc) 5.2. Range of spatial scales/FOV (arcsec): single field (23") 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 6 6.2. Lines and Frequencies (GHz): CO 230.0 GHz (redshifted for 10 Mpc and Ho = 75) 6.3. Spectral resolution (km/s): 10 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 1000 km/s max 8. Line intensity: 8.1. Typical value (K or Jy): 10 - 30 K 8.2. Required rms per channel (K or Jy): 1.5 K 8.3. Spectral dynamic range: 10 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): 6.6 hr per galaxy 11. Total integration time for program (hr): 6.6 x 15 = 99 hours 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) Will be important to fill the gap between pc scale measured with water-vapor maser emission and several hundred pc scale measured with existing arrays. Will pick targets that are reasonably close, because gain in resolution and sensitivity, but the number of very close AGN is limitted. 10 Mpc seems like a reasonable estimate for a typical distance. ************************************************************************ Review Chris Carilli: OK. -------------------------------------------------- Review v2.0: Gas densities and dynamics in central regions Tatematsu et al. This appears unchanged from the viable program in DRSP1. Is the target list of 15 unduly small? How big a project could the authors propose without exhausting target lists or yielding duplicate information? I suspect much more than 15 sources for 99 hours in total. Does the ACA information help to see pc-scale structure in the innermost disk? ===================================================================================== DRSP 1.7.9 Title CO(6-5) emission from a small sample of Ultraluminous Infrared Pi K. Isaak Time 65 hrs 1. Name: CO(6-5) emission from a small sample of Ultraluminous Infrared Galaxies K. Isaak, C. Wilson et al. 2. One short paragraph with science goal(s) A study of the warm dense gas in a small sample of local ULIRGs. The aim of this short project is to obtain a global measure of the warm, dense molecular gas component in a small sample of starbursting/AGN galaxies. The observations will complement existing CO(1-0) interferometer maps that have been made as well as single-dish HCN(1-0) observations, and will provide a clue as to the relative importance and physical extent of the the warm molecular gas component. Observations such as these are central to the interpretation of the results of studies of high-z galaxies where mm interferometers are used to study redshifted CO(7-6), CO(6-5) and CO(5-4). Very few, if any, local templates against which to compare line ratios exist. 3. Number of sources 10, chosen from a list of well-studied local ULIRGs eg. Solomon et al., ApJ 1997, including such objects as Arp220. 4. Coordinates: 4.1. all over the sky (probably) 4.2. Moving target: no 4.3. Time critical: no CO J=6-5 imaging: ---------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.5 5.2. Range of spatial scales/FOV (arcsec): 1-2 primary beams 5.3. Single dish total power data: yes 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 9 6.2. Lines and Frequencies (GHz): CO 690.0 GHz (redshifted to 684 GHz typically) 6.3. Spectral resolution (km/s): 20 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): ~800km/s 8. Line intensity: 8.1. Typical value (K or Jy): 1- 10 K 8.2. Required rms per channel (K or Jy): 20 mK 8.3. Spectral dynamic range: better than S/N 50 at the peak 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): average of 1 hour per field per galaxy; about half the galaxies need two fields total=15 hours CO J=1-0 imaging: ---------------- to match the CO 6-5 data ... 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.5 5.2. Range of spatial scales/FOV (arcsec): 1 primary beam 5.3. Single dish total power data: yes 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 6.2. Lines and Frequencies (GHz): CO 115.3 GHz (redshifted to 114 GHz typically) 6.3. Spectral resolution (km/s): 20 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): ~800km/s 8. Line intensity: 8.1. Typical value (K or Jy): 1-10 K 8.2. Required rms per channel (K or Jy): 40 mK 8.3. Spectral dynamic range: S/N 25 or more at peak 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): average of 5 hours per galaxy = 50 hours 11. Total integration time for program (hr): 10 x ( 300 minutes per source) = approx. 65 hrs 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) The CO(6-5) line has been chosen to explore a strength of ALMA - high sensitivity with large instantaneous bandwidth. Sources will be chosen for which observations in the lower CO transitions and HCN(1-0) already exist in order to make comparisons between different gas components. A second selection criterion will be that sources are sufficiently distant/small to be covered by one, or at most two beams. If we assume an average source size of 3", a main beam temperature in CO(1-0) of 100mK as measured with the IRAM-30m (20" beam), a CO(6-5)/CO(1-0) line ratio of 1, then we would expect a main beam temperature of around 500mK in the primary beam (9"). The emission is likely to be on a much smaller size scales than this, however. If we make the simplifying assumption that the CO(1-0) emission is uniformly distributed over a 3" x 3" extent, and that the CO(6-5) is confined to small regions of say 1" x 1", then we arrive at a peak main beam brightness of up to 10K per synthesized beam. About half of the sources will require more than one pointing to cover either two nuclei in a closely interacting system, or simply that the source is slightly larger than a single beam. Note that most of the time is spent getting matching CO 1-0 data at the same spatial and spectral resolution. If the 6-5/1-0 line ratio is less than 1, will need more time in Band 9 ******************************************************************* Review Chris Carilli: OK. -------------------------------------------------- Review v2.0: CO(6-5) emission from a small sample of ULIRGS Isaak, Wilson et al. Seems fine. What is the biggest program that the authors could forsee in the 3-year period. This seems to be very modest. Is there a reason beyond practical time requests not to cover more of the BGS ULIRGs etc? ===================================================================================== DRSP 1.7.10 Title Searching for Proto- Super Star Clusters in the Antennae Pi C. Wilson Time 20 hrs 1. Searching for Proto- Super Star Clusters in the Antennae C. Wilson 2. One short paragraph with science goal(s) The goal is to identify young massive star clusters that are still deeply embedded in molecular gas or proto-clusters i.e. dense compact cores that are massive enough to form a young massive star clusters. We need sensitivity sufficient to detect an object with 10^5 Msun of gas and dust confined to a region of space roughly 1 pc across. In the Antennae at 20 Mpc, this translates to 0.01" resolution and a detectable dust flux of 60 micro Jy. 3. Number of sources: 1 source, four fields 4. Coordinates: 4.1. Rough RA and DEC: 12 hour -15 degrees 4.2. Moving target: no 4.3. Time critical: no 4.4 Scheduling constraints: no 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.012 5.2. Range of spatial scales/FOV (arcsec): 15" x several fields 5.3 Required pointing accuracy: 1" 6. Observational setup 6.1. Single dish total power data: no 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 7 7.2. Lines and Frequencies (GHz): 350 GHz 7.3. Spectral resolution (km/s): continuum 7.4. Bandwidth or spectral coverage (km/s or GHz): 8 GHz 8. Continuum flux density: 8.1. Typical value (Jy): 60-600 micro Jy (take average value of set of objects) (optional: indicate range of fluxes within set of objects) 8.2. Required continuum rms (Jy or K): 15 micro Jy 8.3. Dynamic range within image: 50; objects may be clustered with several within a few arcseconds. 8.4. Calibration requirements: absolute 10% repeatability n/a relative n/a 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): 5 hours per field; assume 4 fields to cover all gas-rich regions 12. Total integration time for program (hr): 20 hours 13. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) The limiting factor in this experiment is the angular resolution, which pushes the limit of what ALMA can do. -------------------------------------------------- Review v2.0: Searching for proto-SSCs in the Antennae Wilson et al. Very modest proposal, would it help to include higher-J lines alongside? Would ACA help to stretch things to almost mosaic? ===================================================================================== DRSP 1.7.11 Title The CO-to-H2 conversion factor Pi N. Nakai Time 43 hrs 1. Name: The CO-to-H2 conversion factor Tatematsu, K., Nakai, N., et al. 2. One short paragraph with science goal(s) Indirect measurement of the mass of molecular gas from CO(1-0) intensity. Of prime importance for all CO observations of any galaxies. The conversion factor will be determined by using virial mass analysis appling to individual molecular clouds. How different (or common) is the factor at various enviroment with different metalicities, arms/interarms, galactic centers, et al.? 3. Number of sources 6, from early to late type galaxies 4. Coordinates: 4.1. all over the sky (probably) 4.2. Moving target: no 4.3. Time critical: no CO J=1-0 imaging: ---------------- 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.2" (5 pc at 5 Mpc) 5.2. Range of spatial scales/FOV (arcsec): three fields for each galaxies 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 6.2. Lines and Frequencies (GHz): CO 115.0 GHz (redshifted for 5 Mpc and Ho = 75) 6.3. Spectral resolution (km/s): 2 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 1000 km/s max 8. Line intensity: 8.1. Typical value (K or Jy): 5 - 10 K 8.2. Required rms per channel (K or Jy): 0.7 K 8.3. Spectral dynamic range: 10 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): 9.4 hr per a field of a galaxy 11. Total integration time for program (hr): 9.4 x 3 x 6 = 169 hours 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) Limit to only galaxies located at <5 Mpc to satisfy enough velocity resolution, spatial resolution, and sensitivity for reasonable total observing time. Will be important to observe early to extremely late type galaxies and inner to outer disks of a galaxy. So four field in each galaxy and different type of ten galaxies would be needed. ******************************************************************** Review Chris Carilli: this is duplicate of 1.7.3 could combine or assume two groups are doing competing experiments. Comment Ewine: leave both program is DRSP, since there will be several attempts to do this -------------------------------------------------- Review v2.0: The CO to H2 conversion factor Tatematsu, Nakai et al. This seems to be a crucial ALMA goal. Would it make sense to expand its scope to include all the SINGS spirals for example? What about adding in higher-J transition maps? Note the Meier and Turner DRSP proposal - would it make sense to combine these proposals into a larger program on this issue? 1) Spectral line survey in high-z molecular absorption systems 2) A deep search for new molecular absorption systems Wiklind, Combes The revision to integration times seems fine. Are there any prospects for boosting the target list further, from a southerly extension to VLA/FIRST, from ATCA deep surveys etc? Perhaps the number of candidates by the time the DRSP is implemented might be greater, and the time required will grow? This could apply to both the 3 targets destined for detailed study, and the number of flat-spectrum candidates to search for the first time? ===================================================================================== DRSP 1.8.1 Title Structure and starformation of LMC/SMC molecular clouds Pi S. Aalto Time 630 hrs 1. Name of program and authors: Structure and starformation of LMC/SMC molecular clouds Aalto, Johansson, Rubio, Tatematsu, Black, Viallefond 2. One short paragraph with science goal(s): The Magellanic Clouds provide unique possibilities to study the effects of metallicity and radiation field on the structure of the the interstellar medium (ISM). For example, there is tentative evidence that the interstellar molecular gas in the Magellanic Clouds is characterized by a higher degree of clumping than is the case in the Galaxy. This is suggested to be an effect of reduced dust abundances and, accordingly, a deeper penetration of the UV radiation into the ISM, producing strong photodissociation of the molecular species. So far, SEST has provided the highest resolution observations, 3 pc, barely enough to resolve the largest molecular clouds (MC's) in these galaxies. Thus, to establish the true structure of the molecular clouds it is fundamental to study the molecular gas in the LMC/SMC at considerably higher resolution, i.e., 0.1 pc or even less. We suggest observations of a sample of molecular clouds in the LMC and the SMC, i.e., galaxies of significantly different metallicities. Within each galaxy, regions of different radiative environments should be observed. This strategy has the prospect to separate the impact of the metallicity and the radiation field on the structure of the clouds. With a resolution of 0.2 arcseconds we reach linear scales of 0.05 pc. The Magellanic clouds provide a star formation environment which is different in many aspects from that of the Galaxy. It is likely that some of the aspects of starformation in this low metallicity environment are similar to those in the early universe. The high angular resolution provided by ALMA will allow detection of bipolar outflows from young massive stars embedded in the MCs. 3. Number of sources: 5 clouds in the LMC (2 in 30DOR and 3 in N159); 2 in the SMC. (Four clouds in the LMC and one in the SMC are associated with the formation of massive stars and two, one in each galaxy, are located in more quiscent regions) 4. Coordinates: 4.1. 30 Doradus and N159 in LMC: (RA=05h40m, DEC=-69d) N66 and SMCB1-1 in SMC: (RA=01h, DEC=-73d) Two MC in LMC one in 30DOR (intense radiation field) the other N159 in more quiescent surroundings. Similarly for the SMC, N66 (intense radiation field). SMCB1-1, cold quiescent cloud. 4.2. Moving target: no 4.3. Time critical: no 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" - 0.2" (0.2" for a few pointings) 0.2"= 0.05 pc linear 5.2. Range of spatial scales/FOV (arcsec): At 230 GHz (Band 6) the field-of-view is about 35" 5.3. Required pointing accuracy: (arcsec): <2" 6. Observational setup 6.1. Single dish total power data: beneficial Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: beneficial 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: potentially beneficial if significantly better dynamic range is available 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 6 7.2. Lines and Frequencies (GHz): 2 frequency settings (220, 230 GHz) 7.3. Spectral resolution (km/s): 0.2 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 50 km/s 8. Continuum flux density: 8.1. Typical value (Jy): 0.5 (LMC), 0.1 (SMC) (take average value of set of objects) (optional: provide range of fluxes for set of objects) 8.2. Required continuum rms (Jy or K): 0.05 Jy (LMC), 0.01 Jy (SMC) 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) 8.4. Calibration requirements: absolute 5% repeatability 5% relative ( 1-3% would be useful ) 9. Line intensity: 9.1. Typical value (K or Jy): 2-10K (LMC), 1K (SMC) for 12CO For 13CO the values are a factor of 10 lower (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): 0.5K (LMC), 0.1K (SMC) for 12CO 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 5% ) repeatability (at least 5%) relative ( 1-3% would be useful ) 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): Integration time per setting: 50 hrs survey plus 120 hrs high res mode= 170 hrs *Survey mode - 1", 0.2 km/s resolution at 230 GHz (sensitivity 0.1 K after 40 minutes): CO 2-1 fov 35": 30DOR: 2x16= 32 pointings to cover two MCs in 30 DOR times 40 minutes = 20 hrs N159: 3x16 = 48 pointings to cover three clouds = 30 hrs Double this time to cover similar regions in the SMC = 100 hrs N66: 2x16= 32 pointings to cover two MCs in N66 (HII region plus spur) SMCB1-1 = 1x 16" Survey total: 150 hrs *High res mode - 0.2", 0.1 km/s resolution 230 GHz (sensitivity 0.7 K after 20 hours): 30DOR: two pointings in one cloud: central and outskirt - 20 hours per pointing N159: two pointings in two clouds - N159W and N159S A total of 120 hours In SMC = 120 hours. N66: two pointings in two cloud: - 10 hours per pointing - SMCB1-1: two pointing - central and outskirt - 10 hours per pointing High res total: 240 hrs 12. Total integration time for program (hr): -------------------------------------------------- Review v2.0: 1.8.1 Structure and star formation of LMC/SMC molecular clouds Aalto 390 hours there seems no overlap with 1.8.4 and 1.8.5 the emphasis here is on CO, the other two deal with continuum study to separate impact of metallicity and radiation field. Number of sources is very well justified. They propose a low resolution "survey" mode and a high resolution mode. If I understand this correctly the survey mode is used to study the structure of the ISM.. which is what this proposal is about. The high resolution mode will be used to find bipolar outflows. This seems scientifically less unique . survey mode is total 150 hours 1" resolution, i.e. 0.25pc high resolution mode is 240 hours 0.2" 0.05pc Abstract says 0.1pc resolution is needed to study structure of ISM. I am not sure how hard that number is. High resolution mode could be overkill? ===================================================================================== DRSP 1.8.2 Title Evolved stars and mass loss in the Magellanic Clouds Pi S. Aalto Time 500 hrs 1. Name: Evolved stars and mass loss in the Magellanic Clouds Authors: Aalto, Lindqvist, Schöier, Olofsson, Black et al 2. Science goal: The final stages of stellar evolution are associated with considerable mass loss in the form of an intense stellar wind. This mass loss has a profound effect on the evolution of a low- and intermediate-mass the star on the asymptotic giant branch (AGB), eventually terminating its existence as a star. The circumstellar envelope (CSE) formed by the wind contains the products of internal nuclear processes, as well as chemical reactions in the photosphere and envelope itself, and hence contributes to the chemical evolution of the cosmic gas and dust. Red supergiants will have similar cirumstellar envelopes. It is important to establish an understanding of the circumstellar emission of evolved stars. The mass return of such stars, and hence their contribution to the galactic chemical evolution, is determined by the rare high mass-loss rate objects. These are highly obscured and their photospheric abundances cannot be determined using classical methods such as visual and near-IR spectroscopy. One must rely upon estimates based on circumstellar line emission. Observations of molecular line and continuum (sub)millimeter-wave emission have proven to be one of the best tools for studying the structure, kinematics, and chemistry in CSEs. Recent systematic surveys and subsequent modellings of circumstellar CO and SiO radio line emission of evolved low- to intermediate-mass stars (AGB-stars) (Schoeier & Olofsson 2001, A&A 368, 969; Olofsson et al. 2002, A&A 391, 1053; Gonzalez Delgado et al. 2003, A&A) support the idea that these winds are generally driven by radiation pressure on dust grains which condense in the cool external layers of the photosphere, and that pulsation plays an important role in the grainformation process. Similar studies in the LMC/SMC would be of great importance in order to study the impact of a lower metallicity environment on the behaviour of the mass loss process and its evolution, and the chemistry of the envelope. The importance of obtaining an iso-distance sample should be emphasized. This will allow for reliable correlations between varios stellar and circumstellar parameters to be established, critically needed to test current dynamical wind models. We propose here to observe a sample of 60 evolved stars (mainly AGB, but also some red supergiants) that differ in mass loss rate characteristics and chemistry. We suggest using stellar samples from ISO/Herschel. Line surveys: ------------- A.) A detailed CO survey of a sample of 20 stars with high mass-loss rates (10E{-5} Mo per year) at a resolution of 0.05" (0.012 pc) and a velocity resolution of 1 km/s to compare structures and expansion velocities in low metallicity environments to those of stars in our Galaxy. Such spatial resolution makes it possible to also resolve the largest CSEs. B.) Furthermore, we suggest a lower resolution survey of 40 fainter, intermediate mass-loss rate (10E{-6} Mo per year) stars at a resolution of 0.1" (0.025 pc) and 2 km/s. It might be possible to push things down even further if the resolutions are reduced to 0.2" and 2 km/s - stars with mass-loss rates around 10E{-7} Mo per year could be detected. This means that a fair fraction of the AGB mass-loss rate distribution can be covered. Continuum survey of dusty CSEs: ------------------------------- A sample of 40 stars. According to Olofsson (2002; ALMA Science Day, Munich) the expected 340 GHz brightness for a mass-loss rate of 10E{-6} Mo per year, and a distance of 50 kpc is 0.025 mJy, which is the continuum sensitivity we expect after one hour of observing time at 345 GHz. It is therefore feasible to study the dusty envelopes of high to intermediate mass loss stars in LMC/SMC. At these wavelengths the CSEs are optically thin in dust emission and complementary information on mass-loss rates can be obtained. 3. Number of sources: 20+40+40 4. Coordinates: 4.1. 60 sources in 30 Doradus and N159, LMC (RA=3D05h40m, DEC=3D-69d) 40 sources in the SMC (RA=3D01h, DEC=3D-73d) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.05" (for 20 sources); 0.1"=0.025 pc linear 0.1" (for 40 sources) 5.2. Range of spatial scales/FOV: At 345 GHz (Band 7) the field-of-view is about 18" 5.3. Required pointing accuracy: (arcsec) 6. Observational setup 6.1. Single dish total power data: no/beneficial/required Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) no? 6.2. Stand-alone ACA: no/beneficial/required no? 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no/beneficial/required no? 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no no? 7. Frequencies: 345 GHz 7.1. Receiver band: Band 7 7.2. Lines: CO 3-2 Frequency: 345 GHz 7.3. Spectral resolution (km/s): 1 km/s - 4 km/s 7.4. Spectral coverage (km/s or GHz): 50 km/s 8. Continuum flux density: 8.1. Typical value: 0.27 - 0.027 mJy 8.2. Continuum peak value: 8.3. Required continuum rms: 0.014 mJy 8.4. Dynamic range in image: 9. Line intensity: 9.1. Typical value: Stars with high mass loss: (CO 2-1: 30 K) CO 3-2: 30 K Intermediate mass loss: (CO 2-1: 3 K) CO 3-2: 3 K 9.2. Required rms per channel: 1 - 6 K 9.3. Spectral dynamic range: 9.4. Calibration requirements: as good as possible 10. Polarization: no 11. Integration time per setting: 2 - 4 hrs 12. Total integration time for program: New time estimates with 50 telescopes: High mass loss: 3 hrs of CO 3-2 high resolution (0.05" and 1 km/s) observing gives a sensitivity of 6 K which we expect would be a 5 sigma detection. Intermediate mass loss: 6 hrs of CO 3-2 low resolution (0.1" and 2 km/s) observing gives a sensitivity of 0.77 K which would be a 4 sigma detection of a star with an order of magnitude lower mass loss than IRC10216. 11. Total integration time for program: 20x3 hrs=60 hrs 40x6 hrs=240 hrs 40x5 hrs=200 hrs ---------------- 500 hrs ********************************************************** Old sensitivity calculation: 20x2 hrs=40 hrs 40x4 hrs=160 hrs 40x3 hrs=120 hrs ---------------- 320 hrs High mass loss: 2 hrs of CO 3-2 high resolution (0.05" and 1 km/s) observing gives a sensitivity of 6 K which we expect would be a 5 sigma detection. Intermediate mass loss: 4 hrs of CO 3-2 low resolution (0.1" and 2 km/s) observing gives a sensitivity of 0.77 K which would be a 4 sigma detection of a star with an order of magnitude lower mass loss than IRC10216. -------------------------------------------------- Review v2.0: 1.8.2 Evolved stars and mass loss in the magellanic clouds Aalto 500 hours this sounds like the definitive study on evolved stars and stellar mass loss in the magellanic clouds. I just wonder whether a project of this scope is appropriate for a DRSP. propose to observe 20 stars with high mass loss rate at high resolution 60 hours 40 fainter stars with intermediate mass loss rate at lower resolution 240 hours continuum observation of 40 stars 200 hrs requested time is reasonable, but scope of project may not be? MRH: I think definitive studies should be part of the DRSP - they will be attempted, and we should plan for them. ===================================================================================== DRSP 1.8.3 Title Background quasars and the chemistry of the ISM Pi Black Time 396 hrs 1. Name: Background quasars and the chemistry of the ISM in the Magellanic Clouds Authors: Black, Aalto et al 2. Science goal: More than 60 quasars are known to lie behind the Magellanic Clouds (Geha, Alcock, Allsman, et al. 2003; Dobrzycki et al. 2003). A subset of these will have flat spectra with sufficient flux at mm and submm wavelengths to permit absorption spectroscopy that will probe the molecular component of the interstellar gas in the MC. High abundances of molecules like HCO+, H_2CO, HCN, HNC have been found in the diffuse gas of the Galaxy. From HI emission/absorption measurements it is known that the diffuse ISM is colder in the Magellanic Clouds and it is expected that the diffuse gas abundances and physical conditions are different from those in our Galaxy's high metallicity environment. The fact that most of these quasars have been identified by their variability in databases from microlensing surveys is a reminder that ALMA studies of lensed quasars will be of considerable interest. The identification of background quasars via optical variability selects against highly reddened sources occulted by dense molecular gas; however, X-ray-selected AGN include some highly obscured sources Haberl et al. 2001). Quasars behind the MC also provide astrometric reference for measurements of proper motion (see prop on stars and proper motion). 3. Number of sources: 5 4. Coordinates: 4.1. LMC (RA=05h40m, DEC=-69d) SMC (RA=01h, DEC=-73d) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.1"=0.025 pc linear 5.2. Range of spatial scales/FOV: 5.3. Required pointing accuracy: (arcsec) 6. Observational setup 6.1. Single dish total power data: no Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 345 GHz 7.1. Receiver band: Bands 7 7.2. Lines: For example: 1mm and 3mm transitions of CO, 13CO, HCO+, HCN, HNC, CN, CS, C2H, C3H2 - that have been observed in Galactic absorption studies. 7.3. Spectral resolution (km/s):0.2 7.4. Spectral coverage (km/s or GHz): 20 km/s 8. Continuum flux density: 8.1. Typical value: 10 mJy 8.2. Continuum peak value: 8.3. Required continuum rms:0.1 mJy 8.4. Dynamic range in image: 9. Line intensity: 9.1. Typical value: 0-10 mJy 9.2. Required rms per channel:1-2 mJy 9.3. Spectral dynamic range: 9.4. Calibration requirements: as good as possible 10. Polarization: no 11. Integration time per setting: 3mm: 4 hrs x number of molecular species (rms 1.17 mJy) 1mm: 7 hrs x number of molecular species (rms 1.4 mJy) 9 species, two transitions, 4 QSOs = 99x4 11. Total integration time for program: 396 hrs ********************************************************** -------------------------------------------------- Review v2.0: 1.8.3 background quasars and the chemistry of the ISM in the MC Black 396 hours proposal is to do 5 sources. Potentially very interesting, but.. I would start with just one. ===================================================================================== DRSP 1.8.4 Title Low Frequency Continuum Survey of Free-Free Emission in the LMC Pi J. Turner Time 2400 hrs 1. Low Frequency Continuum Survey of Free-Free Emission in the LMC J. Turner et al. 2. The goal is to measure and locate free-free emission from HII regions in star-forming regions of the Large Magellanic Cloud. The images will reveal at high spatial resolution the youngest massive star-forming regions that are optically obscured, and will be able to map regions containing the ionization equivalent of 1 O9 star. These observations will allow an important extension of our current knowledge of Galactic star formation to these nearby HII regions in a low metallicity setting. They include the giant HII region 30 Doradus. The submillimeter fluxes will be measured at 3 and 1mm, spectral regions which are relatively free of synchrotron and dust confusion, at resolutions comparable to the sizes of the HII regions themselves. These images will have the capability of imaging structure within HII complexes the size of Orion and of identifying compact HII regions by their size. 3. Number of sources: 2 4. Coordinates: 4.1 6 fields in LMC 5:23, -69 4.2 Moving target: no 4.3 Time critical: no 5. Spatial scales: 5.1 Angular resolution: 0.08" = .02 pc 5.2 Range of spatial scales/FOV: 3'x3' fields to cover 50 pc regions: require 144 point mosaics for each, using OTF if efficient for these fields. Each field - 2250x2250 beams one additional 12' square field at 30 Doradus 6. Observational setup 6.1. Single dish total power data: no(?) Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 6. Frequencies: 6.1 Receiver band: Bands 3 and 6 6.2 Continuum 6.3 Spectral resolution N/A 6.4 Spectral coverage N/A 7. Continuum flux density 7.1 Typical value mJy/beam 7.2 Continuum peak value: 2800 mJy/beam (10^4K point source) 7.3 Required continuum rms: ~0.05 mJy/beam to detect significant (>6 sigma) structure around an O9 star in an HII region the size of Orion 7.4 Dynamic range in image: 50000:1 (worst case; unlikely to be an HII region with tau >>1 at 3mm! -- more likely 1000:1) 8. Line Intensity N/A 9. Polarization N/A 10. Integration time per setting: 4 minutes at 1mm, 1 minute at 3mm per setting, 144 settings (3'x3' mosaics) in each of 5 locations, plus 2300 settings (12'x12') around 30 Dor field Total integration time, without calibration, ~60 + 191 hours or ~10 days. (N.B. This is dominated by the 30 Doradus field) -------------------------------------------------- Review v2.0: 1.8.4 Low frequency continuum survey of free-free emission in LMC Turner 250 hours Again I don't quite see why all of this needs to be done as part of the DRSP. Why not start with one location and a 3'x3' mosaic, or only do 30 Dor MRH: The DRSP should reflect what will be attempted in the first 3 years of ALMA, not necessarily the first programs to be run (in which case starting with one target would be prudent). ===================================================================================== DRSP 1.8.5 Title Gas and Dust in 30 Doradus Pi J. Turner Time 80 hrs 1.8.5. Gas and Dust in 30 Doradus J. Turner 2. 30 Doradus is the most luminous nebula in the Large Magellanic Clouds and comparable to the most luminous HII regions in the Milky Way (NGC 3603, Carina). The star cluster within 30 Doradus is a "populous" cluster, or small super star cluster, which may be similar to a small globular cluster in nature. There are younger, embedded surrounding this luminous region, which may have been triggered by 30 Doradus. There are 60 or 70 O3 and O4 stars exciting 30 Dor, which is 200 pc in diameter. Large luminous regions such as 30 Dor are rare. 30 Doradus is only 50 kpc away, and the continuum sensitivity of ALMA allows us to map its free-free emission, dust continuum, and CO line emission at high resolution and sensitivity. We propose to map the nebula in the CO lines and continuum in Bands 3, 6, and 7 to trace the ionized gas, molecular gas, and dust within the core of 30 Doradus. We will be able to map down to EM~10^6, similar to Orion, to gas column densities of roughly a few x 10^20 (caveats below) and to clump masses of about 40 Msun in dust emission. Three bands are needed to separate free-free and dust continuum contributions. The primary driver for the time request is the continuum. There is abundant HI line emission in the 30 Dor region, but the dominant large molecular streamer is located a degree or so to the south, and extends over 3 degrees in length. This proposal will map small knots of emission associated with or directly affected by the 30 Doradus nebula. CO knots have been detected at lower resolution. 3. Number of sources: 1 4. Coordinates: 4. 1 field, 20'x20' in size, in LMC 5:39, -69 4.2 Moving target: no 4.3 Time critical: no 5. Spatial scales: 5.1 Angular resolution: 1" 5.2 Range of spatial scales/FOV: 20'x20' field: OTF 5.3 Single dish: yes 5.4 ACA: yes 5.5 Subarrays: no 6. Frequencies: 6.1 Receiver band: Bands 3, 6, 7 6.2 Continuum 8 GHz 6.3 Spectral resolution 3 km/s 6.4 Spectral coverage 300 km/s (LMC is not a big galaxy) 7. Continuum flux density 7.1 Typical value: 0. to 2 mJy/beam 7.2 Continuum peak value: 50 mJy/beam 7.3 Required continuum rms: 0.12, 0.42, 0.44 mJy/beam for Bands 3,6,7 (0.01K) 7.4 Dynamic range in image: 1000:1 8. Line Intensity 8.1. Typical value (K or Jy): 0.1-1 K 8.2. Required rms per channel (K or Jy): 0.2 (345 GHz)-1 (115)K (see note above) 8.3. Spectral dynamic range: 25 9. Polarization N/A 10. Integration time per observing mode/receiver setting (hr): (2700 seconds/15' square OTF map) x 11 maps = 8 hrs Band 3 (5400 seconds/15' square OTF map) x 16 maps = 24 hrs Band 6 (5400 seconds/15' square OTF map) x 32 maps = 48 hrs Band 7 11. Total integration time for program: 80 hours 12. Comments on observing strategy These will be OTF maps, 15' x 15' to cover the 200 pc diameter core of 30 Doradus. I assumed a scan rate of 30"/second for the OTF map, so each row takes 30 seconds. To get the amount of time per map, I took a sampling rate (row spacing) of 10" for Band 3, and 5" for Bands 6 and 7 for simplicity. These could be tweaked, but they sample over the Nyquist rate, which is probably desirable. The ultimate goal is to achieve about 0.01K in each band in continuum. Resolution is 1" = 0.24 pc. Line resolution 3 km/s. Matched beam observations required, 1" beams. Zero spacing desirable to allow spatial smoothing for sensitivity to lower level emission. Sensitivities. 3mm 8 hours gives about 11 maps, x 1.6 seconds/sample/map = 17 seconds per sample. This gives continuum sensitivities of .13 mJy and .012 K. Good enough to see a 320 Msun clump in dust emission (the mass is gas mass) at 3mm, and free-free emission from EM ~ 10^6 cm-6 pc at 5 sigma (Orionish). Line: 1.02 K times 3 km/s =3 K km/s, which would be N_H2 = 6 x 10^20 for a Galactic conversion factor, although the LMC is underluminous, at least in CO(1-0). Compact HII knots easily detectable. 870um: 48 hrs gives 32 OTF maps, at 0.375 sec/sample/map = 12 seconds/sample. Continuum sensitivities are 0.436mJy, .0044K. Can see compact HII regions here but not Orions. Can detect a clump of 40 Msun in dust emission at 4 sigma, scaling from observed Orion clumps, which corresponds to a gas density of about 10^5 in a 0.24 pc (1") diameter region. Line sensitivity of .22K x 3km/s would be .7 K km/s, or 1.4 x 10^20 for a Galactic conversion factor and CO(3-2)/CO(1-0) ~1. However, J=2-1 lines are often brighter than 1-0 in LMC. Could compensate to some degree for high Xco. 1.3mm: In between the two above, use this to separate gas and dust. Extremely optically thick HII regions can still be rising into the millimeter. **************************************************************** Review Chris Wilson: program looks O.K. but did not check integration times -------------------------------------------------- Review v2.0: 1.8.5 Gas and dust in 30 Doradus Turner 80 hours this looks very ok to me. There is overlap with 1.8.4, but there proposed sensitivity is much better. Those proposals could easily be combined. ===================================================================================== DRSP 1.8.6 Title Mass loss and outflow velocities in Magellanic Cloud AGB stars Pi M. Groenewegen Time 50 hrs 1. Name of program and authors: Mass loss and outflow velocities in Magellanic Cloud AGB stars Martin Groenewegen 2. Science goal: Stars with masses below about 8 solar masses shed almost their entire atmosphere at the end of their life during the Asymptotic Giant Branch phase. During this phase of strong mass loss (up to 10(-4) solar masses/year) a circumstellar envelope (CSE) is maintained containing both dust and molecules. The dust radiates mainly in the infrared, up to the sub-mm. Modelling the Spectral Energy Distribution of an AGB star, and its broad-band dust features in the Near- and Mid-IR range provides information about the DUST-mass loss rate and the composition of the dust. However, one of the input parameters in such modelling is the expansion velocity of the wind. The molecular content of the CSE is traced through its most abundant molecule besides H2, namely CO. Heterodyne observations of CO do not only provide information on the GAS-mass loss rate from the peak intensity (assuming a CO/H2 ratio), but additionally the outflow velocity, and the systemic velocity, useful for kinematic studies. Combining IR/sub-mm with heterodyne observations are necessary to obtain the best constrained values on the outflow velocity, TOTAL mass loss and dust-to-gas ratio of AGB stars. Combining data from the Galaxy, LMC and SMC allows one to study the effect of metallicity on AGB mass loss and outflow velocity. Both are theoretically predicted to be smaller at lower metallicity, and the latter is partially confirmed by observations of H20 masers in LMC sources which indicate a 20% smaller outflow velocity (e.g. van Loon et al. 2001, A&A 368, 950). The proposed observations would allow to study a statistically significant sample of both O- and C-stars in both SMC and LMC. Observations of the type discussed above are standard for our galaxy, with maybe 300 AGB stars being detected in CO at mm wavelengths. Regarding the Magellanic Clouds, continuum Near-, Mid- and Far-IR fluxes will be and have been obtained with ISO, SPITZER, and HERSCHEL, and a few 100 AGB stars with mass loss are known in the Clouds. Now, for the first time with ALMA, heterodyne observations of CO lines of AGB stars in the Magellanic Clouds are within reach. (Note that OH and SiO maser detections exist of very few AGB stars and supergiants in the Clouds, but these data are not easily related to the mass loss [OH], or come from a region where the outflow is still being accelerated [SiO]. In addition, many AGB stars, especially at low-Z, are carbon-rich and hence do not show OH or SiO maser lines !). Expected main-beam temperatures have been calculated using a model for the well studied Galactic carbon star CW Leo (Groenewegen et al., 1998, A&A 338, 491), and putting it at 50 kpc. The predicted temperatures in the CO(1-0), (2-1), (3-2), (6-5) line, in a beam of 1.0*(230 GHz/ freq) arcsec are 0.25, 0.47, 0.49, 0.49 K, respectively. In one hour of integration with a velocity resolution of 0.4 km/s, the rms temperatures are, respectively, 0.05, 0.05. 0.08, 0.34 K, according to the ALMA sensitivity tool. This indicates that the CO(2-1) line is the most sensitive one, in accordance with experience for Galactic sources, and is therefore the line selected for the observations. The beam-size is estimated from the CO photodissociation radius in a source like CW Leo, when located at 50 kpc. The high velocity resolution is preferred for 2 reasons. First, one may realistically expect some sources to have expansion velocities of only a few km/s due to the effect of the lower metallicity in the Clouds. Second, the proposed observations do not try to resolve the CO shell; in fact the beam size is tailored to the CO photodissociation radius. However, it might be possible in the brightest sources to get a hint for possible asymmetries in the CSE by looking for deviations from the expected standard parabolic profile. This has been done for IRC 10 216 (Groenewegen & Ludwig, 1998, A&A 339, 489) but requires high velocity resolution. When such deviations would be detected one might then try to resolve these CSEs. 3. Number of sources Based on previous work using IRAS and ISO, about 50 AGB stars in LMC and SMC have the required high luminosities and mass loss rates (i.e. typically 10(-6) msol/yr and larger) to be detectable in 1h of integration in the CO(2-1) line. 4. Coordinates: 4.1. RA and DEC: LMC (5h40 -69d) and SMC (1h -73d) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 1 - 1.5 arcsec 5.2. Range of spatial scales/FOV: 1 to 20 arcsec 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 6 6.2. Lines and Frequencies 12CO(2-1) at 230 GHz 6.3. Spectral Resolution (km/s): 0.4 km/s 6.4. Bandwidth or spectral coverage: 100 km/s 7. Continuum flux density: 7.1. Typical value: N.A. 7.2. Continuum peak value: N.A. 7.3. Required continuum rms: N.A. 7.4. Dynamic range in image: N.A. 8. Line intensity: 8.1. Typical value: 0.5 K 8.2. Required rms per channel: 0.05 K 8.3. Spectral dynamic range: >5 9. Polarization: no 10. Integration time per setting: 1h per star 11. Total integration time for program: 50 hours ************************************************************ Review by Fredrik Schoeier and reply by Martin Groenewegen 1) There appears to be a significant overlap with project 1.8.2 (Aalto et al.). The Aalto et al. project has the same basic scientific motivation but will also aim at obtaining a slightly larger sample of stars with a much larger spread in mass-loss rates. The importance of studying AGB stars in the Magellanic Clouds is of course to see the how the mass loss depends on metallicity but also that you will get rid of any systematic effects introduced in the analysis, through the distance estimates, and possibly get more reliable correlations of wind-properties with, e.g., stellar parameters such as luminosity. This, is were the Aalto et al. proposal is more ambitious. There is indeed some overlap with project 1.8.2. I will briefly discuss the overlap and differences. Proposal 1.8.2 covers both continuum and line observations. The current DRSP does not consider continuum observations as they are only feasible for very few objects, in fact much fewer than suggested by Aalto et al. (see ``Will the LSA detect continuum or line emission from AGB stars in the LMC ?'', Groenewegen M.A.T., in: ``Science with large millimetre arrays'', Dec. 1995, Garching, Ed. P. Shaver, Springer Verlag, p. 164). The quoted continuum sensitivity in DRSP 1.8.2 of 0.025 mJy in 1 hour at 345 GHz is ONE-sigma only. Therefore objects need to be significantly brighter than this to have their photometry reliably determined in a reasonable time. In my opinion this implies much fewer than 40 potential targets. The proposals overlap in the line observations. Aalto et al. mention 20 objects at high mass-loss rates and 40 at mass-loss rates down to 10(-6) msol/yr. The current proposal mentions 50 stars (at implied mass loss rates of 10(-6) and higher). 2) The reviewer agrees with the predicted line intensities. In the proposal text it is not mentioned that the lines are typically 20-40 km/s broad for these high mass-loss-rate objects. Why is a resolution of 0.1 km/s requested? 1-2 km/s is enough to get a very good handle on also the line profile (This is also the resolution requested by Aalto et al.). 3) It should also be pointed out that the sources will generally not be resolved (however the Aalto et al. project will use 0.05 arcsec resolution for some 20 sources with high mass loss rates) and no spatial information of the emission obtained. That said, ALMA is still the best suited telescope for a project like this given the fact that the compact emission is just too diluted in small single-dish telescopes like, eg., APEX. Points 2 and 3 will be addressed together. One difference between Aalto et al. and the current proposal is the required velocity resolution. The former requires 1 km/s, while I preferred 0.1 km/s. Aalto et al also suggest to work at even lower resolution to push the detection of stars at even slightly lower mass-loss rates. One has to be careful on this issue however. The theory of dust-driven winds predicts that at lower metallicity the terminal velocity should be lower, which is confirmed by observations of H2O maser emission (e.g. van Loon et al. 2001, A&A 368, 950) indicating an about 20% smaller expansion velocity in LMC sources, suggesting even lower velocities in SMC sources. In a Galactic sample of 300 carbon stars [with mass loss rates above 10(-6)] the outflow velocities range from 7 to 40 km/s with a mean of 18.7 km/s (Groenewegen et al. 2002, A&A 390, 511). Therefore one has to consider velocities in the range 4 to 30 km/s and means of 10-15 km/s in SMC and LMC. I believe it is safer to go for a high velocity resolution (of 0.4 km/s or better, AND IN THE DRSP I NOW REQUIRE 0.4 km/s INSTEAD OF 0.1 km.s) and have sufficient redundancy from the beginning, and then bin in velocity a posteriori if required, than to go for a resolution of 1 km/s which we already know will not be sufficient to get an accurate determination of the velocity in some sources. The high velocity resolution is preferred for another reason, which was in my mind when I wrote the DRSP, but which I have now made explicit. The proposed observations do not try to resolve the CO shell; in fact the beam size is tailored to the CO photodissociation radius. However, it might be possible in the brightest sources to get a hint for possible asymmetries in the CSE by looking for deviations from the expected standard parabolic profile. This has been done for IRC 10 216 (Groenewegen & Ludwig, 1998, A&A 339, 489) but requires high velocity resolution. When such deviations would be detected one might then try to resolve these CSEs. A final difference between the two DRSP is the fact that 1.8.2 plans to observe the CO(3-2) line, while I propose CO(2-1). As already mentioned in the DRSP, it is expected that the CO(2-1) line will provide the higher S/N. -------------------------------------------------- Review v2.0: 1.8.6 mass loss and outflow velocities in MC AGB stars Groenewegen 50 hours there is significant overlap in science with 1.8.2, and the proposal is followed by an extensive discussion of the pro's and con's of the two proposals. At this time of night.. it seems to me that Groenewegen is right. MRH: Some level of overlap is probably realistic. ===================================================================================== DRSP 1.9.1 Title GRB environment Pi Time 300 hrs 11. Name of program and authors: GRB environment 2. One short paragraph with science goal(s): Gamma ray bursts are thought to originate with the explosion of massive stars in regions of prodigious star forming activity at moderate to large distances. This program seeks to survey the regions of a number of gamma ray burst sources to characterize the infrared emission associated with their hosts. The resulting catalog will help to assess whether the paradigm for GRBs is valid. 3. Number of sources: 300 GRB positions 4. Coordinates: 4.1. Rough RA and DEC All sky. 4.2. Moving target: yes/no (e.g. comet, planet, ...) no 4.3. Time critical: yes/no (e.g. SN, GRB, ...) no, the survey is post GRB 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) single field 5.3. Single dish total power data: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 7 and 9 6.2. Lines and Frequencies (GHz): 280 GHz, 345 GHz 650 GHz 6.3. Spectral resolution (km/s): continuum 6.4. Bandwidth or spectral coverage (km/s or GHz): 8 GHz 7. Continuum flux density: 7.1. Typical value (Jy): .05 7.2. Required continuum rms (Jy or K): .03 mJy (1.1 mm); .25 mJy (.45 mm) 7.3. Dynamic range within image: >5 8. Line intensity: 8.1. Typical value (K or Jy): 8.2. Required rms per channel (K or Jy): 8.3. Spectral dynamic range: 9. Polarization: no (optional) 9.1. Required Stokes 9.2. Total polarized flux density (Jy) 9.3. Required polarization rms and/or dynamic range 9.4. Polarization fidelity 10. Integration time for each observing mode/receiver setting (hr): 20 mins 11. Total integration time for program (hr): 300 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) ************************************************************************ Review Chris Carilli: OK ===================================================================================== DRSP 1.9.2 Title ToO Observing of GRB Afterglows Pi S. Van Dyk Time 30 hrs 1. Name: ToO Observing of GRB Afterglows -- Schuyler Van Dyk, Kurt Weiler et al. 2. One short paragraph with science goal(s) Gamma ray bursts (GRBs) are among the most energetic events in the Universe. Their origins are still unknown. The radio emission from GRB afterglows will provide insight into the physical processes associated with the burst and its immediate circumburst environment. If some (long-duration) GRBs are actually associated with hypernovae (extremely energetic supernovae), then we expect that their properties may be similar to those of the most luminous radio supernovae (RSN); this was particularly true for the nearby SN 1998bw/GRB 980425 and the more distant SN 2003dh/GRB 030329. As such, the justification for detecting and monitoring GRBs early in their radio evolution, particularly in the mm and submm, follow similar lines to that for studying RSNe. The rapid rise to maximum in the ALMA bands will provide valuable information on both the emission and absorption processes for GRBs, which further provides vital insight into the nature of the objects giving rise to the burst. Analogs of SN 1998bw can be detected and followed out to 100's of Mpc. 3. Number of sources The SWIFT mission (launch in December 2003) will greatly increase the discovery rate. Based on current GRB detections, we guess roughly 20 to 100 per semester. 4. Coordinates: 4.1. All over the sky. 4.2. Moving target: no 4.3. Time critical: very 5. Spatial scales: 5.1. Angular resolution (arcsec): any ALMA resolution 5.2. Range of spatial scales/FOV (arcsec): point sources 5.3. Single dish total power data: no 5.4. ACA: no 5.5. Subarrays: could do 6. Frequencies: 6.1. Receiver band: 3, 6, 7, optionally 9 6.2. Lines and Frequencies (GHz): --- continuum 6.3. Spectral resolution (km/s): --- N/A 6.4. Bandwidth or spectral coverage (km/s or GHz): --- 8 GHz 7. Continuum flux density: 7.1. Typical value (Jy): 0.001-0.1 (detection, based on current RSN detections) 7.2. Required continuum rms (Jy or K): 0.00006 (.06 mJy) 7.3. Dynamic range within image: >4 8. Line intensity: 8.1. Typical value (K or Jy): N/A 8.2. Required rms per channel (K or Jy): N/A 8.3. Spectral dynamic range: N/A 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): typically 1/60 hr for Band 3 3/60 hr for Band 6 10/60 hr for Band 6 0.5 hr for Band 9 11. Total integration time for program (hr): 0.5-1 hr for null detection. If there should be a strong detection, requested monitoring program will last for 3-4 days, totaling 10 hours. Estimated ToO time every semester: on average, 10-30 hours for afterglow searches. 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): This is a target of opportunity proposal. The ToO window is very small for GRBs; to date, only SN 2003dh/GRB 030329 has been studied with any regularity in the mm. Detection of these extremely energetic objects is critical. This project is very similar to the RSN ToO program, and will require dynamic scheduling and notification and input from the observing team. ********************************************************************** Review Chris Carilli: Sensitivies look OK. For purposes of DRSP they should be more explicit on the reaction times -- how quickly do we need to get on source to make this interesting? Reply Turner: We dont' know what GRBs are, but assuming they are supernovae, Kurt Weiler's models show that they peak 8-12 hrs after the SN. So the answer is, observations need to be scheduled ASAP after the SN, within 2-3 hours ideally, or even faster. Obviously this will not always work since SN are caught at different stages of evolution, but if you wait 12 hours you will probably never see anything in the submm. At this point so little is known about progenitors of either SN or GRBs that the interruption is well justified. ===================================================================================== DRSP 2.1.1 Title Small scale structure of molecular clouds Pi J. Pety Time 225 hrs 1. Name of program and authors Name: Small scale structure of molecular clouds Authors: J. Pety and E. Falgarone 2. One short paragraph with science goal(s) Characterize the threshold of the self-similar hierarchy of non star forming molecular clouds. This hierarchy is a (multi)fractal structure, resulting of the interplay of gravity and turbulence. Its threshold is determined by the dissipative processes of the turbulent cascade (shocks, coherent vortices, see Pety & Falgarone 2000 AA 356 279). Molecular viscosity sets this threshold at about 10 AU (0.1" at 100pc) in molecular clouds. The formation and structuration of dense cores is linked to dissipation processes of the turbulent and magnetic energy of the molecular clouds. Studying the small-scale structure of molecular clouds in the environment of a non-star forming dense core (in line, continuum) will thus shed light on the underlying dissipation processes. A mosaic of 13 fields obtained with the PdBI in 12CO(1-0) uncovers a set of elongated and straight structures in a high latitude cloud. Some are unresolved in their transverse direction (resolution 500 AU) calling for higher resolution. Other extend further than the field of the mosaic (2' by 1'), calling for large spatial coverage. Several steps are required in the observational strategy, given the fractal distribution of these structures. 3. Number of sources 1 field of 4'x4' at 1.0" resolution 1 field of 2'x2' at 0.3" resolution 4. Coordinates: 4.1. Rough RA and DEC 1 source in Chamaeleon (RA=12:15, DEC=-82, 1950) 4.2. Moving target: no 4.3. Time critical: no 4.4. Scheduling constraints: Avoid windy periods to ensure high precision mosaicing. 5. Spatial scales: 5.1. Angular resolution (arcsec): 1", then 0.3" 5.2. Range of spatial scales/FOV (arcsec): We propose to make Nyquist sampled mosaics following an hexagonal compact pattern. This implies: 240 (59-fields mosaic at 1.0" resolution) 400 (13-fields mosaic at 0.3" resolution) In view of the total number of fields, such a program could benefit from the On-The-Fly interferometric mode that IRAM will try to prototype for ALMA in the coming three years, but this observing mode is not optional for this project. 5.3. Required pointing accuracy: (arcsec) 0.6" rms to ensure high precission mosaicing. 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: * On-The-Fly is required by the field of view. * The narrow zero-power linewidth (6 km/s) makes frequency switch suitable to this project, which will improve single dish signal-to-noise ratio by sqrt(2). 6.2. Stand-alone ACA: Required 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: This question is difficult to answer. We do not know of any public studies that shows that cross-correlation between ACA and ALMA would be beneficial. Several points need to be clarified: 1) Does the collecting surface of ACA is enough to ensure alone (i.e. without a correction for the integrating time) good sensitivity at spatial frequencies around 7m relatively to the sensitivity at frequencies measured by ALMA alone? 2) Cross correlating 2 different interferometers implies a multiplication of the respective primary beams in the measurement equation: Does this implies in practice a limitation of the field of view of the small antennas to the field of view of the large antennas? 6.4. Subarrays of 12m baseline-ALMA antennas: No 7. Frequencies: 7.1. Receiver band: Band 3 7.2. Lines and Frequencies (GHz): 12CO(1-0) at 115 GHz 13CO(1-0) at 110 GHz 7.3. Spectral resolution (km/s): 0.1 km/s at 1.0" resolution 0.3 km/s at 0.3" resolution 7.4. Bandwidth or spectral coverage (km/s or GHz): 2 to 6 km/s for the line 8. Continuum flux density: 8.1. Typical value (Jy): 55 microJy at 1.0" resolutions 8.2. Required continuum rms (Jy or K): 8.2 microJy or 0.7 mK at 1.0" resolution 2.6 microJy or 2.6 mK at 0.3" resolution 8.3. Dynamic range within image: Unknown 8.4. Calibration requirements: Absolute: n/a Repeatability: n/a Relative: 10% 9. Line intensity: 9.1. Typical value (K or Jy): 5K for 12CO(1-0) 2K for 13CO(1-0) 9.2. Required rms per channel (K or Jy): 0.35K at 115 GHz and 1.0" resolution 0.70K at 115 GHz and 0.3" resolution 9.3. Spectral dynamic range: 10 9.4. Calibration requirements: Absolute: n/a Repeatability: n/a Relative: 10% 10. Polarization: No 11. Integration time for each observing mode/receiver setting (hr): 70h for the 4'x4' mosaic at 1.0" resolution 155h for the 2'x2' mosaic at 0.3" resolution 12. Total integration time for program (hr): 225h 13. Comments on observing strategy: This program would probably be submitted 2 times to the proposal committee over the 2 year span of the design reference mission. The idea is to survey a large enough area at 1" resolution and then to zoom on a particularly interesting region to obtain a factor 3 order--of--magnitude increase in resolution over the molecular structures observed by the current generation of mm interferometers. The possibility to have 0.3" structure is the most highly prospective assumption here. This is however the goal of this project to find the threshold of the self-similar hierarchy in molecular clouds. The typical line intensity values come from Plateau de Bure observation of Polaris. We expect that beam dilution will make up for the loss of sensitivity to extended regions when the resolution increase. The large range of spatial scales sampled at the three resolution will enable the meaningful computation of statistical measures like structrure functions to improve the comparison with Magneto-Hydro-Dynamics simulations, which have made huge progresses in the past decade. -------------------------------------------------- Review v2.0: init_1 = 2.1.1 Name: Small scale structure of molecular clouds Authors: J. Pety and E. Falgarone This program will really drive the mosaicing capabilities of ALMA to their limits in terms of pointing and calibration. ACA is essential, but I share the authors view that the 7m x 12m correlations are probably not necessary. The gain in sensitivity is not essential here and the calibration complexity makes me shudder. The authors say that they plan to first get the 1" data and then zoom in on interesting regions at 0.3". Doesn't this introduce a bias that this study should try to avoid? In other words, should one try to get the entire region at both resolution? ===================================================================================== DRSP 2.1.2 Title Kinetics, density and temperature profile in pre-stellar cores Pi A. Bacmann Time 125 hrs Name: Kinetics, density and temperature profile in pre-stellar cores A. Bacmann, A. Dutrey, ... 2. Science goal: to map the inner part (inner ~ 15", not resolved by single dish telescopes) of pre-stellar cores. This program samples both isolated star formation (taurus) and clustered star formation (rho oph). The density profile will be derived from the continuum observations. For the temperature profile, various CO isotopes can be used to probe different optical depths within the core. Other possible strategy: with H2CO observations (but high energy transitions not excited in 10 K objects, line often self-absorbed - maybe better for high-mass star forming regions). Need to have a strong line because of high expected molecular depletion in the centre. The inner core dynamics will be investigated using the 372.4 GHz transition of H2D+. H2D+ is abundant in pre-stellar objects, and is one of the few species not affected by depletion at the high densities and low temperatures characterising the inner parts of pre-stellar cores. This ion makes it possible to map the velocity field (and possible infall / rotation motions) in the cores. Additionally, the abundance of H2D+ is of chemical interest in deuteration processes. 3. Number of sources: 10 sources in ophiucus, 10 in taurus, + 5 other cores scattered in RA, DEC for CO/Band 6 10 sources total for H2D+/Band 7 4. Coordinates 4.1. RA & DEC Taurus: RA=04 DEC=+25 Oph: RA=16:30 DEC=-24 4.2. moving target: no 4.3. Time critical: no 5. Spatial scales 5.1 angular resolution: 1" 5.2 FOV: ~ 20" x 20" (small mosaic) for CO; single field in H2D+ at center 5.3 total power: yes 5.4 ACA: yes 5.5 subarrays: no 6. Frequencies 6.1 Frequency band: Band 6 Band 7 6.2 Line and Frequencies (GHz) 12CO(2-1) 230.5 GHz, H2D+ 1-0 372.4 GHz 13CO(2-1) 220.4 GHz, C18O(2-1) 219.6 GHz (strong, thermalised transitions, optically thick) 6.3 Spectral resolution: 0.1 km/s 6.4 Bandwidth/Spectral coverage: 30 km/s 7. Continuum flux density 7.1 Typical value (Jy) 0.05 Jy 7.2 Required rms 0.005 Jy 7.3 Dynamic range within image 8. Line intensity 8.1 typical value: 3 K in C18O(2-1), 5 K in 13CO(2-1), 0.1-1 K in H2D+ 8.2 required rms per channel: 0.3 K (10 sigma) for CO; 0.05 K for H2D+ 8.3 spectral dynamic range: 20 for H2D+ 9. polarisation: no 10. integration time per setting CO: 7 minutes per field, mosaic 3x3, ie ~ 1h per source (center field in C18O and 13CO, outer fields in 12CO and 13CO) H2D+: 10 hr per source 11. total integration time for program: 25 hr: CO Band 6 100 hr: H2D+ Band 7 Notes: H2D+ 372.4 GHz falls just outside the official frequency range of Band 7, but may be obtained with reduced sensitivity. Current integration times are for 370 GHz. Extension of Band 7 to 372 GHz is part of a change request. ************************************************************************* Review John Richer: See program 2.1.1. Comment Ewine: H2D+ has been added -------------------------------------------------- Review v2.0: init_2 = 2.1.2 Name: Kinetics, density and temperature profile in pre-stellar cores A. Bacmann, A. Dutrey, ... Program remains unchanged w.r.t. DRSP 1.1. THe H2D+ observations are the most informative, and take up most time of this project. The observational setup for the CO (+isotopes) and/or H2CO part could use some more details on how exactly the temperature information will be extracted independent of chemistry. ===================================================================================== DRSP 2.1.3 Title Kinetic Temperature Structure in Protostars and YSOs Pi J. Mangum Time 15 hrs 1. Name: Kinetic Temperature Structure in Protostars and YSOs Authors: J. Mangum, A. Wootten 2. Science goal: Measure molecular spectral line emission from the H2CO molecule from a representative sample of protostars and YSOs. Measurements of the following transitions will provide accurate kinetic temperatures for sources with Tk < 75 K: -- 3(03)-2(02) at 218.2 GHz -- 3(22)-2(21) at 218.5 GHz -- 5(05)-4(04) at 362.7 GHz -- 5(24)-4(23) at 363.9 GHz The program is based on Mangum & Wootten (1993), which described the kinetic temperature probing properties of the H2CO molecule. This technique has remained relatively untapped due to the lack of sensitive instrumentation which can provide the spatial resolution required to map the kinetic temperature structure in the youngest star formation regions. 3. Number of sources: 30 4. Coordinates: 4.1. 10 sources in Oph (RA=16:30, DEC=-24) 10 sources in Perseus (RA=03, DEC=+30) 10 sources distributed over sky (RA=any, DEC=any visible) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.5" 5.2. Range of spatial scales/FOV: 30" 5.3. Single dish: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 6, Band 7 6.2. Line: H2CO 3(03)-2(02), 3(22)-2(21), 5(05)-4(04), 5(24)-4(23) Frequency: 218.2 GHz, 218.5 GHz, 362.7 GHz, 363.9 GHz 6.3. Spectral resolution (km/s): 0.05 km/s 6.4. Spectral coverage (km/s or GHz): 20 km/s 7. Continuum flux density: 7.1. Typical value: O.3 Jy 7.2. Continuum peak value: 0.3 Jy 7.3. Required continuum rms: 0.0002 K 7.4. Dynamic range in image: 20 8. Line intensity: 8.1. Typical value: 0.03 Jy 8.2. Required rms per channel: 0.5 K 8.3. Spectral dynamic range: 20 9. Polarization: no 10. Integration time per setting: 30 x 0.5 hrs 11. Total integration time for program: 15 hr ************************************************************************** Review John Richer: see 2.1.1. -------------------------------------------------- Review v2.0: init_3 = 2.1.3 Name: Kinetic Temperature Structure in Protostars and YSOs Authors: J. Mangum, A. Wootten Unchanged w.r.t. DRSP 1.1. If sensitivity is an issue 7m x 12m correlations may be useful. ===================================================================================== DRSP 2.1.4 Title Density and temperature profile in high-mass cores Pi A. Bacmann Time 155 hrs Name: Density and temperature profile in high-mass cores ================================================== A. Bacmann, A. Dutrey, ... 2. Science goal: to map the high mass cores at distances between 1 and 10 kpc in order to derive density and temperature profiles. The aim is to reach similar/better linear resolution for sources at 1-5 kpc as those obtained by present day single dish telescopes. Density profiles will be derived from continuum observations. A combination of transitions of formaldehyde (H2CO) will be used to derive temperature profiles, following Magum & Wootten (1993). The transitions can be observed in a single receiver setting. 3. Number of sources: 10 Galactic sources in various high-mass star forming clouds. Distances 1 - 10 kpc 4. Coordinates 4.1. RA & DEC M17: RA 18 DEC -16 Cygnus: RA 20 DEC +30 Sagittarius: RA 18 DEC -25 Monoceros: RA 07 DEC -06 NGC2264: RA 06:30 DEC +10 + others 4.2. moving target: no 4.3. Time critical: no 5. Spatial scales 5.1 angular resolution: 0.5" 5.2 FOV: ~ 100" x 100" (5x5 mosaic) for 1-5 kpc sources, small mosaic (3x3) for 10 kpc sources. 5.3 total power: yes 5.4 ACA: yes 5.5 subarrays: no 6. Frequencies 6.1 Frequency band: 7 6.2 Line and Frequencies (GHz): H2CO(505-404):362.7 GHz H2CO(524-423):363.9 GHz H2CO(542-441):364.1 GHz H2CO(533-432), H2CO(532-431):364.3 GHz H2CO(523-422): 365.4 GHz 6.3 Spectral resolution: 0.5 - 1 km/s 6.4 Bandwidth/Spectral coverage: 50-100 km/s 7. Continuum flux density 7.1 Typical value (Jy) 0.2 Jy 7.2 Required rms 0.02 Jy 7.3 Dynamic range within image 8. Line intensity 8.1 typical value: 1 K in H2CO(5-4) 8.2 required rms per channel: 0.1 K 8.3 spectral dynamic range 9. polarisation: no 10. integration time per setting 1.5 hours per field in 5x5 mosaics, ie 37.5 h/source 1 hour per field in 3x3 field, ie 9h/source 11. total integration time for program: 5 sources with 5x5 mosaics, 110 h 5 sources with 3x3 mosaics, 45 h ************************************************************************ Review John Richer: see program 2.1.1. -------------------------------------------------- Review v2.0: init_4 = 2.1.4 Name: Density and temperature profile in high-mass cores ================================================== A. Bacmann, A. Dutrey, ... Unchanged w.r.t. DRSP 1.1. 7m x 12m correlations may be useful to increase sensitivity. ===================================================================================== DRSP 2.1.5 Title Spatial Density Probe Comparison in Protostars and YSOs Pi J. Mangum Time 15 hrs 1. Name: Spatial Density Probe Comparison in Protostars and YSOs Authors: J. Mangum, A. Wootten 2. Science goal: Compare the spatial density derived from measurements of the molecular spectral line emission from the CS and H2CO molecules from a representative sample of protostars and YSOs. Coupled with studies of the kinetic temperature structure within these sources, spatial densities over a range from 10^5 - 10^8 cm^(-3) can be derived. 3. Number of sources: 30 4. Coordinates: 4.1. 10 sources in Oph (RA=16:30, DEC=-24) 10 sources in Perseus (RA=03, DEC=+30) 10 sources distributed over sky (RA=any, DEC=any visible) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.5" 5.2. Range of spatial scales/FOV: 30" 5.3. Single dish: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 6, Band 7 6.2. Line: H2CO 3(13)-2(12), H2CO 5(15)-4(14), CS 5-4, CS 7-6 Frequency: 211.2 GHz, 351.8 GHz, 244.9 GHz, 342.9 GHz 6.3. Spectral resolution (km/s): 0.05 km/s 6.4. Spectral coverage (km/s or GHz): 20 km/s 7. Continuum flux density: 7.1. Typical value: O.3 Jy 7.2. Continuum peak value: 0.3 Jy 7.3. Required continuum rms: 0.0002 K 7.4. Dynamic range in image: 20 8. Line intensity: 8.1. Typical value: 0.03 Jy 8.2. Required rms per channel: 0.5 K 8.3. Spectral dynamic range: 20 9. Polarization: no 10. Integration time per setting: 30 x 0.5 hrs 11. Total integration time for program: 15 hr ************************************************************************* Review John Richer: see program 2.1.1. -------------------------------------------------- Review v2.0: init_5 = 2.1.5 1. Name: Spatial Density Probe Comparison in Protostars and YSOs Authors: J. Mangum, A. Wootten Unchanged w.r.t. DRSP 1.1. 7m x 12m correlations may be useful to increase sensitivity. To what extent will continuum-only measurements already provide the density information? The combined interpretation of SEDs and continuum visibilities has become quite powerful in recent years. (I guess the answer is that this is an independent measure of the volume density) ===================================================================================== DRSP 2.1.6 Title The Connection Between Cloud Structure and the IMF Pi C. Chandler Time 400 hrs 1. Name: The Connection Between Cloud Structure and the IMF ================================================= Authors: C. Chandler, A. Wootten, J. Mangum 2. Science goal: The origin of the IMF and its relationship to the initial conditions within star forming molecular clouds is one of the major unsolved problems in star formation, and one which has implications for almost every scientific field in which ALMA will be important. We propose to conduct a large-scale survey of the Ophiuchus, Lupus, Perseus, and Orion molecular cloud complexes in order to determine this relationship. The main survey will be carried out at 1 mm, and companion survey at 3 mm is needed to enable us to distinguish unambiguously between dust and free-free emission. 3. Number of sources: 4 4. Coordinates: 4.1. Ophiuchus (RA=16:30, DEC=-24); Perseus (RA=03, DEC=+30); Lupus (RA=16, DEC=-35); Orion (RA=05:30, DEC=-05) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 1" 5.2. Range of spatial scales/FOV: 1 degree 5.3. Single dish: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 6 230 GHz Band 3 100 GHz 6.2. Line: 6.3. Spectral resolution (km/s): 6.4. Spectral coverage (km/s or GHz): 7. Continuum flux density: 7.1. Typical value: 1 mJy 7.2. Continuum peak value: 1 Jy 7.3. Required continuum rms: 0.3 mJy 7.4. Dynamic range in image: 1000 8. Line intensity: 8.1. Typical value: 8.2. Required rms per channel: 8.3. Spectral dynamic range: 20 9. Polarization: no 10. Integration time per setting: 4 x 6 s x 57600 fields at 300 GHz 4 x 1 s x 14400 fields at 100 GHz (NOTE: use OTF mosaicing) 11. Total integration time for program: 400 hr ************************************************************************* Review John Richer: see program 2.1.1. -------------------------------------------------- Review v2.0: init_6 = 2.1.6 1. Name: The Connection Between Cloud Structure and the IMF ================================================= Authors: C. Chandler, A. Wootten, J. Mangum Unchanged w.r.t. DRSP 1.1. This is a very large program. How does it compare in terms of sensitivity to what is being done with Spitzer and what is being planned with SCUBA2 on JMCT? Angular resolution will be much higher with ALMA, but do you need to do the _entire_ clouds, or just a number of representative regions to "translate" number counts and mass distributions from one scale to another? ===================================================================================== DRSP 2.1.7 Title Physical Structure of Low-mass Star-Forming Cores Pi Y. Shirley Time 120 hrs 1. Name: Physical Structure of Low-mass Star-Forming Cores Authors: Yancy Shirley, et al. 2. Science goal: Map dust continuum emission on a wide range of spatial scales to probe the density and temperature structure of the envelope and disk. Current dust continuum studies suffer from large uncertainties in the structure of the inner envelope (R < 1000 AU) and in the size/brightness of accretion disks around low-mass YSOs. The dust continuum should be imaged at submm wavelengths since the flux goes as a high power of the frequency (S ~ nu^4). A solid understanding of the physical structure (density and temperature) of the core is the foundation for all molecular line radiative transfer studies as well as a understanding of collapse dynamics. The sources chosen would have been imaged at low-resolution with the current generation of mm/submm bolometers as well as observed with SIRTF. The initial phase of the project would image several cores in a range of evolutionary states (and masses) at 850 microns. Future studies would attempt to image at higher frequencies (e.g., 450/350 microns) where questions such as changes in dust opacity due to differential dust coagulation/ice evaporation throughout the envelope and disk may be addressed. 3. Number of sources: 15 4. Coordinates: 4.1. 3 sources in Oph (RA=16:30, DEC=-24) 3 sources in Perseus (RA=03, DEC=+30) 3 sources in Taurus (RA=04, DEC=+25) 6 sources distributed over sky (RA=any, DEC=any visible) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.5" 5.2. Range of spatial scales/FOV: 11"x8" 5.3. Single dish: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 7 6.2. Line: N/A Frequency: N/A 6.3. Spectral resolution (km/s): N/A 6.4. Spectral coverage (km/s or GHz): Widest bandwidth possible 7. Continuum flux density: 7.1. Typical value: 10 - 100 mJy (disks) 7.2. Continuum peak value: a few hundred mJy (inner envelope) 7.3. Required continuum rms: 0.002 K (but require full tracks - see Note1) 7.4. Dynamic range in image: 8. Line intensity: 8.1. Typical value: N/A 8.2. Required rms per channel: N/A 8.3. Spectral dynamic range: N/A 9. Polarization: NO 10. Integration time per setting: 15 x 8 hrs 11. Total integration time for program: 120 hr Note 1: 8 hrs per source are required to sufficiently cover u,v plane. Need a large number of visibilities over a wide range of u,v-distance to reconstruct physical structure of the core. ************************************************************************* Review John Richer: see program 2.1.1. -------------------------------------------------- Review v2.0: init_7 = 2.1.7 1. Name: Physical Structure of Low-mass Star-Forming Cores Authors: Yancy Shirley, et al. Unchanged w.r.t. DRSP 1.1. ACA will be critical here, and calibration should be careful to make sure that no spurious "breaks" are created in the inferred density / temperature profiles. It is noted that 8 hrs are required to fill the uv-plane. This is not true for ALMA. With 50 antennas the uv-plane is filled quite rapidly, and detailed simulations are required to determine when it is filled sufficiently. Multi-frequency observing may be a better strategy to fill in missing spacings. ===================================================================================== DRSP 2.1.8 Title Infall velocity structure of starless cores Pi JP. Myers Time 100 hrs 1. Name: Infall velocity structure of starless cores Authors: P. Myers, T. Bourke, C. De Vries (CfA) 2. Science goal: Determine the spatial structure of inward motions in a sample of starless cores showing infall asymmetry in multiple lines at lower angular resolution. Select lines known to trace gas densities 10^4 to 10^6 cm^(-3). Select lines with minimal abundance depletion due to freeze-out onto grains (N2H+, N2D+, DCO+) to trace motions in the inner core, and with strong depletion (HCO+, HCN), to trace motions in the outer core. Select lines with resolved hyperfine structure (N2H+ 1-0, N2D+ 1-0, HCN 1-0) to probe zones along the line of sight with differing optical depth. Measure the continuum structure to obtain the density profile with radius. Compare the spectra, maps, and density profile with monte carlo radiative transfer models to constrain the velocity field with radius. Test the consistency of the velocity field with models of gravity-driven motion, including infall onto point mass and onto extended mass, and including resistive forces due to gas pressure gradients and to magnetic fields (ambipolar diffusion). 3. Number of sources: 10 4. Coordinates: 4.1. 10 sources distributed over sky (RA=any, DEC=any visible) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 1" 5.2. Range of spatial scales/FOV: 5.3. Single dish: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: 6.2. Lines: N2H+ 1-0, 3-2 N2D+ 1-0, 3-2 DCO+ 2-1, 3-2 HCN 1-0, 2-1, 3-2 HCO+ 1-0, 2-1, 3-2 6.3. Spectral resolution (km/s): 0.03 km/s 6.4. Spectral coverage (km/s or GHz): 30 km/s 7. Continuum flux density: 7.1. Typical value: O.05 Jy 7.2. Continuum peak value: 0.1 Jy 7.3. Required continuum rms: 0.001 Jy 7.4. Dynamic range in image: 8. Line intensity: 8.1. Typical value: 3 K 8.2. Required rms per channel: 0.01 K 8.3. Spectral dynamic range: 9. Polarization: no 10. Integration time per setting: 10 x 10 hrs 11. Total integration time for program: 100 hr **************************************************************************** Review John Richer: see program 2.1.1. -------------------------------------------------- Review v2.0: init_8 = 2.1.8 1. Name: Infall velocity structure of starless cores Authors: P. Myers, T. Bourke, C. De Vries (CfA) Unchanged w.r.t. DRSP 1.1. Do we still think that the maolecules mentioned are the appropriate tracers. Are we really sure we understand the chemistry and the depletion characteristics? There's overlap witg 2.1.1 where H2D+ is proposed. ===================================================================================== DRSP 2.1.9 Title Envelope Structure of Intermediate-Mass YSOs Pi J. Di Francesco Time 4850 hrs 1. Name of program and authors Envelope Structure of Intermediate-Mass YSOs James Di Francesco (NRC-HIA) 2. One short paragraph with science goal(s) The goal of this project is to probe the density and thermal structure of envelopes surrounding intermediate-mass young stellar objects by imaging the submillimeter continuum emission of selected Herbig Ae/Be stars. Herbig Ae/Be stars are young stellar objects of 2-10 Msun, which may have large infrared excesses due to reprocessing of stellar photons by dust in circumstellar disks and envelopes. Such objects may or may not have followed the same formation path as low-mass stars. Comparing the circumstellar structures of Herbig Ae/Be stars with those of low-mass objects should reveal the similarities or differences in their formation. Early work on this subject was performed by Mannings (1994; MNRAS, 271, 587) based on continuum measurements made from the JCMT. (Similar, recent studies of low-mass embedded objects have been done by Shirley et al. (2000; ApJS, 131, 249) and Young et al. (2003; ApJS, 145, 111)) The low-resolution data of Mannings, however, could not distinguish well the relative contributions of submillimeter continuum emission from disks and envelopes around the Herbig Ae/Be stars studied. ALMA will provide very sensitive, high-resolution submillimeter continuum data of the envelopes surrounding these stars. Data from 3 well-spaced bands will allow these structures to be well characterized using modern, multidimensional radiative transfer codes. 3. Number of sources 12 4. Coordinates: 4.1. Rough RA and DEC Targets are distributed at low galactic latitudes across the sky. 4.2. Moving target: No. 4.3. Time critical: No. 4.4. Scheduling constraints: (optional) None. 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.50" (all bands) 5.2. Range of spatial scales/FOV (arcsec): Wide-field mosaics over a range of spatial scales from 0.5-30" (all bands) 5.3. Required pointing accuracy: (arcsec) 0.1" (**justifiable?**) 6. Observational setup 6.1. Single dish total power data: Beneficial. Observing modes for single dish total power: OTF 6.2. Stand-alone ACA: Required. 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: Beneficial. 6.4. Subarrays of 12m baseline-ALMA antennas: No. 7. Frequencies: 7.1. Receiver band: Bands 3, 6, 9 7.2. Lines and Frequencies (GHz): n/a 7.3. Spectral resolution (km/s): n/a 7.4. Bandwidth or spectral coverage (km/s or GHz): n/a 8. Continuum flux density: (values below listed for Bands 3, 6 and 9 respectively) 8.1. Typical value (Jy): 0.01, 0.1, 1.0 Jy 8.2. Required continuum rms (Jy or K): 0.000002, 0.00002, 0.0002 Jy 8.3. Dynamic range within image: 500, 500, 500 8.4. Calibration requirements: absolute: 5%, 10%, 10% repeatability: 5%, 10%, 10% relative: 5%, 10%, 10% 9. Line intensity: 9.1. Typical value (K or Jy): n/a 9.2. Required rms per channel (K or Jy): n/a 9.3. Spectral dynamic range: n/a 9.4. Calibration requirements: absolute ( n/a ) repeatability ( n/a ) relative ( n/a ) 10. Polarization: yes/no (optional) No. 10.1. Required Stokes parameters: No. 10.2. Total polarized flux density (Jy): n/a 10.3. Required polarization rms and/or dynamic range: n/a 10.4. Polarization fidelity: n/a 10.5. Required calibration accuracy: n/a 11. Integration time for each observing mode/receiver setting (hr): 121, 81, 768 hrs 12. Total integration time for program (hr): 970 hr (+ 3880 hrs ACA time to get same sensitivity in low uv-spacing data) 13. Comments on observing strategy : (optional) Note 1: To sample well the envelopes of these objects, mosaicked observations will be necessary at the higher bands. For example, the Band 3 observations will sample the sky within 30" radius of the phase centre beam in one pointing but the Band 6 and Band 9 observations will require respectively 3x3 and 8x8 pointing mosaics to sample the same field. To get the required sensitivities across the respective fields, each object will have to be observed over 11 hrs, 6.75 hrs, and 64 hrs in Bands 3, 6, and 9 respectively. Note 2: Given the difficulties in observing at Band 9, Band 8 data could be substituted for Band 9 data in the above program. In this case, the required sensitivities could be very similar to those for Band 6, i.e., maybe an rms of 0.0001 Jy would be sufficient. In this instance, 5x5 pointing mosaics for 12 sources would be 375 hrs, and the total integration time would be 577 hrs (+ 2308 hrs ACA time). Note 3: The dynamic range goal is flexible with a minimum of 100 preferred. Integration times may be scaled down significantly to meet this minimum. Note 4: Simultaneous observations of 12CO/13CO transitions may be useful to trace gas dynamics in the envelopes, although depletion and outflows could make interpreting these data difficult. Note 5: Higher angular resolution observations will begin to probe the disks of these stars. Since this is an interesting topic of its own, it would be useful to define a DSRP for such a project in the disks sub-theme and link this project to it. Note 6: Determination of radial structure of envelopes (e.g., "p", the exponent of a radial power-law function) is more dependent upon the observed radial profile of the emission than the absolute flux values. The low-mass embedded object studies described above by Shirley et al. and Young et al. used 1-D RT codes to model continuum emission from various Class 0 and I sources and fit "p" through *normalized* angularly-averaged radial intensity profiles. These studies found that simultaneous SED fitting was less influential in determining "p". Their methods could fit "p" within +/- 0.2, although other sources of un- certainty (ISRF strength, presence of a disk) could modify "p" dramatically , e.g., ~0.5. Their JCMT data had flux uncertainties of ~10% at 850 microns and ~40% at 450 microns. We note, however, that their determinations of the envelope mass and source luminosities are dependent upon the SED. Improvements to the accuracies of low and high frequency flux data by factors of only 2-4 (e.g., 5% at Band 3 and 10% for Bands 6 and 9) for the case of ALMA data of intermediate-mass YSO envelopes would likely improve determinations of envelope mass, source luminosities and envelope "p" - the main science goals. Note 7: These objects are not expected to have submillimeter or millimeter fluxes that are variable on short (monthly) timescales, so the precision of the observations need only match the relatively low accuracy quoted above. Note 8: Again, since the SED (i.e., relative fluxes) is less important than radial intensity distributions in determining "p" through models, relative calib- ration accuracy that is superior to absolute calibration accuracy is not necessary. If, however, one wanted to find variations of dust opacities within the sources, higher relative calibration accuracy may be needed, but the requirements for that are not well known. Note 9: This program depends on making mosaics of extended submillimeter and millimeter emission. Such mosaics are made generally by stepping through a series of pre-defined sky positions separated by the Nyquist sampling distance or less. Gain stability *over the time required to make such a mosaic* (20-30 minutes?) is crucial to obtain accurate visibilities across the field. Since this project depends more on radial intensity profiles and not absolute fluxes, gain instabilities over the timescale of a pass through a mosaic could impact the science. Such time-related requirements are not specifically questioned in this survey, but it is hoped that the gain stability can be specified within some limits in the future. Moreover, Young et al. described how the shape of the JCMT beam over time affected their 450 micron observations due to thermal variations of the telescope (pointing and beam size). It is likely that the ALMA telescopes will also encounter this problem, with higher frequencies affected more than lower frequencies. Since this DRSP program involves making mosaics at high frequencies, untracked variations of the pointing and beam size will have a dramatic effect on the science. It is hoped that pointing and beam size will be monitored regularly by the ALMA Observatory. -------------------------------------------------- Review v2.0: init_9 = 2.1.9 1. Name: Envelope Structure of Intermediate-Mass YSOs ============================================ DiFrancesco Unchanged w.r.t. DRSP1.1. This is a large program requiring lots of ACA time. Would it be useful to also record the 7m x 12m correlations? Answer: Since this project involves probing the extended envelopes of intermediate mass stars, correlations of the 7m x 12m antennas may be useful. First, the added spatial frequency coverage would be welcome, provided the ACA is situated near the center of the compact ALMA 50-m configuration. Otherwise, I suspect the extended structure would be resolved out along ALMA/ACA baselines. Second, the added sensitivity would be welcome, given the same concern as to spatial frequency coverage. ===================================================================================== DRSP 2.2.1 Title Mapping the turbulence in a molecular cloud Pi J. Richer Time 121 hrs 1. Name: Mapping the turbulence in a molecular cloud Authors: J Richer 2. Science goal: To image at 2 arcsec resolution a nearby quiescent molecular cloud containing full spatial information up to the diffraction limit. Aim is to compare quantitatively with numerical models of turbulence in molecular clouds, in particular looking for filaments and shock strcutures, and the fluid flow within these. Various quantitative diagnostics will be used to compare with models (delta variance, wavelets techniques, power spectra). I have chosen the C18O 1-0 line as gas tracer. The observation will produce a 6000x6000 pixel data cube, with perhaps 40 or so spectral channel containing emission. Tis survey will also produce serendipitous sources - it has an rms of 12 micro Jy at 110GHz. 3. Number of sources: 1 4. Coordinates: 4.1. Somewhere in Ophiuchus would do, say RA=16:30, DEC=-24 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 2.0 arcsec 5.2. Range of spatial scales/FOV: 10 arcmin 5.3. Single dish: yes 5.4. ACA: possibly, perhaps not essential 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 6.2. Line: C18O 1-0 Frequency: 110 GHz 6.3. Spectral resolution (km/s): 0.1 km/s 6.4. Spectral coverage (km/s or GHz): 5 km/s 7. Continuum flux density: 7.1. Typical value: 10 mJy but irrelevant 7.2. Continuum peak value: 40 mJy 7.3. Required continuum rms: 12 micro Jy achieved (0.3mK) 7.4. Dynamic range in image: 8. Line intensity: 8.1. Typical value: 2 K 8.2. Required rms per channel: 0.15 K 8.3. Spectral dynamic range: 15 9. Polarization: no 10. Integration time: Mosaic size is 22x22 fields to cover 10x10 arcmin = 484 fields (assuming sampling at 27 arcsec, half the primary beam size at 110 GHz) Time required per field is 900 seconds to get to delta T = 0.15 K 11. Total integration time for program: 121 hrs ************************************************************************* Review Munetake Momose: OK -------------------------------------------------- Review v2.0: yso_1 = 2.2.1 1. Name: Mapping the turbulence in a molecular cloud Authors: J Richer Unchanged w.r.t. DRSP 1.1. Now this is a project where ACA is essential I would think and perhaps even getting the correlations between the 7m and 12m antennas. Some careful modeling of the response of the actual (u,v) sampling with a cloud structure may be required to settle on the optimal observational strategy. Consider multifrequency imaging for the continuum to increase the spatial sampling? ===================================================================================== DRSP 2.2.2 Title Magnetic field geometry in protostellar envelopes Pi J. Richer Time 112 hrs 1. Name: Magnetic field geometry in protostellar envelopes Authors: J Richer 2. Science goal: Make images of linearly polarised dust emission in the envelopes of protostars to constrain role of magnetic fields in star formation. 3. Number of sources: 4 4. Coordinates: 4.1. 2 sources in Oph (RA=16:30, DEC=-24) 2 sources in Taurus (RA=03, DEC=+30) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 1.0" 5.2. Range of spatial scales/FOV: 20 arcsec 5.3. Single dish: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 7 6.2. Line: Not important but most likely HCO+ 4-3 at 357GHz 6.3. Spectral resolution (km/s): 0.1 km/s 6.4. Spectral coverage (km/s or GHz): 20 km/s 7. Continuum flux density: 7.1. Typical value: 10 mK 7.2. Continuum peak value: 7.3. Required continuum rms: 130 micro K 7.4. Dynamic range in image: 8. Line intensity: 8.1. Typical value: N/A 8.2. Required rms per channel: N/A 8.3. Spectral dynamic range: N/A 9. Polarization: yes - critical 10. Integration time per setting: 4 sources x 7 pointings per source x 240 minutes per pointing In 4 hours one reaches 130 micro Kelvin of brightness sensitivity. In the inner parts (<1000 AU) of the envelope one expects emission at the level of about tens of mK and stronger (using a simple 1/r^2 isothermal envelope model). Thus one can detect few % polarisation at the several sigma level, which is just about good enough. This is very model dependent of course. 11. Total integration time for program: 112 hr ************************************************************************ Review Munetake Momose: OK. -------------------------------------------------- Review v2.0: yso_2 = 2.2.2 1. Name: Magnetic field geometry in protostellar envelopes Authors: J Richer Unchanged w.r.t. DRSP 1.1. Obvious project and calibration will be hell. Are the cross-correlation between the 7m and 12m antennas also useful, or would they only add to calibration-hell? ===================================================================================== DRSP 2.2.3 Title Structure and collapse of protostellar envelopes Pi J. Richer Time 240 hrs 1. Name: Structure and collapse of protostellar envelopes Authors: J Richer 2. Science goal: Make good resolution images of a sample of protostars in continuum and line emission. The goals are to test dynamical models of cloud collapse, and trace the accretion flow from envelope to disk, without resolving in any detail the disk structure. Moderate mosaicing is required, and good small/zero spacing measurements. Continuum and line emission both equally important to this study. The observing stategy outlined here is make large images at 3mm, smaller ones at 1mm and smaller still at 450 microns as we expect the line emission to get more compact at higher frequencies. 3. Number of sources: 10 4. Coordinates: 4.1. 5 Class 0 sources in Oph (RA=16:30, DEC=-24) 5 Class 0 sources in Taurus (RA=03, DEC=+30) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.5 arcsec 5.2. Range of spatial scales/FOV: A) 100 arcsec at 3mm B) 40 arcsec at 0.85mm C) 15 arcsec at 0.45mm 5.3. Single dish: yes 5.4. ACA: preferably 5.5. Subarrays: no 6. Frequencies: A) 6.1. Receiver band: Band 3 6.2. Line: HCO+ 1-0 and/or H13CO+ isotope in stronger sources. f=89 GHz 6.3. Spectral resolution (km/s): 0.05 km/s 6.4. Spectral coverage (km/s or GHz): 10 km/s B) 6.1. Receiver band: Band 7 6.2. Line: HCO+ 4-3 and/or H13CO+ isotope in stronger sources Frequency: 367 GHz 6.3. Spectral resolution (km/s): 0.05 km/s 6.4. Spectral coverage (km/s or GHz): 20 km/s C) 6.1. Receiver band: Band 9 6.2. Line: ? TBD, perhaps CO 6-5 isotope, HCN - no time to check freqs... Frequency: 650GHz 6.3. Spectral resolution (km/s): 0.05 km/s 6.4. Spectral coverage (km/s or GHz): 20 km/s 7. Continuum flux density: 7.1. Typical value: 7.2. Continuum peak value: 7.3. Required continuum rms: 7.4. Dynamic range in image: 8. Line intensity: 8.1. Typical value: 8.2. Required rms per channel: 1 K 8.3. Spectral dynamic range: 10 9. Polarization: no 10. Integration time: A) 4x4 mosaic, 30 minutes per pointing B) 4x4 mosaic, 30 minutes per pointing C) 4x4 mosaic, 30 minutes per pointing 24 hours per source, 11. Total integration time for program: 240 hr Notes ************************************************************************ Review Munetake Momose: This is a plan to observe protostellar envelopes at three different frequencies with an identical rms level in line brightness and velocity resolution, though the mapping area is larger at lower frequencies. Such strategy requires more observing time for lower frequencies because (Tb dv) is proportional to (lambda ^3) for the same flux density and dv, but this plan does not take it into account. As a result, the required integration time at 90GHz is severely underestimated (by a factor of ~10). Although it's not clear whether all the regions of an envelope should be mapped with an identical rms level in line brightness, the outer regions must have lower temperature/density and narrower velocity width, hence the brightness sensitivity of ~ 1K and velocity resolution of ~0.05 km/s are crucial in the 90 GHz observations, as stated in the plan. To fulfill the scientific goal within a reasonable observing time, I believe the requirement for the beam size at 90 GHz can be relaxed by a factor of ~2. Since the protostellar collapse would proceed in a "self-similar" way, angular resolution in linear scale is less important when one observes outer regions of the envelope at lower frequencies. If we take 0.9" as the beam size of the 90 GHz observations, 30-minute integration is sufficient to achieve 1 K rms at the velocity resolution of 0.05 km/s, and we don't have to change the total integration time. Concerning about the observed line in Band 9, which is not clearly specified in the plan, I also agree that it is still unclear which line is appropriate and that we should remain it TBD. -------------------------------------------------- Review v2.0: ok ===================================================================================== DRSP 2.2.4 Title Infall toward protostars Pi A. Wootten Time 900 hrs 1. Name of program and authors Infall toward protostars [2.2.4 in DRSP 1.1] A. Wootten 2. One short paragraph with science goal(s) Detect molecular line absorption against the continuum of a disk surrounding a protostar. The program is based on the detection of formaldehyde at 1.3 mm in IRAS4A by Di Francesco et al. 2001, ApJ 562, 770. Using IRAM, they detected H$_2$CO absorption at 1.3 mm of $T_b = 10$ K against a continuum of 3000 mJy with a velocity resolution of 0.16 km/s. This provides the best evidence for infall, but it is currently only possible for the few brightest sources. To generalize the result and to study the infall velocity field in detail, we would like to do similar experiments on 30 sources with 10 times weaker disks with a velocity resolution of 0.05 km/s. 3. Number of sources 30 YSOs 4. Coordinates: 4.1. Rough RA and DEC 10 sources in Oph (RA=16:30, DEC=-24) 10 sources in Perseus (RA=03, DEC=+30) 10 sources distributed over sky (RA=any, DEC=any visible) 4.2. Moving target: no 4.3. Time critical: no 4.4. Scheduling constraints: (optional) None 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.5" 5.2. Range of spatial scales/FOV (arcsec): 0.5" to 11" single field 5.3. Required pointing accuracy: (arcsec) 2" 6. Observational setup 6.1. Single dish total power data: beneficial Observing modes for single dish total power: Nutator switch 6.2. Stand-alone ACA: beneficial 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: beneficial 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, 9 7.2. Lines and Frequencies (GHz): Line: 2 freqeuncy settings in B4 4 freqeuncy settings in B6 7 frequency settings in B7 H2CO 3_12 - 2_11 Frequency: B6 226 GHz and 211 GHz. multiline H2CO 2-1 K=1, K=0 B4: 140 and 145 GHz multiline H2CO 4-3 K=2, K=1, K=0 B7: 362736.0480 363945.8940 364103.2490 364103.2490 364275.1410 364288.8840 365363.4280 GHz multiline 7.3. Spectral resolution (km/s): 0.08 km/s @ B6 7.4. Bandwidth or spectral coverage (km/s or GHz): 20 km/s 8. Continuum flux density: 8.1. Typical value (Jy): .3 Jy 8.2. Required continuum rms (Jy or K): 0.2 mJy 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 9. Line intensity: 9.1. Typical value (K or Jy): 0.03 Jy 9.2. Required rms per channel (K or Jy): 0.1 K 9.3. Spectral dynamic range: 20 9.4. Calibration requirements: absolute ( 5% ) repeatability ( 1-3% ) relative ( 1-3% ) 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 10 hr 12. Total integration time for program (hr): 30 x 3 x 10 = 900 hr 13. Comments on observing strategy : (optional) B4: The K=1 and K=0 lines lying at 140839.5020 & 145602.9490 GHz lie within the 4 GHz range of the B4 receiver and are to be observed with one correlator setting. B6: I would choose dual polarization no cross products, 8 digitizers of 125 MHz bandwidth giving 2048 channels across each placement of the digitizers. I would place these on the lines specified in this DRSP but within the expected 8 GHz bandwidth of the B6 receiver, I could also cover other lines. I would choose the 3(0,2)-2(0,2) line at 218.222 GHz, the 3(2,2)-3(2,1) line at 218.475 GHz, the 3(1,2)-2(1,1) H213CO line at 219.908 GHz and the primary target the 3(1,2)-2(1,1) H2CO line at 225.698 GHz, on each of which would be placed a digitizer pair. Note that in the latest System Technical Specs, the IF of B6 was lowered to 4.5-10 GHz but that it is expected to be capable of meeting specs across the range of the spectral lines proposed for observations (Webber and Effland, private communication). B7: The lines chosen lie within the 4 GHz range of the B7 receiver with one correlator setting. -------------------------------------------------- Review v2.0: In the course of preparation of DRSP version 2, I have reviewed your DRSP (2.2.4) entitled: "Infall toward protostars", and I have a following minor comment. This is an important program making full use of the ALMA capability. It is not very clear for me why multiple lines of H2CO (and its isotopomers) be observed. Probably some information on the infalling structure can be derived? A sentence describing this may be helpful. Furthermore it may be useful to prioritize the observing bands. ---------------------------------------------------------------------- Reply: Recall the proposed settings: H2CO 3_12 - 2_11 Frequency: B6 226 GHz and 211 GHz. multiline H2CO 2-1 K=1, K=0 B4: 140 and 145 GHz multiline H2CO 4-3 K=2, K=1, K=0 B7: 362736.0480 363945.8940 364103.2490 364103.2490 364275.1410 364288.8840 365363.4280 GHz multiline Since the optical depths of these lines will vary, the structure of the infalling gas should be derivable from the variation of its optical depth with frequency (and velocity excursions/lineshape). For example, Choi claimed that the absorption seen by DiFrancesco in the 226 GHz line occurred in a low excitation sheet of material which overlay the star forming region. If so, this sheet should not be detectable for instance in the higher excitation lines in B7 and would have greater optical depth in the low lying B4 lines. In reality, it is unlikely a single physical state exists in the absorbing material, and we would want to characterize its density structure by utilizing the many transitions H2CO offers. The plan is similar to the deconstruction of the column to a protostar used by Hurt, R. L., Barsony, M., & Wootten, A. 1996, apj, 456, 686 and similar objects in naughtily unpublished data. Each band has several lines which might be observed with a single correlator setting. Possibly, the settings for B6 would be sufficient, with next priority B4 then B7. ===================================================================================== DRSP 2.2.5 Title Magnetic field in molecular outflows Pi J. Richer Time 168 hrs 1. Name: Magnetic field in molecular outflows Authors: J Richer 2. Science goal: Make images of linearly polarised CO emission in molecular outflow sources to trace magnetic field direction in flow (Goldreich Kylafis effect). 3. Number of sources: 4 4. Coordinates: 4.1. 1 source in Oph (RA=16:30, DEC=-24) 2 sources in Taurus/Perseus (RA=03, DEC=+30) 1 in Orion (05h, 0d) Choose very compact outflows to fit mostly in primary beam - eg HH211, NGC2024-FIR5 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 1.0" 5.2. Range of spatial scales/FOV: 45 arcsec 5.3. Single dish: maybe needed 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 6.2. Line: CO 1-0 6.3. Spectral resolution (km/s): 3.0 km/s 6.4. Spectral coverage (km/s or GHz): 200 km/s 7. Continuum flux density: 7.1. Typical value: N/A 7.2. Continuum peak value: 7.3. Required continuum rms: 7.4. Dynamic range in image: 8. Line intensity: 8.1. Typical value: 1 K 8.2. Required rms per channel: 28 mK 8.3. Spectral dynamic range: 200 9. Polarization: yes - critical 10. Integration time: Need mosaic size of about 7 fields for each object 6 hours per field neeeded to get 28 mK 11. Total integration time for program: 168 hrs Notes Achieving 28 mK should be OK to detect few per cent polarisation in lines about 3-10 K bright. ************************************************************************ Review Munetake Momose: OK. -------------------------------------------------- Review v2.0: 2.2.5 Richer Magnetic field in molecular outflows (should say revised) the integration time should increase a little given fewer dishes or the sensitivity is decreased by about 20 percent but I don't think these are issues to worry about here ===================================================================================== DRSP 2.2.6 Title Energetics of the HH 80-81 molecular outflow Pi D. Shepherd Time 325 hrs DRSP 2.0, re-submittal of DRSP 1.1 project 2.2.6 1. Name: Energetics of the HH 80-81 molecular outflow. Authors: D. Shepherd et al. 2. Science Goal: HH 80-81 is a well-collimated jet powered by an intermediate mass young stellar object with a spectral type later than B1. It is the most massive star which powers a well-collimated, parsec-scale jet similar to those produced by low-mass young stellar objects. The ionized jet has a projected length of about 5 pc (Marti, Rodriguez, & Reipurth 1993; Heathcote et al. 1998). The truncated CO flow (mass ~ 460 Msun) full opening angle is roughly 40 deg and does not re-collimate (Yamashita et al. 1989). The dynamics of the jet suggest that it is a scaled-up version of a T Tauri star jet. The CO flow position angle is misaligned with the jet by roughly 30deg and it is unclear if the observed jet can power the CO flow. However, the only CO measurements that exist were done with less than Nyquist spacing, 15'' resolution, and the authors assumed the emission was optically thin. These factors place a large uncertainty on the known dynamics of the CO flow and its relationship to the ionized jet. To determine the total mass and dynamics in the molecular flow we would like to image the HH 80-81 molecular outflow in three spectral lines (12CO(J=2-1), 13CO(J=2-1), & C18O(J=2-1). The aims are to recover all emission in the flow in the CO isotopes to estimate optical depth and energetics, and trace high velocity emission to specific regions. The continuum emission between 230 & 219 GHz will be used to get the millimeter SED of the driving source(s) as well as other sources detected in the region at 6cm. The mosaic must be sensitive to size scales between 1" and 60" in the outflow, thus, ACA and Total Power measurements are absolutely required to recover the extended emission. Multi-scale reconstruction of the combined uv-data will be needed to generate the final mosaic images. 3. Number of Sources: 1 field of 15'x15' 4. Coordinates: 4.1 Central coordinates: 18 19 12.11 -20 47 30.4 (J2000), (Galactic coordinates: LII= 10.8415 BII= -2.5916) mosaic region: 15'x15' centered on above coordinates 4.2 Moving target: No 4.3 Time Critical: No 4.4. Scheduling constraints: (optional) None 5. Spatial Scales: 5.1 Angular Resolution (arcsec): 1" 5.2 Range of spatial scales/FOV (arcsec): 1" to 60" large mosaic FOV: 15'x15' 5.3. Required pointing accuracy: (arcsec) 0.6" High pointing accuracy is required for accurate mosaic imaging with this band 6 30" primary beam. 0.6" should be achievable with reference pointing. 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: Position switch in on-the-fly mapping mode 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: beneficial 6.4. Subarrays of 12m baseline-ALMA antennas: ? Not clear what this means. This project requires 3 subarrays: 1 for the ALMA 12m array, 1 for the ACA 7m array, and 1 for the ACA 12m TP antennas. 7. Frequencies: 7.1 Receiver Band: 6 7.2 Lines: Main lines of interest = CO isotopes (e.g. CO(J=2-1), 13CO(J=2-1), C18O(J=2-1)) Frequencies (GHz): 230 GHz, 220 GHz, 219 GHz (lines listed are the main lines of interest, other will also be observed). CO will be observed in the USB while 13CO & C18O will be observed in the LSB simultaneously. 7.3 Spectral Resolution (km/s): 0.3 km/s 7.4 Spectral Coverage (km/s or GHz): 200 km/s per line 8. Continuum flux density: 8.1 Typical Value: 0.5-10 mJy 8.2 Required Continuum RMS: 0.03 mJy (to detect primary driving source of the flow as well as any lower-mass YSOs in the cluster) 8.3 Dynamic Range within Image: > 20 There is expected to be bright, large-scale (>30"), diffuse emission with faint, small scale and/or extended emission overlaid or very close to the brighter emission. This will be a complicated imaging experiment. 8.4 Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 5% relative ( 1-3% / 5% / 10% / n/a ) 5% Continuum is not the highest priority science here. It will be important to see where the continuum emission is located and derive mass estimates based on that emission. But assumptions inherent in the mass calculations will be far greater than this 5% uncertainty. What will be important is that the continuum and background sources must be subtracted from the final image. For this, it is important to make sure the continuum errors have the same order of uncertainty as the line emission. 9. Line Intensity: 9.1 Typical value: > 10 Jy at 12CO line peak 10-100 mJy in high velocity wings 9.2 Required RMS per channel: 15 mJy/beam 9.3 Spectral Dynamic Range: > 10 9.4 Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 1-3% relative ( 1-3% / 5% / 10% / n/a ) 5% While absolute calibration and relative calibration between spectral lines in this band do not require extremely high accuracy, I think that the repeatability is another issue. This is a LARGE mosaic and if the line flux densities between different segments of the mosaic (taken on different days) and/or different observations of the same field (12m array & ACA) have significantly different flux densities, this will compromise the accuracy of the final mosaic deconvolution. 10. Polarization: No 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 11.1 Integration time per field for the ALMA array (interferometric and total power observations): Assuming a multi-field mosaic, 50 antennas, 30" primary beam, 15'x15' mosaic, 4 beams/arcmin => 60x60beams = 3600 fields (just less than Nyquist spaced). 15 mJy/beam RMS in each field => 2 min integration on each field (0.3 km/s resolution) x 3600 fields = 120 hrs. Because fields will overlap, we will gain roughly a root 2 increase in sensitivity over the mosaic region. Integration time = 120/sqrt(2) hrs = 85 hrs. Note on overhead: we will likely have to do several passes through the mosaic to collect the total 2 min integration required for each field. This will increase the overhead beyond what calibration and slew times require. The 12CO(2-1) line will have to be observed separately from 13CO and C18O. Doing them all at one time may mean that one polarization will have to be sacrificed ==> lowered sensitivity. This is not acceptable. Thus, 2 mosaics will have to be made, each requiring 85 hrs of total integration time. 11.2 The ACA interferometer will require 4 times more integration to achieve a similar RMS to the ALMA array but the primary beam is larger: 50" primary beam, 15'x15' mosaic ==> 36x36 beams = 1296 fields (just less than Nyquist spaced). 2x4min integration/field = 173 hrs/sqrt(2) = 120 hrs. 11.3 ACA 12m total power dishes: The extended emission in this cloud will be significantly brighter than the compact, more high-velocity, outflow emission. Nominally it should be adequate to get total power data with the same integration time as the 12m interferometer. However, this source is near the galactic plane and in a region rich with CO emission. The Total Power mosaic will likely need to be larger than the interferometer mosaic to ensure that the edge of the mosaic has emission-free regions (required to spatially smooth the image across the scanning direction to remove artifact stripes that may be present due to changes in the atmosphere between observing OFF positions). As a guess, say the 12m TP integration time will be the same as the ACA interferometer (larger mosaic, less integration time on each field). 12. Total integration time for program (hr): In summary, this project requires: * 85 hours of 12m array time * 120 hours of ACA interferometer time. * 120 hours of ACA TP time (see note in sect 11.3 for details). (Overhead is not included in this estimate.) 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): This project must obtain a larger mosaic in Total Power than the field needed to be covered by the interferometer. Actual size of the TP mosaic is uncertain (here I assume it will take 4 times longer than the 12 array to make this larger TP mosaic). For efficiency, the ACA TP antennas should be controlled in a separate subarray, ---------------------------------------------------------------- Note that this band 6 project observes CO, 13CO & C18O simultaneously. It is equally important to and valid to observe these same isotopes in other bands/transitions. However, time estimates change dramatically because all isotopes cannot be observed at the same time. Thus: Band 3, 12co and 13co(1-0) separated by about 5.1 GHz ==> must have 2 different spectral setups. Band 7: 12co and 13co(3-2) separated by about 15.2 GHz ==> this will barely fit into the USB/LSB spread but c18o(3-2) cannot be observed at the same time. Thus, you still need 2 separate tuning, one for 12co and one for 13co/c18o. Band 8: 12co and 13co(4-3) separated by 20.2 GHz ==> must have 2 different spectral setups. Band 9: 12co and 13co(6-5) separated by 30 GHz ==> must have 2 different spectral setups. All other bands that propose to observe these isotopic ratios will require double the time than this proposal. -------------------------------------------------- Review v2.0: 2.2.6 Shepherd Energetics of the HH 80-81 outflow Personally I think this map is far too large for an ALMA project and that the other proposals are a much better way to do this but undoubtedly this type of project will be accomplished by ALMA ===================================================================================== DRSP 2.2.7 Title Survey of massive molecular outflows with ACA and TP only Pi D. Shepherd Time 180 hrs DRSP 2.0, re-submittal of DRSP 1.1 project 2.2.7 1. Name: Survey of massive molecular outflows with ACA and TP only. Authors: D. Shepherd et al. 2. Science goal(s): Molecular outflows from massive and intermediate-mass young stars are generally complex and are the result of the combined energetics from several OB stars and lower mass YSOs in a relatively dense cluster. The global properties of massive flow complexes is important for understanding the star formation efficiency in massive star forming regions and being able to relate galactic and extra-galactic star formation regions. Our current understanding of massive outflows is often based on CO(J=1-0 or 2-1) images that may not cover the entire outflow and that assume optically thin emission - both of these constraints can dramatically underestimate the dynamics of the outflowing gas (often by more than a factor of 10). Thus, a survey of molecular outflows from intermediate to high-mass YSOs in 12CO(J=2-1), 13CO(J=2-1), & C18O(J=2-1) (along with several other shock and high-density tracers) using the ACA combined with total power observations would provide a uniform sample with accurate estimates of outflow, dense gas, and cluster properties. Continuum observations with at least 2GHz of bandwidth will also detect embedded high- and intermediate-mass stars in the cluster that may be contributing to the outflow dynamics. If the continuum emission can be distributed between 230 & 219 GHz will be used to estimate the millimeter SED of the driving source(s). The mosaics must also be sensitive to size scales up to about 60" in the outflow. Multi-scale reconstruction of the combined uv-data will be needed to generate the final mosaic images. High resolution is NOT required at this stage. Promising candidates will be identified during this program and high-resolution and high-sensitivity follow up studies will be proposed. ************** Note: A similar survey should be contemplated for lower mass outflows. The low-mass survey should be separate from this one because: 1) The lines chosen will likely be different (fewer high density tracers) and the spectral resolution will be different. 2) The spatial resolution should be lower (e.g. low-mass outflows are generally less than a kiloparsec away, lower resolution is required match the expected size scale in the flows). 3) The continuum sensitivity will need to be higher to detect dust emission around the less luminous sources. ************** 3. Number of sources: 20 - 10'x10' mosaics 4. Coordinates: 4.1. Rough RA and DEC: 20 sources distributed through out the galactic plane. There will likely be some clustering toward the inner quadrant of the galaxy. 4.2. Moving target: no 4.3. Time critical: no 4.4. Scheduling constraints: (optional): None 5. Spatial scales: 5.1. Angular resolution (arcsec): 10" 5.2. Range of spatial scales/FOV (arcsec): 10" to 60" FOV range from 5'-20', depends on distance & source structure. These will all be large-field mosaics. 5.3. Required pointing accuracy: (arcsec): 0.6" High pointing accuracy is required for accurate mosaic imaging with this band 6 primary beam. 0.6" should be achievable with reference pointing. 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: Position switch in on-the-fly mapping mode 6.2. Stand-alone ACA: yes 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no (*** NO ALMA ARRAY TIME REQUESTED ***) 6.4. Subarrays of 12m baseline-ALMA antennas: ? Not clear what this means. This project requires 2 subarrays: 1 for the ACA 7m array, and 1 for the ACA 12m TP antennas. 7. Frequencies: 7.1 Receiver Band: 6 7.2 Lines: Main lines of interest = CO isotopes (e.g. CO(J=2-1), 13CO(J=2-1), C18O(J=2-1)) Frequencies (GHz): 230, 220, 219 (lines listed are the main lines of interest, other will also be observed). 7.3 Spectral Resolution (km/s): 0.3 km/s 7.4 Spectral Coverage (km/s or GHz): 100-200 km/s per line 8. Continuum flux density: 8.1. Typical value (Jy): 0.5-10 mJy 8.2. Required continuum rms (Jy or K): 0.3 mJy (to detect primary driving source of the flow as well as any lower-mass YSOs in the cluster) 8.3. Dynamic range within image: > 20 There will be weak and bright, extended emission. 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 5% relative ( 1-3% / 5% / 10% / n/a ) 5% This data will be VERY valuable for archive purposes (e.g. to combine with ALMA 12m array observations of the sources made at a later time). Thus, calibration accuracy should be adquate to ensure that this data is useful. 9. Line intensity: 9.1. Typical value (K or Jy): > 10 Jy at 12CO line peak 10-100 mJy in high velocity wings 9.2. Required rms per channel (K or Jy): 60 mJy/beam 9.3. Spectral dynamic range: > 10 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 1-3% relative ( 1-3% / 5% / 10% / n/a ) 5% While absolute calibration and relative calibration between spectral lines in this band do not require extremely high accuracy, I think that the repeatability is another issue. This is a LARGE mosaic and if the line flux densities between different segments of the mosaic (taken on different days) and/or different observations of the same field ( ACA 7m & 12m dishes) have significantly different flux densities, this will compromise the accuracy of the final mosaic deconvolution. 10. Polarization: No 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 11.1 Time requested (for ACA 12-7m array) Assuming a multi-field mosaic, 50" primary beam for 7m dishes, 10'x10' mosaic, => 24x24beams = 576 fields (just less than Nyquist spaced). Estimate (ALMA sensitivity calculator doesn't work with 10" resolution), use calculator for 50 antennas, then multiply by 4 to get ACA time estimate: 60 mJy/beam RMS in each field => 10s integration on each field (0.3 km/s resolution) => 1.6hrs x 4 = 6.4hrs for one source Because fields will overlap, we will gain roughly a root 2 increase in sensitivity over the mosaic region. Integration time = 6.4/sqrt(2) hrs = 4.5 hrs times 20 sources = 90 hrs total for the survey. NOTE: this is an average time, assuming all flows mapped are 10'x10', actual time estimate may differ depending on size of actual outflow fields. 11.2 Time requested for ACA 12m total power dishes: Same as above, thus, 4.5 hr/source x 20 sources = 90 hours However, if the TP mosaic must be larger than the interferometric array (e.g. to get out of the galactic plane) then this time could increase by a factor of 4. 12. Total integration time for program (hr): * 90 hours for the ACA 7m array * 90 hours for the ACA 12m TP antennas 13. Comments on observing strategy : (optional) This project may have to obtain a larger mosaic in Total Power than the field needed to be covered by the interferometer for some sources. Actual size of the TP mosaic is uncertain. -------------------------------------------------- Review v2.0: 2.2.7 Shepherd Survey of massive molecular outflows In this, and all other projects, there seems to be an open question as to how much time is needed for the ACA component. The basic assumption seems to be 4 times the ALMA array times but I am not sure if this is well justified or not. A question I cannot answer. ===================================================================================== DRSP 2.2.8 Title Survey of the central fields in massive molecular outflow with the ALMA interferometer. Pi D. Shepherd Time 200 hrs DRSP 2.0, re-submittal of DRSP 1.1 project 2.2.8 1. Name: Survey of the central fields in massive molecular outflows with the ALMA interferometer. Authors: D. Shepherd et al. 2. Science goal(s) Molecular outflows from massive and intermediate-mass young stars are generally complex and are the result of the combined energetics from several OB stars and lower mass YSOs in a relatively dense cluster. The global properties of massive flow complexes is important for understanding the star formation efficiency in massive star forming regions and being able to relate galactic and extra-galactic star formation regions. In a companion proposal, 20 molecular outflow sources are chosen to obtain lower resolution observations of the molecular outflows and dust emission near embedded stars in the central clusters. This proposal seeks to obtain high angular resolution molecular line and continuum observations on the central fields in the survey to map the outflowing gas back to specific sources and obtain a census of the number of sources in the cluster and the mass, distribution, and kinematics of circumstellar material. Source and circumstellar properties will then be compared to outflow properties to examine trends in circumstellar material versus outflow evolution. Thus, a sensitive survey of outflow and dense molecular gas from intermediate to high-mass YSOs in lines such as 12CO(J=2-1), 13CO(J=2-1), C18O(J=2-1), C17O(2-1), and hydrogen recombination lines (H28-30alpha) (along with several other shock and high-density tracers in bands 6 & 7 (mm to submm) using the ALMA and ACA combined arrays would provide a uniform sample with accurate, high resolution estimates of high velocity gas near protostars, dense gas, and cluster properties. Continuum observations with at least 2GHz of bandwidth will also detect embedded high- and intermediate-mass stars in the cluster that may be contributing to the outflow dynamics. If the continuum emission can be distributed between 230 & 219 GHz will be used to estimate the millimeter SED of the driving source(s). 3. Number of sources 20 massive YSOs 4. Coordinates: 4.1. Rough RA and DEC: 20 sources distributed through out the galactic plane. There will likely be some clustering toward the inner quadrant of the galaxy. 4.2. Moving target: No 4.3. Time critical: No 4.4. Scheduling constraints: None 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.01" to 0.1" (depending on source) 5.2. Range of spatial scales/FOV (arcsec): 0.01" to 5" (depending on source), FOV = 30" single field 5.3. Required pointing accuracy: (arcsec) 1-2" 6. Observational setup 6.1. Single dish total power data: no (we want to resolve out some of the confusing outflow emission) 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 6 & 7 7.2. Lines and Frequencies (GHz): 7.2.1 Band 6 lines: 3 CO isotopes at 230, 220 & 219 GHz plus others (as many lines as possible) 7.2.2 Band 7 lines: Multiple lines at e.g. 294 & 303 GHz 7.3. Spectral resolution (km/s): 0.1 to 0.3 km/s (differs with line depending on whether it is an outflow or disk/dense gas tracer). 7.4. Bandwidth or spectral coverage (km/s or GHz): 20-100 km/s per line 8. Continuum flux density: 8.1. Typical value (Jy): 0.5-10 mJy 8.2. Required continuum rms (Jy or K): 0.03 mJy 8.3. Dynamic range within image: > 20 Some lines will be a mix of weak & bright emission, others will just show weak emission, depends on the line. 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 5% relative ( 1-3% / 5% / 10% / n/a ) 1-3% 9. Line intensity: 9.1. Typical value (K or Jy): > 10 Jy at 12CO line peak 10-100 mJy in high velocity wings few mJy to microJy for RRLs. 9.2. Required rms per channel (K or Jy): 3-4 mJy/beam *** NOTE: decreased required RMS from previous DRSP 1.1 proposal because decreased antennas and new sensitivity calculations show that previous proposal would have required way too much time. 9.3. Spectral dynamic range: > 100 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 1-3% relative ( 1-3% / 5% / 10% / n/a ) 1-3% 10. Polarization: No 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 11.1 Integration time per source for the ALMA array: 50 antennas, 30" primary beam, single field For a typical source/line with 0.3 km/s resolution Band 6 230 GHz: ~3 mJy/beam RMS in each field => 1 hr integration x 20 sources = 20 hrs Band 7 300 GHz: 1 hrs (4mJy/bm RMS) x 20 sources = 20 hrs 10.2 ACA observations take about 4 times longer to achieve a similar RMS as the ALMA array. Thus, this project requires Band 6: 1x4 hrs integration x 20 sources = 80 hrs. Band 7: 1x4 hrs x 20 sources = 80 hrs 12. Total integration time for program (hr): * ALMA 12m array = 40 hrs (20 each in Bands 6 & 7) * ACA 7m array = 160 hrs * (no total power requested) 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): -------------------------------------------------- Review v2.0: 2.2.8 Shepherd Survey of the central fields in massive molecular outflows There should not be an ACA component in this proposal in sections 11 and 12 they are a mistake due to cutting and pasting. There may also be a problem with emission outside the primary beam affecting the map fidelity. Given that this project follows 2.2.7 it may be desired to place a constraint on extended structures in choosing which regions to observe. ===================================================================================== DRSP 2.2.9 Title Deep integration on the massive jet source HH80-81: the disk-outflow connection Pi D. Shepherd Time 95 hrs DRSP 2.0, re-submittal of DRSP 1.1 project 2.2.9 1. Name: Deep integration on the massive jet source HH80-81: the disk-outflow connection. 2. Science goal(s): HH 80-81 is a well-collimated jet powered by an intermediate-mass young stellar object with a spectral type later than B1. It is the most massive star known which powers a well-collimated, parsec-scale jet similar to those produced by low-mass young stellar objects. The dynamics of the jet suggest that it is a scaled-up version of a T Tauri star, thus, it should have an accretion disk with a *VERY* powerful wind. Assuming the outflow and central source has been mapped with ALMA and the source powering the outflow jet has been identified, this proposal seeks to map several outflow/disk tracers to get a handle on the disk properties and the outflowing wind as close to the surface of the disk as possible. Obtaining clear evidence for ionized or molecular gas outflow from the disk and providing constraints on where the outflow gas originates will help to determine whether a disk wind or X-wind powers this massive flow. This proposal requires very sensitive observations (to detect faint emission originating from the disk surface) at high resolution to resolve out confusing, extended emission. The disk radius that is relevant should be about 1-100 AU (= 0.5-50 mas at distance of 1.7 kpc). At 270-700 GHz (bands 7 & 9), the array will have a resolution of roughly 8-13 mas - this seems like a reasonable compromise between getting adequate resolution to see the fine-scale structure and not resolving out too much of the disk material. Lines of interest include hydrogen recombination lines (H25a, H21a) to trace ionized outflow, molecular disk tracers (e.g. CH3CN), and molecular outflow tracers (e.g. 12CO, C34S, 13CO, SiO, H13CO+) and even a H2O maser transition. 3. Number of sources: 1, single field. 4. Coordinates: 4.1. Rough RA and DEC Central coordinates: 18 19 12.11 -20 47 30.4 (J2000), (Galactic coordinates: LII= 10.8415 BII= -2.5916) 4.2. Moving target: no 4.3. Time critical: no 4.4. Scheduling constraints: (optional) None 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.008"-0.013" (depending on line) 5.2. Range of spatial scales/FOV (arcsec): 10-1000 AU = 0.005" - 0.5" single field 5.3. Required pointing accuracy: 1 arcsec 6. Observational setup 6.1. Single dish total power data: no Observing modes for single dish total power: N/A 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA & 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no 7. Frequencies: 7.1. Receiver band: Bands 7 and 9 7.2. Lines and Frequencies (GHz): 7.2.1 Receiver band 7: 6-10 lines around 280, 300, 340 GHz 7.2.2 Receiver band 9: 12-15 lines around 613-694 GHz. 7.3. Spectral resolution (km/s):0.1 to 0.3 km/s (differs with line depending on whether it is an outflow or disk/dense gas tracer). 7.4. Bandwidth or spectral coverage (km/s or GHz): 20-200 km/s per line 8. Continuum flux density: 8.1. Typical value (Jy): 0.5-10 mJy 8.2. Required continuum rms (Jy or K): 0.03 mJy (to detect primary driving source of the flow as well as any lower-mass YSOs in the cluster) 8.3. Dynamic range within image: > 20 Mixture of weak and bright emission in some lines. 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 5% relative ( 1-3% / 5% / 10% / n/a ) 5% 9. Line intensity: 9.1. Typical value (K or Jy): Unknown at this resolution, this will be a deep survey to see if any are detected. At lower resolution, all lines are strong in star forming regions. We want microJy RMS levels. 9.2. Required rms per channel (K or Jy): It would be good to get 1 microJy/beam but this is unreasonable. Band 7: Choose 1 mJy/beam with 0.3 km/s resolution Band 9: Choose 2 mJy/beam 9.3. Spectral dynamic range: > 100 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 1-3% relative ( 1-3% / 5% / 10% / n/a ) 1-3% 10. Polarization: No 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 12. Total integration time for program (hr): 10.1 Integration time: For a line with 0.3 km/s resolution: 1 mJy/beam RMS => 15 hrs integration (band 7, 275-370 GHz) 2 mJy/beam RMS => 80 hrs integration (band 9, 602-720 GHz) 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): -------------------------------------------------- Review v2.0: 2.2.9 Shepherd Deep integration on the massive jet source HH80-81 This project is fine as written although I agree with Munetake that it is not clear such high velocity resolution is needed in the first instance. That said, undoubtedly ALMA will try and do this type of observation! ===================================================================================== DRSP 2.2.10 Title The internal structure of the BHR71 outlow Pi F.Gueth Time 65 hrs 1. Name: The internal structure of the BHR71 outlow Authors: F.Gueth 2. Science goal: Detailed study of the CO and SiO line emission in an extremely young (Class 0) protostellar outflow, such as BHR 71. The goal is to i) study the internal structure and formation mechanism of the outflow using a flow (CO) and shock (SiO) tracer, and ii) investigate the physical conditions of the emitting gas by multi-transition analysis. The observing strategy is therefore to map the outflow in three different transitions, at the same angular resolution. This could require a different configuration to be used for each line. Mosaicing as well as short-spacings measurements are definitely required. 3. Number of sources: 1 4. Coordinates: 4.1. RA = 11:59, DEC= -64:52 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 1 arcsec 5.2. Range of spatial scales: 1" to 10' FOV: 2' x 10' 5.3. Single dish: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: a) 6.1. Receiver band: Band 3 6.2. Line: CO 1-0 6.3. Spectral resolution (km/s): 1.0 km/s 6.4. Spectral coverage (km/s or GHz): 30 km/s b) 6.1. Receiver band: Band 6 6.2. Line: CO 2-1 6.3. Spectral resolution (km/s): 1.0 km/s 6.4. Spectral coverage (km/s or GHz): 30 km/s c) 6.1. Receiver band: Band 7 6.2. Line: CO 3-2 6.3. Spectral resolution (km/s): 1.0 km/s 6.4. Spectral coverage (km/s or GHz): 30 km/s d) 6.1. Receiver band: Band 3 6.2. Line: SiO 2-1 6.3. Spectral resolution (km/s): 1.0 km/s 6.4. Spectral coverage (km/s or GHz): 30 km/s e) 6.1. Receiver band: Band 6 6.2. Line: SiO 5-4 6.3. Spectral resolution (km/s): 1.0 km/s 6.4. Spectral coverage (km/s or GHz): 30 km/s f) 6.1. Receiver band: Band 7 6.2. Line: SiO 8-7 6.3. Spectral resolution (km/s): 1.0 km/s 6.4. Spectral coverage (km/s or GHz): 30 km/s 7. Continuum flux density: 7.1. Typical value: total flux of a few Jy, but spread over 2' 7.2. Continuum peak value: unkwown 7.3. Required continuum rms: probably < 0.1 mJy/b 7.4. Dynamic range in image: >10 at all frequencies 8. Line intensity: 8.1. Typical value: up to 10 K for CO, 0.5 (or less) K for SiO 8.2. Required rms per channel: 0.3 K for CO, 0.05 K for SiO 8.3. Spectral dynamic range: 10 9. Polarization: no 10. Integration time Integration time are computed for a 1 km/s velocity resolution and a 2 arcsec angular resolution. The number of fields corresponds to a 2 x 10 arcmin field of view, assuming half-power primary beam overlap. The increase of sensitivity provided by the overlap of adjacent beams has not been taken into account. a) 4 x 20 fields mosaic 300 s per field to obtain 0.1 K rms b) 8 x 40 fields mosaic 60 s per field to obtain 0.06 K rms c) 12 x 64 fields mosaic 60 s per field to obtain 0.04 K rms d) 3 x 16 fields mosaic 600 s per field to obtain 0.1 K rms e) 8 x 40 fields mosaic 100 s per field to obtain 0.05 K rms f) 12 x 64 fields mosaic 100 s per field to obtain 0.03 K rms Total: a) 7 h b) 6 h c) 13 h d) 8 h e) 9 h f) 22 h 11. Total integration time for program: 65 hr on source with ALMA + overheads (pointing etc). Short spacings will be obtained with ACA (240 h observations) and single-dish (960h total observations, eg 240h with 4 antennas or 15h with 64 antennas). Notes Number of fields in each mosaics are estimated with half-power overlaps bewteen adjacent fields. For larges mosaic, we should be able to use OTF mosaicing. Before starting this program, it would be wise to have a couple of single-dish observations of each line, in order to get a good estimate of the lines intensities, and thus optimize the integration time. ********************************************************************* Review Munetake Momose: Science scope is OK, but time estimate for SiO lines seems to be significantly underestimated. According to the ALMA sensitivity calculator, the resultant rms levels in line brightness for the quoted integration time are d) SiO(2-1)@86.8GHz : 0.33 K if T=600 sec, e) SiO(5-4)@217.1GHz : 0.197K if T=100sec, f) SiO(8-7)@347.3GHz : 0.129K if T=100sec. (when the resolution is 1" and dV=1km/s.) Even if one takes into account the factor of ¥sqrt(2) improvement in a mosaicked map, the above rms levels do not fulfill the requirement (0.05 K). The correct estimates to achieve 0.1K rms in the SiO(2-1) map and 0.05K in the SiO(5-4)/(8-7) maps may be d) 3000 sec. per field (0.15K in rms) or 40 hr in total, e) 800 sec. per field (0.07K in rms) or 71 hr in total, f) 350 sec, per field (0,07K in rms) or 75 hr in total. Therefore the total integration time to observe both the CO and SiO lines may be 212 hours. Reply Gueth: Concerning SiO: in fact, in order to avoid too long an observing time, I computed the integration times with a 2" beam (not a 1" as assumed by Munetake). I'm sorry for the confusion. I have updated section 10. the section 10 as follows: Note that I also updated the numbers for CO, which were too pessimistic. Comment Ewine: new DRSP is now baseline -------------------------------------------------- Review v2.0: 2.2.10 Gueth The intenal structure of the BHR71 outflow This project appears fine as written. ===================================================================================== DRSP 2.2.11 Title Inner kinematics in pre-stellar cores with H2D+ Pi A. Bacmann Time 360 hrs 1. Name of program and authors Inner kinematics in pre-stellar cores with H2D+ A. Bacmann 2. One short paragraph with science goal(s) Determining the kinematics in pre-stellar cores is essential to constrain the initial conditions of gravitational collapse, especially in the centers where the collapse is supposed to start. In the cold and dense interiors of pre-stellar cores, heavy molecules have been shown to be depleted, so that only light species may be used to trace the kinematics. H2D+ is abundant in pre-stellar objects, and one of the few species not affected by depletion. This project proposes to map the velocity field of a sample of pre-stellar cores in the ortho H2D+ line at 372.4 GHz. Modelling of the line profiles over the cores will make it possible to determine whether infall has already started and to determine the nature of the motions (infall/rotation). 3. Number of sources ~10 The sources should span a range of evolution stages (e.g. various central densities) (e.g., 1 deep field of 4'x4', 50 YSO's, 300 T Tauri stars with disks, ...; do NOT list individual sources or your "pet object", except in special cases like LMC, Cen A, HDFS) 4. Coordinates: 4.1. Rough RA and DEC ~ 4 in Taurus (isolated star formation), ~ 4 in Ophiuchus (clustered star formation) + 2-3 cores scattered in RA, DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 30 in Lupus) Indicate if there is significant clustering in a particular RA/DEC range (e.g., if objects in one particular RA range take 90% of the time) 4.2. Moving target: yes/no (e.g. comet, planet, ...) no 4.3. Time critical: yes/no (e.g. SN, GRB, ...) no 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.5" 5.2. Range of spatial scales/FOV (arcsec): extended sources (larger than primary beam) (optional: indicate whether single-field, small mosaic, wide-field mosaic...) small mosaic the mosaic should cover the inner 30" of the cores, ie around 9 fields 5.3. Required pointing accuracy: (arcsec) 1" 6. Observational setup 6.1. Single dish total power data: no/beneficial/required required (extended sources) Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no/beneficial/required 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no/beneficial/required 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no no 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9 Band 7 7.2. Lines and Frequencies (GHz): single line, 372.4 GHz (approximate; do _not_ go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify, e.g., "6 frequency settings in Band 3". Apply redshift correction yourself.) 7.3. Spectral resolution (km/s): 0.1 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 30 km/s 8. Continuum flux density: 8.1. Typical value (Jy): (take average value of set of objects) (optional: provide range of fluxes for set of objects) 8.2. Required continuum rms (Jy or K): 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 9. Line intensity: 9.1. Typical value (K or Jy): 0.4 K (between 0.1 and 1 K) (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): rms 40 mK in this project, it is required to fit the line profile, therefore 10 sigma detections should be achieved. 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) absolute: 10% repeatability: 5% relative: 5% 10. Polarization: yes/no (optional) no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 4 hours per field ie 36 hours per source (this takes the overlap of the mosaic fields into account). The time estimator does not accept the frequency of the line, though the receivers will be tunable at 372.4 GHz. Therefore the time estimation was carried out at 370 GHz. 12. Total integration time for program (hr): 360 hrs 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): -------------------------------------------------- Review v2.0: 2.2.11 Bacmann Inner kinematics in pre-stellar cores with H2D+ This project shows that some extremely important observations by ALMA will take considerable time! I am trying to figure out with Aurore whether there is any errors in the integration times as I get different results than her - stay tuned. ===================================================================================== DRSP 2.2.12 Title Proving the existence of Keplerian rotation about a 20 solar masses young star Pi M. Beltran Time 55 hrs DRSP 2.0 - section 2.2 proposal 1. Name: Proving the existence of Keplerian rotation about a 20 solar masses young star Authors: M.Beltran 2. Science goal: G24.78+0.08 A1 is a unique example of a bipolar outflow/rotating toroid system undergoing infall towards a central O star with a mass of ~20 solar masses, based on the free-free continuum flux at cm wavelengths. Unlike disks in lower mass stars, the rotation curve of this toroid, which has a mass of ~130 solar masses and a diameter of ~0.04 pc, is not Keplerian. "True" circumstellar disks, which have been found in B type stars (e.g. Cesaroni et al. 2006), might be so elusive in O stars due to an observational bias, since O stars are on average more distant than B stars. However, disks might be "hidden" inside the massive toroids. Therefore, despite the large mass of the toroid, close enough to the star rotation might become Keplerian: this will occur inside the radius enclosing a gas mass comparable to that of the star, which for G24.78+0.08 A1 is ~0.5". The goal of this proposal is (i) to prove the existence of a Keplerian accretion disk around a young O star; and (ii) to obtain a precise estimate of the stellar mass to be compared with that derived from the free-free continuum of the associated hypercompact HII region. This goal can be achieved by imaging 13-CH3CN transitions in the densest parts of the rotating toroid. The advantage of observing the optically thin isotopomer 13-CH3CN instead of CH3C-13N, which are expected to have the same intensity (Olmi et al. 1996), is that CH3C-13N lines are affected by blending with the K >= 5 components of CH3CN. On the other hand, CH3CN lines could be too optically thick to trace the region of 1" in diameter. By observing different transitions of 13-CH3CN, it will be possible to measure the rotational temperature (which one expects to be ~equal to the kinetic temperature) and column density of the gas in the embedded disk by means of the rotation diagram method. For this purpouse it may be useful to observe different transitions of CH3C-13N (and/or CH3CN v8=1, vibrationally excited) as well. 3. Number of sources: 1 4. Coordinates: 4.1. Rough RA and DEC RA = 18:36:12.57, DEC= -07:12:10.9 4.2. Moving target: no 4.3. Time critical: no 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution: ~< 0.5 arcsec 5.2. Range of spatial scales: up to 3 arcsec 5.3. Required pointing accuracy: 1'' ##### Maite: is this pointing accuracy reasonable? Also, I added section below saying you don't need ACA. 6. Observational setup 6.1. Single dish total power data: no Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver Bands: 4 & 6 & 8 ------------------------------------------------------------------ 7.2 Lines and Frequencies (GHz): Band 4 Lines & Frequencies: (13)CH3CN 7(0)-6(0) 125.061 GHz \ CH3(13)CN 7(0)-6(0) 128.716 GHz | 4.1 GHz sep CH3CN 7(0)-6(0) v8=1 l=+1 129.162 GHz / (13)CH3CN 8(0)-7(0) 142.926 GHz \ CH3(13)CN 8(0)-7(0) 147.102 GHz | 4.7 GHz sep CH3CN 8(0)-7(0) v8=1 l=+1 147.611 GHz / ##### Band 4: Max separation allowed within one sideband = 4 GHz. USB and LSB are separated by 8 GHz so you can observe lines that are separated by 8-16 GHz or within 4 GHz. You have to observe the 125 GHz line separate from 128/129 GHz and observe the 142 GHz line separate from the 147 GHz lines. 22.6 GHz separation between 125 and 147 GHz lines. ==> need to observe each group separately (can't get them in USB and LSB). Band 6 Lines & Frequencies: (13)CH3CN 12(0)-11(0) 214.374 GHz \ CH3(13)CN 12(0)-11(0) 220.638 GHz | 7 GHz sep CH3CN 12(0)-11(0) v8=1 l=+1 221.394 GHz / ##### Band 6: Max separation allowed within one sideband = 4 GHz. USB and LSB are separated by 12 GHz although you can get a separation of only 8 GHz with some decrease in performance. You can observe the 220 and 221 GHz lines together but will have to get the 214 GHz line separately. Band 8 Lines & Frequencies: (13)CH3CN 26(0)-25(0) 464.277 GHz \ CH3(13)CN 26(0)-25(0) 477.838 GHz | 15 GHz sep CH3CN 26(0)-25(0) v8=1 l=+1 479.369 GHz / ##### Band 8: Max separation allowed within one sideband = 4 GHz. USB and LSB are separated by 8 GHz so you can observe lines that are separated by 8-16 GHz or within 4 GHz. So you can get these in one observation, 477/479 lines in the USB and 464 line in the LSB. ------------------------------------------------------------------- 7.3. Spectral resolution (km/s): ~<0.3 km/s 7.4. Bandwidth or Spectral coverage (km/s or GHz): <20 km/s ##### Maite: I would recommend making the BW larger here so you can subtract continuum easily if you need it. Say, 50-100 km/s? This is easy for ALMA. 8. Continuum flux density: 8.1. Typical value: total flux ~0.2-1 Jy spread over ~1.5" at (2mm and 1mm). Continuum peak value expected to be a few mJy/beam for a <0.5" resolution 8.2. Required continuum rms: 0.1 mJy/b 8.3. Dynamic range in image: low 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 5% relative ( 1-3% / 5% / 10% / n/a ) 5% ##### Maite: Is this reasonable calibration accuracy for your project? 1-3% is hard to do so only ask for it if you need it. But if you need it to get the rotation diagram accurate, then specify 1-3%. 9. Line intensity: 9.1. Typical value: expected ~0.5-1 K for band 4 transitions and 3-4 K for band 6, for a resolution of 0.5" unknown for band 8 transitions 9.2. Required rms per channel: 0.1-0.2 K, depending on the band 9.3. Spectral dynamic range: low 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 5% relative ( 1-3% / 5% / 10% / n/a ) 5% ##### Maite: again, check to make sure this is reasonable. 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): Band 3: rms ~0.1 K (line brightness) per 10 hours integration time, for a spectral resoluion of 1 km/s and resolution of 0.5" per tuning. ##### Maite: multiply this by 4 based on arguments above. Band 6: rms 0.2 K (line brightness) per 20 hours integration time, for a spectral resolution of 0.3 km/s and resolution of 0.3" Probably, the band 6 is the most suitable to carry on the kinematical study of the velocity field, that's why better spectral and angular resolutions are required. ##### Maite: multiply this by 2. Band 7: rms 0.2 K (line brightness) per 15 hours integration time, for a spectral resolution of 0.3 km/s and resolution of 0.3". The transitions in this band would probably allow us to trace material closer to the central star, however, the expected line intensities for the transitions in this band are unknown. 12. Total integration time for program: 55 hr on source with ALMA + overheads (pointing etc). ##### Maite: So total observing time would be 4x10 + 2x20 + 15 = 95 hours plus overhead. 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): DRSP 2.0 - section 2.2 proposal 1. Name: Proving the existence of Keplerian rotation about a 20 solar masses young star Authors: M.Beltran 2. Science goal: G24.78+0.08 A1 is a unique example of a bipolar outflow/rotating toroid system undergoing infall towards a central O star with a mass of ~20 solar masses, based on the free-free continuum flux at cm wavelengths. Unlike disks in lower mass stars, the rotation curve of this toroid, which has a mass of ~130 solar masses and a diameter of ~0.04 pc, is not Keplerian. "True" circumstellar disks, which have been found in B type stars (e.g. Cesaroni et al. 2006), might be so elusive in O stars due to an observational bias, since O stars are on average more distant than B stars. However, disks might be "hidden" inside the massive toroids. Therefore, despite the large mass of the toroid, close enough to the star rotation might become Keplerian: this will occur inside the radius enclosing a gas mass comparable to that of the star, which for G24.78+0.08 A1 is ~0.5". The goal of this proposal is (i) to prove the existence of a Keplerian accretion disk around a young O star; and (ii) to obtain a precise estimate of the stellar mass to be compared with that derived from the free-free continuum of the associated hypercompact HII region. This goal can be achieved by imaging 13-CH3CN transitions in the densest parts of the rotating toroid. The advantage of observing the optically thin isotopomer 13-CH3CN instead of CH3C-13N, which are expected to have the same intensity (Olmi et al. 1996), is that CH3C-13N lines are affected by blending with the K >= 5 components of CH3CN. On the other hand, CH3CN lines could be too optically thick to trace the region of 1" in diameter. By observing different transitions of 13-CH3CN, it will be possible to measure the rotational temperature (which one expects to be ~equal to the kinetic temperature) and column density of the gas in the embedded disk by means of the rotation diagram method. For this purpose it may be useful to observe different transitions of CH3C-13N (and/or CH3CN v8=1, vibrationally excited) as well, if it's possible to observe them simultaneously with the 13-CH3CN lines. 3. Number of sources: 1 4. Coordinates: 4.1. Rough RA and DEC RA = 18:36:12.57, DEC= -07:12:10.9 4.2. Moving target: no 4.3. Time critical: no 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution: ~< 0.5 arcsec 5.2. Range of spatial scales: up to 3 arcsec 5.3. Required pointing accuracy: 1'' 6. Observational setup 6.1. Single dish total power data: no Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver Bands: 4 & 6 & 8 ------------------------------------------------------------------ 7.2 Lines and Frequencies (GHz): #### In the list below, it appears only the frequency for the K=0 component, but the goal of the proposal is to observe as many K components as possible. Band 4 Lines & Frequencies: (13)CH3CN 7(0)-6(0) 125.061 GHz CH3(13)CN 7(0)-6(0) 128.716 GHz (13)CH3CN 8(0)-7(0) 142.926 GHz ##### Band 4: (13)CH3CN 7-6 can be observed simultaneously with CH3(13)CN 7-6 as they fall within one sideband of 4 GHz. (13)CH3CN 8-7 will be observed separately with a different tuning. Band 6 Lines & Frequencies: (13)CH3CN 12(0)-11(0) 214.374 GHz Band 8 Lines & Frequencies: (13)CH3CN 26(0)-25(0) 464.277 GHz CH3(13)CN 26(0)-25(0) 477.838 GHz CH3CN 26(0)-25(0) v8=1 l=+1 479.369 GHz ##### Band 8: these lines can be observed simultaneously by placing (13)CH3CN 26-25 in the LSB and CH3(13)CN 26-25 and CH3CN 26-25 v8=1 l=+1 in the USB. ------------------------------------------------------------------- 7.3. Spectral resolution (km/s): ~<0.3 km/s 7.4. Bandwidth or Spectral coverage (km/s or GHz): 50-100 km/s 8. Continuum flux density: 8.1. Typical value: total flux ~0.2-1 Jy spread over ~1.5" at (2mm and 1mm). Continuum peak value expected to be a few mJy/beam for a <0.5" resolution 8.2. Required continuum rms: 0.1 mJy/b 8.3. Dynamic range in image: low 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 5% relative ( 1-3% / 5% / 10% / n/a ) 5% 9. Line intensity: 9.1. Typical value: expected ~0.5-1 K for band 4 transitions and 3-4 K for band 6, for a resolution of 0.5" unknown for band 8 transitions 9.2. Required rms per channel: 0.1-0.2 K, depending on the band 9.3. Spectral dynamic range: low 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 5% relative ( 1-3% / 5% / 10% / n/a ) 5% 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): Band 4: rms ~0.1 K (line brightness) per 10 hours integration time, for a spectral resolution of 1 km/s and resolution of 0.5" per tuning. Therefore, a total of 20 hours integration time for the 2 tunings. Band 6: rms 0.2 K (line brightness) per 20 hours integration time, for a spectral resolution of 0.3 km/s and resolution of 0.3" Probably, bands 6 and 8 are the most suitable to carry on the kinematical study of the velocity field, that's why better spectral and angular resolutions are required. Band 7: rms 0.2 K (line brightness) per 15 hours integration time, for a spectral resolution of 0.3 km/s and resolution of 0.3". The transitions in this band would probably allow us to trace material closer to the central star, however, the expected line intensities for the transitions in this band are unknown. 12. Total integration time for program: 2x10 + 20 + 15 = 55 hr on source with ALMA plus overhead 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): -------------------------------------------------- Review v2.0: 2.2.12 - 2.2.15 I found no problems with these proposals other than the standard question of calculating ACA time. ===================================================================================== DRSP 2.2.13 Title Resolving the jet-disk interaction Pi H. Beuther Time 18 hrs DRSP 2.0 - section 2.2 proposal 1. Name of program: Resolving the jet-disk interaction Author: Henrik Beuther et al. 2. One short paragraph with science goal(s) Protostellar jets and molecular outflows are believed to be driven by magneto-centrifugal winds emanating from the inner regions of the accretion disks. These jets are considered to be the prime mechanism to remove excess angular momentum from the protostellar system and hence allow the protostar to rotate only moderately far below break-up speed. However, there exists only scarce observational evidence of the jet-acceleration and the momentum transport from the accretion disk into the protostellar jet and molecular outflow. While the jet-acceleration is already interesting in itself, the angular momentum problem and its transport to large distances away from the protostar is a central issue in star formation in general. The actual magneto-centrifugal jet-acceleration processes take place on scales of a few AU, below the capability of ALMA in its early science phase. However, observing jet and disk rotational signatures at slightly larger spatial scales (between 10 and 100AU) allows to infer the central physical processes indirectly (Ray et al., PPV). The rotation of the accretion disks can be observed on scales between 10 and a few 100AU (e.g., Simon et al. 2000), and we expect to observe jet rotation also up to scales of 50-100AU. For example, assuming momentum conservation, a typical jet has an Alfven surface of ~5AU, and below the Alfven surface its velocity scales with 1/r where r is the distance from the jet-axis. Following Bacciotti et al. (2002), we can expect jet-rotational velocities of approximately 19, 10 and 6 km/s at 15, 30, and 50AU from the jet-axis, respectively. For typical low-mass disk-jet sources at distances between Taurus (140pc) and Orion (450pc), this requires a spatial resolution of ~0.05'' and a velocity resolution in the sub-km/s regime, both well in the range of ALMA. Therefore we propose to observe 3 well-known disk-jet sources in the high-excitation line of SiO(11-10) to study the collimated jet, and in CS(10-9) to investigate the accretion disk. The SiO(11-10) line has previously been detected toward one of the candidate sources, and CS should be easily detected in such kind of source as well. Studying the kinematics of the combined jet-disk system will allow to investigate the jet-disk-rotation, the jet acceleration as well as the momentum transport in these systems. 3. Number of sources: 3 disk-jet sources 4. Coordinates: 4.1. Rough RA and DEC One in Taurus, one in IC348 and one in Orion 4.2. Moving target: no 4.3. Time critical: no 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.05'' (~3.5km baselines at 480GHz) 5.2. Range of spatial scales/FOV (arcsec): 0.05'' to 10'', single-fields are sufficient 5.3. Required pointing accuracy: 1'' 6. Observational setup 6.1. Single dish total power data: no Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 8 7.2. Lines and Frequencies (GHz): SiO(11-10) at 477.5GHz and CS(10-9) at 489.8GHZ 7.3. Spectral resolution (km/s): 0.5km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 8GHz for the continuum and 2 times 100km/s for the spectral lines. 8. Continuum flux density: 8.1. Typical value (Jy): a few mJy to a few 10 mJy 8.2. Required continuum rms (Jy or K): 0.5mJy 8.3. Dynamic range within image: 100 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 10% repeatability ( 1-3% / 5% / 10% / n/a ) 10% relative ( 1-3% / 5% / 10% / n/a ) 10% 9. Line intensity: 9.1. Typical value (K or Jy): between a few 10 and a few 100mJy 9.2. Required rms per channel (K or Jy): ~5mJy/beam 9.3. Spectral dynamic range: 500 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 10% repeatability ( 1-3% / 5% / 10% / n/a ) 10% relative ( 1-3% / 5% / 10% / n/a ) 10% 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 6 hours on-source, plus overhead. 12. Total integration time for program (hr): 18 hours plus overhead for calibration, pointing etc. 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): -------------------------------------------------- Review v2.0: 2.2.12 - 2.2.15 I found no problems with these proposals other than the standard question of calculating ACA time. ===================================================================================== DRSP 2.2.14 Title Probing the outflow launching mechanism through observations of the molecular outflow rotation Pi H. Arce Time 80 hrs DRSP 2.0 - section 2.2 proposal 1. Name of program and authors Name: Probing the outflow launching mechanism through observations of the molecular outflow rotation Author: Hector G. Arce 2. Science goal: The leading theories on the origin of protostellar outflows indicate that they are generated through the interaction of ionized disk material and the rotating magnetic filed lines anchored to the star+disk system. Until a few years ago it was thought that observational test of these models were practically impossible, as the launching process is believed to occur within only a few AU (or less) of the source. However, recent theoretical studies have shown that the launching radius of a disc wind can be derived from the rotation and speed of the jet observed at large distances (tens to hundreds of AU) from the source (Anderson et al. 2003; Ferreira et al. 2006). High resolution observations of regions tens to hundreds of AU from the young stars using HST have detected rotation in the jets of four T Tauri sources (Coffey et al. 2004; Ferreira et al. 2006, and references therein), and from their measurements they estimate jet launching radii of 0.2 to 3 AU (implying an extended disk wind is the source of the observed outflow). The existing HST outflow rotation studies can only investigate optical jets from T Tauri (class II) stars (young stars about a few million years old), and cannot probe the rotation in outflows from younger and more embedded (Class 0/I) sources (a few 10^4 to a few 10^5 yrs old). (Sub)millimeter molecular line observations are required to study the entrained molecular gas (i.e., the molecular outflow) and probe the outflow rotation in young embedded sources. In order to constrain the models of outflow launching mechanism in young protostars and investigate if there are any changes in the mechanism as young stars evolve, observations of the outflow rotation in Class 0/I sources are needed. We plan to observe the CO(3-2) at high velocity and angular resolution (0.1 km/sec and 0.5", respectively) to probe the high-velocity molecular outflow and search for outflow rotation. Simultaneous observations of HCN(4-3) and H13CN(4-3) will probe the inner regions of the circumstellar gas and will allow us to investigate the rotational motion of the envelope/disk material close to the protostar and outflow launching region (uncontaminated by outflow motions). 3. Number of sources A sample of 5 Class 0 and 5 Class I sources with known molecular outflows in the Taurus and Ophiuchus molecular clouds. 4. Coordinates: 4.1. Rough RA and DEC About 5 sources in Taurus (R.A. 4:30, Dec 24:00) and about 5 sources in Ophiuchus (R.A. 16:24, Dec. -24:25) 4.2. Moving target: NO 4.3. Time critical: NO 4.4. Scheduling constraints: NO 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.4" 5.2. Range of spatial scales/FOV (arcsec): 0.4 to 12" (single field) 5.3. Required pointing accuracy: 1" 6. Observational setup 6.1. Single dish total power data: NOT REQUIRED 6.2. Stand-alone ACA: NOT REQUIRED 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: NOT REQUIRED 6.4. Subarrays of 12m baseline-ALMA antennas: NOT REQUIRED 7. Frequencies: 7.1. Receiver band: Band 7 7.2. Lines and Frequencies (GHz): Multi-line observations, 3 lines: 12CO(3-2) at 345.8 GHz HCN(4-3) at 354.5 GHz H13CN(4-3) at 345.3 GHz 12CO(3-2) and H13CN(4-3) can be observed in the LSB while HCN(4-3) can be observed in the USB (separation of 9.3 GHz). 7.3. Spectral resolution (km/s): 0.1 km/sec 7.4. Bandwidth or spectral coverage (km/s or GHz): 40 km/sec per line 8. Continuum flux density: 8.1. Typical value (Jy): 10 mJy 8.2. Required continuum rms (Jy or K): 0.03 mJy (to easily detect faint outer regions of disk/envleope) 8.3. Dynamic range within image: ~50-100 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 5% relative ( 1-3% / 5% / 10% / n/a ) 5% 9. Line intensity: 9.1. Typical value (K or Jy): ~0.8K-5 K (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): ~0.2 K (to detect low-level high-velocity gas) 9.3. Spectral dynamic range: < 50 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 5% relative ( 1-3% / 5% / 10% / n/a ) 5% 10. Polarization: NO 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 8 hr 12. Total integration time for program (hr): 80 hr 13. Comments on observing strategy : NONE -------------------------------------------------- Review v2.0: 2.2.12 - 2.2.15 I found no problems with these proposals other than the standard question of calculating ACA time. ===================================================================================== DRSP 2.2.15 Title The energetics and temperature structure of protostellar outflows Pi H. G. Arce Time 840 hrs DRSP 2.0 - section 2.2 proposal 1. Name of program and authors Name: The energetics and temperature structure of protostellar outflows Author: H. G. Arce, et al. 2. One short paragraph with science goal(s) Protostellar outflows interact with their gaseous surroundings, injecting momentum and energy into their parent molecular cloud. The interaction between the outflow and the cloud could play a crucial role in the chemical composition of the gas (e.g., Jorgensen et al. 2004), the turbulence of the cloud (e.g., Williams et al. 2003; Li & Nakamura 2006) and the cloud's velocity and density distribution (Arce & Goodman 2001;2002). Morphology and velocity structure are two relatively well-studied physical characteristics of molecular outflows. On the other hand, the energetics and temperature structure of outflows have been rarely studied. Further studies of outflow energetics are needed in order to fully understand the outflow phenomenon, its impact on the parent cloud, and the entrainment mechanism (e.g., Hatchell et al. 1999). We plan to observe all the 12CO and 13CO transitions accessible to ALMA in order to use line ratios to study the temperature distribution of the high-velocity outflow gas and to better understand how protostellar winds heat and impact their surroundings. We will obtain ~1'x2' mosaic maps of the area around four HH objects from the same protostellar source (RNO43), at an angular resolution similar to ground-based observations (~1"). For this, we will exploit ALMA's capability to map regions at different frequencies, with similar synthesized beams. The HH knots (i.e., bright optical/NIR emission from shocks arising from the interaction of the protostellar wind and the ambient gas) we plan to observe lie at different distances from the source and are interacting with drastically different ambient density gas. Temperature estimates using molecular line ratio heavily depend on the optical depth of the line, and thus it is essential we obtain 13CO measurements to estimate the 12CO line opacity. 3. Number of sources Four 1'x2' fields surrounding different HH knots from one giant protostellar jet. 4. Coordinates: 4.1. RA~5:30 Dec~12:50 4.2. Moving target: NO 4.3. Time critical: NO 4.4. Scheduling constraints: NO 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" (in order to compare with ground-based optical and NIR images, as well as Spitzer mid-IR images) 5.2. Range of spatial scales/FOV (arcsec): 60" x 120" 5.3. Required pointing accuracy: (arcsec) 0.6" (for accurate mosaic imaging at all bands) 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: Position switch on-the-fly mapping (can't do freq. switch, as low-level high velocity spectral wings are expected) 6.2. Stand-alone ACA: No 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: beneficial 6.4. Subarrays of 12m baseline-ALMA antennas: NO 7. Frequencies: 7.1. Receiver band: Band 3, 6, 7, 8, AND 9 7.2. Lines and Frequencies (GHz): *Band 3: Observe 12CO(1-0) at 115.3 GHz and 13CO(1-0) at 110.2 GHz using two different spectral setups *Band 6: Simultaneous observations of 12CO(2-1) at 230.5 GHz and 13CO(2-1) at 220.4 GHz *Band 7: Simultaneous observations of 12CO(3-2) at 345.8 GHz and 13CO(3-2) at 330.6 GHz *Band 8: Observe 12CO(4-3) at 461.0 GHz and 13CO(4-3) at 440.8 GHz using two different spectral setups *Band 9: Observe 12CO(6-5) at 691.5 GHz and 13CO(6-5) at 661.5 GHz using two different spectral setups 7.3. Spectral resolution (km/s): 0.3 km/sec 7.4. Bandwidth or spectral coverage (km/s or GHz): 200 km/sec per line 8. Continuum flux density: NOT A CONTINUUM PROJECT 8.1. Typical value (Jy): (take average value of set of objects) (optional: provide range of fluxes for set of objects) 8.2. Required continuum rms (Jy or K): 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 9. Line intensity: 9.1. Typical value (K or Jy): 0.6K to 10K 9.2. Required rms per channel (K or Jy): 0.2K 9.3. Spectral dynamic range: <20 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 1-3% repeatability ( 1-3% / 5% / 10% / n/a ) 1-3% relative ( 1-3% / 5% / 10% / n/a ) 1-3% (Very good absolute calibration for all bands is needed in order to obtain accurate line ratios. We will need good repeatability because the mosaics will be done over several passes and some of the larger mosaics will be made by combining smaller mosaics.) 10. Polarization: NO 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): Time estimated to obtain T_rms ~ 0.4 K per field. We plan to obtain Nyquist sampled mosaic, so T_rms ~0.2 K in final 1'x2' map. The following is for one 1'x2' mosaic (at the end we need to multiply by 4 to obtain total time for all planned fields) Band 3: We need a map at 115 GHz of 4x5 = 20 ptgs. time/ptg = 30min. total time = 10 hr Also, one map at 110GHz of 4X5 = 20 ptgs. time/ptg = 17min. total time = 5.7 hr Band 6: We need one map of 6x10 = 60 ptgs. time/ptg = 2min. total time = 2 hr Band 7: We need one map of 7x14 = 98 ptgs. time/ptg = 1min total time = 1.63 hr Band 8: We need one map at 461 GHz of 10x18 = 180 ptgs. time/ptg = 2.5min. total time = 7.5 hr Also, one map at 440.8 GHz of 10x18 = 180 ptgs. time/ptg. = 4 min. total time = 12 hr Band 9: We need one map at 691.5 GHz of 15x28 = 420 ptgs. time/ptg = 1.25min. total time = 8.75 hr Also, one map at 661.1 GHz of 15x28 = 420 ptgs. time/ptg. = 1 min. total time = 7 hr Total for one field at all frequencies = 10 + 5.7 + 2 + 1.63 + 7.5 + 12 + 8.75 + 7 ~ 54.6 ~ 55hr So, for all 4 regions, a total of 220hr. For ACA 7m array:We will need 4 times the integration of the 50 antenna ALMA array, to achieve same RMS. However, primary beam is 1.7 larger, so for mosaic we only need a factor of 1.4 more time with the ACA 7m array than the full ALMA array. That is, ~ 55 x 1.4 x 4 ~ 77 x 4 ~ 308hr ~310hr For total power: We will assume that we will get the ACA total power time at the same time as the ACA 7m data although in a separate sub-array. We will need to get a larger area than the synthesis maps to get out of the CO emission (so residual striping can be calibrated out in post-processing). The beam is smaller than the ACA 7m dishes and the mosaic region will be larger. It is not clear whether we will need the same integration time on source in total power as with the ACA. In this proposal, we assume we will not need as much time on source (it will be confusion limited?) so we assume the total integration time for the ACA (12m TP) to be the same as the ACA(7m array) = 310 hrs 12. Total integration time for program (hr): 220 (12m array) + 310 (ACA 7m array) + 310 (ACA TP) This does not include overhead for calibration and slew times (which will be significant for such large mosaics). 13. Comments on observing strategy : NONE -------------------------------------------------- Review v2.0: 2.2.12 - 2.2.15 I found no problems with these proposals other than the standard question of calculating ACA time. ===================================================================================== DRSP 2.2.16 Title Ionized Gas Accretion in Hypercompact HII Regions Pi S. Kurtz Time 6 hrs DRSP 2.0 - section 2.2 proposal 1. Name of program and authors Ionized Gas Accretion in Hypercompact HII Regions S. Kurtz 2. One short paragraph with science goal(s) Hypercompact HII regions have emerged as one of the earliest observable stages of a young massive star. On these very small scales (tens of milliparsec) the ionized gas is extremely dense, and radio recombination lines suffer substantial impact broadening and non-LTE effects. The dynamics of the ionized gas on these scales are not at all clear. Due to the high over-pressure within the HII region, outward, expansive flows might be expected. On the other hand, models for massive star formation suggest that ionized in-fall may be occurring, as the star continues to accrete matter from the parental cloud. It is probable that the stellar gravity maintains a steep density gradient within the ionized gas, further contributing to the complicated problem of separating radiative transfer effects from gas dynamics. Here, we propose to observe a sample of HC HII regions in several millimeter radio recombination line tracers, to map the gas flows within the region, and distinguish the contribution from non-LTE effects from that of actual gas dynamics. These observations will help to distinguish in a detailed way between several of the currently proposed mechanisms for massive star formation. 3. Number of sources Six presumed hypercompact HII regions 4. Coordinates: 4.1. Rough RA and DEC 6 "galactic plane" objects (18-19 hours RA, -20 to +15 Dec) 4.2. Moving target: yes/no (e.g. comet, planet, ...) no 4.3. Time critical: yes/no (e.g. SN, GRB, ...) no 4.4. Scheduling constraints: (optional) none 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.1 5.2. Range of spatial scales/FOV (arcsec): single field, LAS 1 arcsec 5.3. Required pointing accuracy: (arcsec) 10% of primary beam 6. Observational setup 6.1. Single dish total power data: no/beneficial/required no 6.2. Stand-alone ACA: no/beneficial/required no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no/beneficial/required no 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no no 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9 Band 4 7.2. Lines and Frequencies (GHz): H36a 135.286 H45b 135.249 He36a 135.341 7.3. Spectral resolution (km/s): 0.1 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 80 km/s 8. Continuum flux density: 8.1. Typical value (Jy): 1 Jy 8.2. Required continuum rms (Jy or K): 0.001 Jy 8.3. Dynamic range within image: 500:1 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 10% repeatability ( 1-3% / 5% / 10% / n/a ) 5% relative ( 1-3% / 5% / 10% / n/a ) 5% 9. Line intensity: 9.1. Typical value (K or Jy): 1 Jy 9.2. Required rms per channel (K or Jy): 0.004 Jy 9.3. Spectral dynamic range: 200:1 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 10% repeatability ( 1-3% / 5% / 10% / n/a ) 5% relative ( 1-3% / 5% / 10% / n/a ) 5% 10. Polarization: yes/no (optional) no 10.1. Required Stokes parameters: I 10.2. Total polarized flux density (Jy): n/a 10.3. Required polarization rms and/or dynamic range: n/a 10.4. Polarization fidelity: n/a 10.5. Required calibration accuracy: n/a 11. Integration time for each observing mode/receiver setting (hr): 1 hr 12. Total integration time for program (hr): 6 hr + calibration overhead 13. Comments on observing strategy : (optional) none -------------------------------------------------- ===================================================================================== DRSP 2.2.17 Project: The outflows in G5.89-0.39 PI: Klaassen Time: 8 hrs 2. One short paragraph with science goal(s) When the massive star forming region G5.89-0.39 is observed with a single dish (i.e. the JCMT), a large scale (diameter ~1pc, ~2') outflow predominantly in the E-W direction is observed (Klaassen et al. 2006). When it is observed with an interferometer (i.e. the SMA), other, much smaller outflows are observed predominantly in the NE-SW direction (Sollins et al. 2005, Hunter et al. 2008). A high resolution ALMA mosaic (with total power flux included) will show if/how these outflows are related to eachother. 3. Number of sources G5.89-0.39; which has already been observed in CO J=3-2 at the JCMT (15'' resolution) and SMA (3'' resolution) 4. Coordinates: 4.1. Rough RA and DEC RA 18 hr, DEC -24 deg 4.2. Moving target: no 4.3. Time critical: no 4.4. Scheduling constraints: None 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.2'' 5.2. Range of spatial scales/FOV (arcsec): 0.2'' - 2.5' these observations will require mosaicing, as well as total power observations (and ACA observations for middle scale structures) 5.3. Required pointing accuracy: 0.1'' 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: OTF mapping 6.2. Stand-alone ACA: required 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 7 7.2. Lines and Frequencies (GHz): CO & 13CO J=3-2, SiO J=8-7 (since they've already been observed with the JCMT and SMA) 7.3. Spectral resolution (km/s): 0.25 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): CO linewidths in this source can get up to 200 km/s 8. Continuum flux density: 8.1. Typical value (Jy): 2 8.2. Required continuum rms (Jy or K): 0.02 Jy 8.3. Dynamic range within image: 100 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 9. Line intensity: 9.1. Typical value (K or Jy): CO = 45 K (full power) 9.2. Required rms per channel (K or Jy): 0.5 K 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): each pointing will take 2.5 minutes. Since the ALMA beam at 345 GHz is 18'', the mosaic pointings will need to be spaced by 9''. To fully map the large scale outflow, this will require 170 pointings. At 2.5 min. per pointing, this project requires 7 hours of integration with 50 antennas (and much smaller integration times with the ACA and TP antennae). 12. Total integration time for program (hr): about 8 hours 13. Comments on observing strategy : (optional) ===================================================================================== DRSP 2.3.1 Title Chemical survey of hot cores and inner warm envelopes around YSOs Pi E. van Dishoeck Time 650 hrs 1. Name: Chemical survey of hot cores and inner warm envelopes around YSOs Authors: E. van Dishoeck, M. Wright, P. Schilke, F. Schoeier, ..... 2. Science goal: In recent years, it has become clear that the chemistry in the inner few hundred AU around deeply embedded (`class 0') YSOs is distinctly different from that of their outer colder envelopes. This chemistry is driven by sublimation of ices at temperatures around 90 K and subsequent high temperature chemical reactions between the evaporated species leading to complex organic species. These so-called `hot cores' have been detected both around low- and high-mass YSOs on the basis of single-dish unresolved data and their sizes have been determined from detailed modeling of continuum and multi-line data to be a few hundred AU (high-mass) (e.g., Wyrowski et al. 1999, ApJ 514, L43; van der Tak et al. 2000, ApJ 537, 283) to <100 AU (low-mass) (e.g. Ceccarelli et al. 2000, A&A 357, L9, Schoeier et al. 2002, A&A 390, 1001). ALMA can resolve these hot core regions and map the distribution of the molecules. These data can be used to test models of thermal evaporation vs. liberation of icy mantles in shocks, models of hot core chemistry (e.g., spatial separation of oxygen- and nitrogen-bearing species) and dynamical effects (are these complex molecules infalling or outflowing?). Chemical signatures of disks in the embedded stage can also be investigated. Multiline/multiband observations are needed to separate excitation effects from abundance effects. The source list should be coordinated with that of HIFI so that complementary information on H2O is also obtained. Band 5 will cover the H218O 204 GHz line, Band 8 the HDO 464 GHz line. Water is a crucial species in the chemistry. 3. Number of sources: 50 (20 high mass; 10 intermediate mass; 20 low-mass) 4. Coordinates: 4.1. 7 sources in Oph (RA=16:30, DEC=-24) 7 sources in Perseus (RA=03, DEC=+30) 7 sources in Taurus (RA=04, DEC=+20) 7 sources in Orion/Monoceros (RA=05-06, DEC=-05) 22 sources distributed over sky (RA=any, DEC=<+20) 4.2. Moving target: no 4.3. Time critical: no 4.4. Scheduling constraints: no 5. Spatial scales: 5.1. Angular resolution: 0.20"-0.25" 5.2. Range of spatial scales/FOV: 3"x3" 5.3. Required pointing accuracy: <1" (cf. specifications) 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: nutator switch 6.2. Stand-alone ACA: beneficial/required (would be required if same data are also used to study outer envelope) 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3 Band 4 Band 5 Band 6 Band 7 Band 8 Band 9 7.2. Line: 1 1 1 3 4 1 2 settings 7.3. Spectral resolution (km/s): ~0.25 km/s (may be binned for weaker/broad lines) 7.4. Spectral coverage (km/s or GHz): maximum at spectral resolution with both polarizations (1 GHz Band 6-7; 2 GHz Band 9) 8. Continuum flux density: Band 3 Band 6 Band 7 Band 9 8.1. Typical value: 0.02-0.2 0.2-2 0.3-8 1-60 Jy low-mass 0.2-2 2-20 6-100 30-600 Jy high-mass 8.2. Continuum peak value: 0.2-2 2-20 8-100 60-600 (interpolate for Bands 3, 4, 5 and 8) 8.3. Required continuum rms: 0.1 Jy (not relevant for this program) 8.4. Dynamic range in image: >100 9. Line intensity: 9.1. Typical value: 2-150 K (low-mass) 3-500 K (high-mass) 9.2. Required rms per channel: 1 K 9.3. Spectral dynamic range: 3 (for species which are barely detected) >100 (for brightest lines) 9.4. Calibration requirements: absolute 10% repeatability 5% relative 5% See earlier response for motivation 10. Polarization: no 10.1. Required Stokes parameters: N/A 10.2. Total polarized flux density (Jy): N/A 10.3. Required polarization rms and/or dynamic range: N/A 10.4. Polarization fidelity: N/A 10.5. Required calibration accuracy: N/A 11. Integration time per setting: typically 1 hr per setting (for all bands, binning to lower spectral/spatial resolution for weakest lines) 12. Total integration time for program: 50 x 1 x 1 = 50 hr Band 3 50 x 1 x 1 = 50 hr Band 4 50 x 1 x 1 = 50 hr Band 5 50 x 3 x 1 = 150 hr Band 6 50 x 4 x 1 = 200 hr Band 7 50 x 1 x 1 = 50 hr Band 8 50 x 2 x 1 = 100 hr Band 9 650 hr Total *********************************************************************** Review Lee Mundy: OK. ===================================================================================== DRSP 2.3.2 Title Chemical fractionation in Low-mass Cores Pi Y. Aikawa Time 358 hrs 1. Name of program and authors Name: Chemical fractionation in Low-mass Cores Authors: Y. Aikawa, K. Tatematsu 2. One short paragraph with science goal(s) From recent observational studies, it became clear that the molecular abundances have local spatial variation within molecular cloud cores. In the central region of some prestellar cores C-bearing species (e.g. CO) are depleted, while molecular D/H ratio is significantly enhanced and depletion of N-bearing species are rare. Such fractionation is mainly caused by molecular depletion onto grains and subsequent gas-phase reactions. Detailed observation of the chemical fractionation reveals not only the gas-dust chemical interaction, but also helps us to understand the formation process of dense cores and their evolution, because spatial abundance variation is determined by a balance between physical and chemical timescales. Molecules to be observed are CO, N2H+, H2D+, etc. Our source list includes very young prestellar cores with little depletion, prestellar cores with significant depletion, and very young protostellar cores, which are not yet warm enough to start the hot-core type chemistry. We need imaging of the dust continuum emission for reference. We will observe two frequencies to disentangle the column density distribution and the dust temperature distribution. 3. Number of sources: 3 starless cores and 3 protostellar cores 4. Coordinates: 4.1. Rough RA and DEC 6 sources either in Lupus (RA=15, DEC=-40) or in Chamaeleon (RA=10:30, DEC=-78) or in Oph (RA=16:30, DEC=-24) or in Taurus (RA=04, DEC=+20)) 4.2. Moving target: no 4.3. Time critical: no 4.4. Scheduling constraints: (optional) 5. Spatial scales: 1. Angular resolution (arcsec): 2'' (For continuum, 5.we do not need 2" for comparison, but it would be better to observe 5.continuum at the same time slot, which means the same array 5.configuration. Otherwise, we must wait for array 5.re-configuration...) 5.2. Range of spatial scales/FOV (arcsec): 0.5'-2' Band 3: 2' - 9 field mosaic of FOV=50" Band 4: 2' - 25 field mosaic of FOV=33'' Band 6: 2' - 36 field mosaic of FOV=20'' Band 7: 0.5' - 5 field mosaic of FOV=17'' Band 9: 0.5' - 25 field mosaic of FOV=8'' 5.3. Required pointing accuracy: 0.1'' 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: position switch 6.2. Stand-alone ACA: required 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: beneficial 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9: 3, 4, 7, 9 (Band 6 for continuum ?) 7.2. Lines and Frequencies (GHz): Band 3 (3LO settings) (1) H13CO+ (1-0): 87GHz (2) N2H+ (1-0): 93GHz, C34S (2-1): 96GHz (3) C18O (1-0): 110GHz, C17O(1-0): 112GHz Band 4 (2LO settings): (1) DCO+ (2-1): 144GHz, DCN: 145GHz, C34S 2-1: 145GHz, CS(3-2): 147GHz (2) N2D+ (2-1): 154GHz Band 7 (1LO setting) (1) H2D+: 372GHz Band 9 (1LO setting) (1) HD2+: 692GHz 7.3. Spectral resolution (km/s): 0.2 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 5km/s 8. Continuum flux density: 8.1. Typical value (Jy): 20-400 mJ/beam at B6, 0.5-10J/beam at B9 8.2. Required continuum rms (Jy or K): 4 mJ/beam at B6, 28mJ/beam at B9 8.3. Dynamic range within image: 100 8.4. Calibration requirements: absolute 10% repeatability 5% relative 5% 9. Line intensity: 9.1. Typical value (K or Jy): 0.5-5 K 9.2. Required rms per channel (K or Jy): 0.07 K 9.3. Spectral dynamic range: 7-70 9.4. Calibration requirements: absolute 10% repeatability 5% relative 5% 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 6 sources x 9-field mosaic x 3 LO setting x 25 min =67.5 hrs (B3 line) 6 sources x 25-field mosaic x 2 LO setting x 15 min =75 hrs (B4 line) 3 sources x 5-field mosaic x 1LO setting x 120min =30 hrs (B7 line) 3 sources x 25-field mosaic x 1LOsetting x 120min=150 hrs (B9 line) 6 sources x 36-field mosaic x 1 min =3.6 hrs (B6 continuum) 6 sources x 320-field mosaic x 1 min = 32 hrs (B9 continuum) 12. Total integration time for program (hr): 358 hrs 13. Comments on observing strategy : (optional) We assume mosaic with 1-min imaging for continuum (The time will be reduced if OTF systhesis is available in 2012). OTF synthesis is preferable, because it will improve UV coverage drastically and it will save observing time largely. ===================================================================================== DRSP 2.3.3 Title Chemical differentiation in star-forming regions Pi M. Wright Time 134 hrs Name: Chemical differentiation in star-forming regions ================================================= Authors: M. Wright, E. van Dishoeck, K. Tatematsu, R. Plume, P. Schilke, ... 2. Science goal: The abundances of various molecules respond differently to the processes associated with star formation. Very close to the protostars, abundances of certain species may be enhanced due to evaporation of grain mantles (e.g., CH3OH, H2CO) or high-temperature chemistry (e.g.,complex organics, HCN), whereas further out in the envelope, many molecules will be frozen out on the grains. On larger scales, the outflows interact with the envelope and general molecular cloud material, sputtering grain cores (leading to SiO) and releasing mantle material. Some of the released material can react further with other gas-phase molecules producing new species (e.g., HCO+). Although some of these chemical variations have been recognized from single-dish data and lower-resolution interferometry, no systematic "chemical images" in various species have been made at arcsec resolution characterizing the cores, knots, outflows, filaments and other small scale structure in these regions. We propose here to map 3 star-forming regions over a ~100"x100" scale in several species. Multi-line observations are needed to distinguish excitation from abundance variations. This DRSP complements DRSP 2.3.1 (which is limited to a single pointing on hot cores) and DRSP 2.3.2 (which is focussed on imaging cold clouds prior to star formation). It could incorporate the DRSP submitted by Rene Plume to map HCO+ in outflow regions, although at somewhat lower spatial resolution and fewer sources. 3. Number of sources: 3 4. Coordinates: 4.1. Coordinates: well-known star-forming regions visible by ALMA 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 1" 5.2. Range of spatial scales/FOV: 100"x100" 16 point mosaic at B3 64 point mosaic at B6 ~100 point mosaic at B7 selected regions at B9 (assume 50 pointings) 5.3. Single dish: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 Band 6 Band 7 Band 9 6.2. Line: 2 settings 3 settings 2 settings 1 setting 6.3. Spectral resolution (km/s): ~0.25 km/s (but typically smoothed to 0.5-1 km/s to get better S/N) 6.4. Spectral coverage (km/s or GHz): maximum at spectral resolution with full polarization (1 GHz Band 6-7; 2 GHz Band 9) 7. Continuum flux density: Band 3 Band 6 Band 7 Band 9 7.1. Typical value: 2-200 10-1000 20-8000 100-10000 mJy/beam 7.2. Continuum peak value: 200 1000 10000 10000 7.3. Required continuum rms: 1 mJy/beam (not relevant for this program) 7.4. Dynamic range in image: >100 8. Line intensity: 8.1. Typical value: 2-500 K 8.2. Required rms per channel: 0.15 K at B3 => 30 min per point at 0.5 km/s 0.1 K at B6 => 5 min per point at 0.5 km/s 0.1 K at B7 => 3 min per point at 0.5 km/s 0.15 K at B9 => 3 min per point at 0.5 km/s 8.3. Spectral dynamic range: 3 (for species which are barely detected) >100 (for brightest lines) 9. Polarization: no 10. Integration time per setting: 11. Total integration time for program: 16 pointings x 3 sources x 2 settings x 30 min = 48 hr at B3 64 pointings x 3 sources x 3 settings x 5 min = 48 hr at B6 100 pointings x 3 sources x 2 settings x 3 min = 30 hr at B7 50 pointings x 3 sources x 1 setting x 3 min = 8 hr at B9 Total time: 134 hr **************************************************************************** Review Lee Mundy: OK. -------------------------------------------------- Review v2.0: ok ===================================================================================== DRSP 2.3.4 Title Unbiased line surveys of high mass star forming regions Pi P. Schilke Time 612 hrs 1. Name: Unbiased line surveys of high mass star forming regions Authors: P. Schilke, E. van Dishoeck, M. Wright, C. Comito, F. Wyrowski ... 2. Science goal: Unbiased line surveys are the only way to get an unbiased view on the chemical composition of sources, which allows, provided the modeling is understood, to reconstruct the evolution history of high mass star forming regions. Since many such regions show pronounced spatial variations of the molecular distribution and excitation conditions, it is necessary to spatially resolve them. This also aids in the finding of new lines and molecules, because it reduces the confusion. In the best studied source so far, Orion-KL, the source intrinsic confusion limit is in the order of 1~K, so that integration down to this level, but not much further down, seems advised. Spanning the survey over the whole frequency range of ALMA allows to cover a large range of excitation conditions for most observed molecules, which is a prerogative for detailed modeling of the temperature, density and FIR field. For high column density sources it seems likely that the dust becomes optically thick at the highest frequencies, which will cause some lines to show up in absorption. This, while it complicates interpretation, permits a modeling of the exitation conditions along the line of sight. The source list should be coordinated with that of HIFI so that complementary information on higher frequencies is also obtained. 3. Number of sources: 10 4. Coordinates: 4.1. 1 source in Orion (RA=05, DEC=-05) 9 sources in Galactic Plane (RA=15, DEC=-54 to RA=19, DEC=15) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.6" for Band 3, 0.3" for Bands 6, 7 and 9 5.2. Range of spatial scales/FOV: 3"x3" 5.3. Single dish: yes, for some sources 5.4. ACA: yes (particularly at higher frequencies) 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 Band 6 Band 7 Band 9 6.2. Line: 60 64 95 69 settings 6.3. Spectral resolution (km/s): 0.5 km/s 6.4. Spectral coverage (km/s or GHz): 500 MHz at Band 3, 1 GHz at Bands 6, 7, 2GHz at Band 9 7. Continuum flux density: Band 3 Band 6 Band 7 Band 9 7.1. Typical value: 2-20 2-20 6-100 30-600 Jy (high-mass) 7.2. Continuum peak value: 50 mJy/beam 200 mJy/beam 300 mJy/beam 1 Jy/beam 7.3. Required continuum rms: 0.1 Jy (not relevant for this program) 7.4. Dynamic range in image: >100 8. Line intensity: 8.1. Typical value: 5-500 K 8.2. Required rms per channel: 1 K 8.3. Spectral dynamic range: 3 (for species which are barely detected) >100 (for brightest lines) 9. Polarization: no 10. Integration time per setting: 10 min/Bd 3, 15 min/Bd 6,7, 10 min/Bd 9 11. Total integration time for program: 10 x 60 x 10m : 100 h Band 3 10 x 64 x 15m: 160 h Band 6 10 x 95 x 15m: 237 h Band 7 10 x 69 x 10m: 115 h Band 9 ------------------------------------------- 612 h total Comments: 1) Increasing the spatial resolution for Band 3 to match the others will result in a vast increase of observing time. 2) There are no overheads calculated here. Since the individual settings are only 10-15 min on source, these could be significant, according to Memo 375 in the order 50-100%, depending on frequency. Since some of these overheads apply only once per frequency setting (sideband ratio, bandpass, flux), the best strategy may be to tune to a frequency, observe all the sources, and then retune. Some of the overheads on the other hand apply per source (pointing, phase calibration), so if these dominate the best strategy may be to stay on a source and tune through. 3) Depending on the exact characteristics of the corrlator filters, one would want to decrease the spacing to get some overlap at the edges, increasing the number of correlator settings. This would particularly be the case if the upgraded correlator is used, since there is a lot of aliasing. 4) The correlator upgrade would be very beneficial for this project, but see 3) above. 5) We note that in the current ALMA software there is NO provision to get SSB spectra from single dish observations at least in Band 9, although a deconvolution (as will be done for HIFI) will be possible, using the sideband gain ratios determined in interferometer mode, as noted by Mel Wright. 6) One would want to get even high spatial resolution for selected parts of the survey. **************************************************************************** Review Lee Mundy: OK. -------------------------------------------------- Review v2.0: ok ===================================================================================== DRSP 2.3.5 Title Low Frequency Spectral Survey aimed at Complex Organics Pi B. E. Turner Time 35 hrs 1. Name of program and authors Low Frequency Spectral Survey aimed at Complex Organics ======================================================== B. E. Turner 2. One short paragraph with science goal(s) The NRAO spectral line survey covers ~40 GHz in the 2mm band; 17,000 spectral lines are observed in seven sources. Frequency resolution is 0.78 MHz; sensitivity is generally 4 mK. Line emission covering factors reach 0.52 for SgrB2N and 0.24 for Ori(KL). The confusion limit is reached in this survey. Traditional methods of line identification, based on specific search and identification of ~5 lines is unjustified in the face of such confusion. Algorithms based on binomial statistical analysis have been applied to asses the probability that an apparent identification is not just due to chance. Species 'identified' in the interstellar medium are shown to have chances of misidentification of ~10% (e.g. glycol aldehyde; ethylene glycol) while 75 other candidates have probabilities ~<0.001. Many of these candidates are quite complex and suggest active involvement of grain surfaces in interstellar chemistry. A sensitive ALMA survey is proposed; the results will be used to 1) complement the current survey, increasing the confidence in statistical identification of the complex molecules selected by the 2mm survey. 2) Study the images produced to determine whether statistically identified lines arise from colocated regions. 3) Explore the astrochemistry of sources beyond the reach of northern hemisphere observatories. 3. Number of sources: 7 4. Coordinates: 4.1. Rough RA and DEC 2 sources in Sgr, 2 sources in Orion, 1 source in Leo, 1 source in Aquila, NGC6334. 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution (arcsec): 1.0" 5.2. Range of spatial scales/FOV (arcsec): Single field 1"/60" 5.3. Single dish total power data: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 6.2. Lines and Frequencies (GHz):Band scan, 86 GHz - 116 GHz requires 30 settings per source. 6.3. Spectral resolution (km/s): 0.32 6.4. Bandwidth or spectral coverage (km/s or GHz):30 GHz 7. Continuum flux density: 7.1. Typical value (Jy): ~2 7.2. Required continuum rms (Jy or K): N/A 7.3. Dynamic range within image: ~100 8. Line intensity: 8.1. Typical value (K or Jy): 1.7 K 8.2. Required rms per channel (K or Jy): 0.5 K 8.3. Spectral dynamic range: >5 weak lines >1000 strong lines 9. Polarization: no 9.1. Required Stokes 9.2. Total polarized flux density (Jy) 9.3. Required polarization rms and/or dynamic range 9.4. Polarization fidelity 10. Integration time for each observing mode/receiver setting (hr): 10 min. 11. Total integration time for program (hr): 7x30x10 min = 35 hr 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): line survey This program could be executed more quickly with the availability of the polyphase filter, by a factor of four. These heavy molecules emit at lower frequencies; Bands 1, 2 and 4 would be valuable complements to this survey when available. ************************************************************************ Review Lee Mundy: OK. -------------------------------------------------- Review v2.0: ok ===================================================================================== DRSP 2.3.6 Title Surveys of interstellar HCO+ absorption Pi R. Lucas Time 80 hrs 1. Name of program and authors Surveys of interstellar HCO+ absorption R. Lucas, H. Liszt 2. One short paragraph with science goal(s) Absorption measurement in front of background sources is the preferred method to detect unexcited interstellar molecules. Low density environments (diffuse and translucent clouds) are sites of a remarkable complex chemistry, despite their unprotected exposition to photodissociating radiation from stars. Relative abundances of the molecules are grossly similar to those of dark clouds, but with several notable differences. Moreover the small observed scatter in some of the abundance ratios clearly indicates that these low density regions are a choice laboratory for the study of the basic physical and chemical processes of the interstellar medium. We propose to do a systematic survey of the typically 900 point sources of flux larger than 0.2 Jy visible from Chajnantor. The available frequency coverage is 250 MHz if we use the highest velocity resolution (0.18 km/s). Alternately we may consider using only 0.37 km/s resolution and survey also the C2H molecule. This survey will provide a unique data base on diffuse/translucent molecular clouds, of importance comparable or larger than all existing optical interstellar absorption data. 3. Number of sources (e.g., 1 deep field of 4'x4', 50 YSO's, 300 T Tauri stars with disks, ...; do NOT list individual sources or your "pet object", except in special cases like LMC, Cen A, HDFS) 5 sources of About 900 sources with flux greater than 200 mJy 4. Coordinates: 4.1. Rough RA and DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 30 in Lupus) Sources are everywhere. Indicate if there is significant clustering in a particular RA/DEC range (e.g. if objects in one particular RA range take 90% of the time) NO 4.2. Moving target: yes/no (e.g. comet, planet, ...) NO 4.3. Time critical: yes/no (e.g. SN, GRB, ...) NO 5. Spatial scales: 5.1. Angular resolution (arcsec): These are point sources. The angular resolution does not really matter. 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) These are point sources. 5.3. Single dish total power data: yes/no NO 5.4. ACA: yes/no NO 5.5. Subarrays: yes/no NO 6. Frequencies: 6.1. Receiver band: Band 3, 6, 7, or 9 Band 3 6.2. Lines and Frequencies (GHz): (approximate; do NOT go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify e.g. "6 frequency settings in Band 3". Apply redshift correction yourself) HCO+ (1-0) 89.19 GHz C2H (1-0) 87.28 GHz 6.3. Spectral resolution (km/s): 0.5 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 250 MHz = 840 km/s is more than we really need. 7. Continuum flux density: 7.1. Typical value (Jy): (take average value of set of objects) (optional: provide range of fluxes for set of objects) Minimum 0.2 Jy, average around 0.3 Jy 7.2. Required continuum rms (Jy or K): .04 mJy is expected but not required. 7.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether e.g. weak objects next to bright objects) 100, but no imaging is needed. 8. Line intensity: 8.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) typical 0.02 Jy (10% absorption). 8.2. Required rms per channel (K or Jy): 1% of flux density (.002 Jy for weakest sources) 8.3. Spectral dynamic range: 100 9. Polarization: yes/no (optional) no 9.1. Required Stokes total intensity only 9.2. Total polarized flux density (Jy) N/A 9.3. Required polarization rms and/or dynamic range N/A 9.4. Polarization fidelity N/A 10. Integration time for each observing mode/receiver setting (hr): total time 80 hr (600 s for 0.2Jy sources, 100s for 0.5Jy sources, 24s for 1Jy sources) 11. Total integration time for program (hr): total time 80 hr 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) This is a survey. The observations are essentially self calibrated, so there is NO requirement on phase stability. The data are usable provided that the pointing accuracy is better than, say, 5" and the 3mm optical depth smaller than 0.5. This means the stringency is probably very low (close to 1). The sensitivity calculation is based on detecting features with typical line widths of 1.0 km/s. Higher velocity resolution is actually available and used to detect structure in stronger lines. ********************************************************************* Review Lee Mundy: OK. -------------------------------------------------- Review v2.0: ok ===================================================================================== DRSP 2.3.7 Title Surveys of interstellar molecular absorption Pi R. Lucas Time 57 hrs 1. Name of program and authors Surveys of interstellar molecular absorption R. Lucas, H. Liszt 2. One short paragraph with science goal(s) Absorption measurement in front of background sources is the preferred method to detect unexcited interstellar molecules. Low density environments (diffuse and translucent clouds) are sites of a remarkable complex chemistry, despite their unprotected exposition to photodissociating radiation from stars. Relative abundances of the molecules are grossly similar to those of dark clouds, but with several notable differences. Moreover the small observed scatter in some of the abundance ratios clearly indicates that these low density regions are a choice laboratory for the study of the basic physical and chemical processes of the interstellar medium. We propose to do a systematic frequency survey of band 3 for a few (~ 3) sources, selected for high molecular content (estimated from HCO+ column density and/or visual extinction). Each source requires 64 settings to cover all band 3. 3. Number of sources (e.g., 1 deep field of 4'x4', 50 YSO's, 300 T Tauri stars with disks, ...; do NOT list individual sources or your "pet object", except in special cases like LMC, Cen A, HDFS) About 3 sources with flux in range 0.3-2 Jy. 4. Coordinates: 4.1. Rough RA and DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 30 in Lupus) Sources coordinates are not known at this time. Indicate if there is significant clustering in a particular RA/DEC range (e.g. if objects in one particular RA range take 90% of the time) Sources are in galactic plane. 4.2. Moving target: yes/no (e.g. comet, planet, ...) NO 4.3. Time critical: yes/no (e.g. SN, GRB, ...) NO 5. Spatial scales: 5.1. Angular resolution (arcsec): These are point sources. The angular resolution does not really matter. 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) These are point sources. 5.3. Single dish total power data: yes/no NO 5.4. ACA: yes/no NO 5.5. Subarrays: yes/no NO 6. Frequencies: 6.1. Receiver band: Band 3, 6, 7, or 9 Band 3 6.2. Lines and Frequencies (GHz): (approximate; do NOT go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify e.g. "6 frequency settings in Band 3". Apply redshift correction yourself) 32 settings in band 3, spaced by 1.0 GHz. 6.3. Spectral resolution (km/s): 0.5 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 1.0 GHz 7. Continuum flux density: 7.1. Typical value (Jy): (take average value of set of objects) (optional: provide range of fluxes for set of objects) Minimum 0.3 Jy 7.2. Required continuum rms (Jy or K): .04 mJy is expected but not required. 7.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether e.g. weak objects next to bright objects) 100, but no imaging is needed. 8. Line intensity: 8.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) typical 0.03 Jy (10% absorption). 8.2. Required rms per channel (K or Jy): 1% of flux density (.003 Jy for weakest sources) 8.3. Spectral dynamic range: 100 9. Polarization: yes/no (optional) no 9.1. Required Stokes total intensity only 9.2. Total polarized flux density (Jy) N/A 9.3. Required polarization rms and/or dynamic range N/A 9.4. Polarization fidelity N/A 10. Integration time for each observing mode/receiver setting (hr): time 19.2 hr per source (0.6 hr per setting) assuming a 0.3Jy source flux 11. Total integration time for program (hr): total time 57 hr 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) This is a line survey. The observations are essentially self calibrated, so there is NO requirement on phase stability. The data are usable provided that the pointing accuracy is better than, say, 5" and the 3mm optical depth smaller than 0.5. This means the stringency is probably very low (close to 1). ************************************************************************ Review Lee Mundy: OK. -------------------------------------------------- Review v2.0: ok ===================================================================================== DRSP 2.3.8 Title Chemical Enhancements in Outflows Pi R. Plume Time 16 hrs 1. Name: Chemical Enhancements in Outflows Authors: R. Plume, ... 2. Science Goal: To determine the location and mechanism by which the enhancement of HCO+ occurs in molecular outflows. Rawlings et al. (2000, MNRAS, 313, 461) have suggested that the HCO+ enhancement occurs continuously along the outflow in a turbulent mixing layer. This model is supported by OVRO observations of HCO+ 1-0 in L1527 by Hogerheijde et al. (1998, ApJ, 502, 315) which shows an "X-shaped" distribution of HCO+ emission. However, the OVRO resolution was too poor to confirm this model prediction in the other sources observed by Hogerheijde et al. Given the compact nature of these sources, it is also possible that the HCO+ enhancement occurs at the base of the jet and then gets carried downstream. We would like to examine the HCO+ 3-2 emission from L1527, to better resolve the X-shaped structure first seen by Hogerheijde et al in HCO+ 1-0, as well as from L1489, L1551, and L1535 to determine the location of the HCO+ emission. Previous single-dish observations show that the HCO+ 3-2 lines are a few K in strength and a few km/s wide. This project should also be extended to outflows from high-mass protostellar objects (e.g. G5.89) in order to determine if there are quantitative differences between the HCO+ enhancement mechanisms in high and low mass YSOs. 3. Number of sources: 8 4. Coordinates: 4.1. L1527, L1489, L1551, L1535 (RA ~ 04h 30m, DEC ~ 18-23 degrees) G5.89-0.39 (aka W28A2) (RA ~ 17h 57m, DEC ~ -24 degrees) 3 other high-mass outflows (RA = any, DEC = any) 4.2. Moving Target: no 4.3. Time critical: no 5. Spatial Scales: 5.1. Angular Resolution: 0.5" 5.2. Range of Spatial Scales/FOV: 20" 5.3. Single Dish: yes 5.4. ACA: yes 5.5. subarrays: no 6. Frequencies 6.1. receiver band: 6 6.2. Line: HCO+ 3-2 Frequency: 267 GHz 6.3. Spectral resolution: 0.2 km/s 6.4. Spectral Coverage: 60 km/s 7. Continuum Flux Density: 7.1. Typical value: 7.2. Continuum peak value: 7.3. Required continuum rms: 7.4. Dynamic Range in image: 8. Line Intensity: 8.1. Typical value: 2-8 K 8.2. Required rms per channel: 0.2 K 8.3. Spectral Dynamic Range: 10 9. Polarization: no 10. Integration time per setting: 2 hours x 8 sources 11. Total Integration time for program: 16 hrs *********************************************************************** Review Lee Mundy: OK.-------------------------------------------------- Review v2.0: ok ===================================================================================== DRSP 2.3.9 Title Tracing the photoprocesses shaping the Horsehead nebula Pi J. Pety Time 103 hrs ************************************************************************* 1. Name of program and authors Program: Tracing the photoprocesses shaping the Horsehead nebula Authors: J.Pety, M.Gerin and J.R.Goicoechea 2. One short paragraph with science goal(s) The Horsehead nebula is a fantastic laboratory of physics and chemistry. It is a typical pillar shaped by the photoevaporation of low density material which was protected by the shadow of denser material (Pound et al. 2003). This is the first pillar where rigid rotation of gas around its axis has been demonstrated (Hily-Blant et al. 2005). The horsehead contains two dense cores surrounded by a lower density halo (Ward-Thompson et al. 2006; Philipp et al. 2006). But its stunning particularity is the relatively simple geometry of the illuminated cloud edge: Abergel et al. 2003 and Habart et al. 2005 demonstrated that the PDR at the edge of the west condensation can be accurately modeled as a 1D PDR-structure, seen almost edge-on. For that reason, several observational studies at medium resolution (5") have been triggered with the Plateau de Bure Interferometer (PdBI) (e.g. Pety et al. 2005 and Goicoechea et al. 2006), the idea being to use this source as a reference for PDR chemical models. It is proposed here to map the top of the Horsehead (whose shape gave birth to its name) in the different 13CO lines observable with the ALMA receivers as well as the CI lines. This program would enable 1) to study the dynamics of photoevaporation of the dense material at the pillar top, 2) to precisely determine the thermal profile (by having access to diagnostics of the warm gas), 3) to observe the transition between atomic carbon and carbon monoxide. Note that complementary C+ observations towards the Horsehead will be done within the framework of the HIFI/Herschel guaranteed-time key-programs. Current state-of-the-art PDR models show that the typical spatial scale of the physical and chemical gradients range from 1" to 50", making this source an excellent target for ALMA. The choice of the 13CO isotopologue enable to minimize optical depth effects (as probed by PdBI 12CO observations) while still observing bright lines. C18O and continuum would also be observed in the same tunings. The Horsehead nebula is one of the most famous object of the sky. We thus propose to incorporate the nose and the mane in the maps as the obtained maps would thus be an excellent advertisement of the ALMA capabilities in the wide-field mapping area. 3. Number of sources The top of the Horsehead, i.e. a region of 150"x300". 4. Coordinates: 4.1. Rough RA and DEC Ra 2000: 05:40:54 Dec 2000: -02:28:00 4.2. Moving target: No 4.3. Time critical: No 4.4. Scheduling constraints: Avoid windy periods to ensure high precision mosaicing. 5. Spatial scales: 5.1. Angular resolution (arcsec): 1" 5.2. Range of spatial scales/FOV (arcsec): 150"x300" We propose to make Nyquist sampled mosaics following an hexagonal compact pattern. This implies: 49 pointings at 110 GHz (Band 3) 195 pointings at 220 GHz (Band 6) 507 pointings at 330 GHz (Band 7) 869 pointings at 440 GHz (Band 8) 1193 pointings at 492 GHz (Band 8) 2165 pointings at 661 GHz (Band 9) In view of the total number of fields, it is clear that such a program would benefit from the On-The-Fly interferometric mode that IRAM will try to prototype for ALMA in the coming three years. 5.3. Required pointing accuracy: (arcsec) 0.6" rms to ensure high precission mosaicing. 6. Observational setup 6.1. Single dish total power data: Required Observing modes for single dish total power: * On-The-Fly is required by the field of view. * The narrow zero-power linewidth (3 km/s) makes frequency switch suitable to this project, which will improve single dish signal-to-noise ratio by sqrt(2). 6.2. Stand-alone ACA: Required 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: This question is difficult to answer. We do not know of any public studies that shows that cross-correlation between ACA and ALMA would be beneficial. Several points need to be clarified: 1) Does the collecting surface of ACA is enough to ensure alone (i.e. without a correction for the integrating time) good sensitivity at spatial frequencies around 7m relatively to the sensitivity at frequencies measured by ALMA alone? 2) Cross correlating 2 different interferometers implies a multiplication of the respective primary beams in the measurement equation: Does this implies in practice a limitation of the field of view of the small antennas to the field of view of the large antennas? 6.4. Subarrays of 12m baseline-ALMA antennas: No 7. Frequencies: 7.1. Receiver band: Band 3, 6, 7, 8, 9 7.2. Lines and Frequencies (GHz): Band 3: 110 GHz. Band 6: 220 GHz. Band 7: 330 GHz. Band 8: 440 and 492 GHz. Band 9: 661 GHz. 7.3. Spectral resolution (km/s): 0.2 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 3 km/s for lines but this implies a much larger bandwidth for the single dish frequency switched observations. 8. Continuum flux density: 9. Line intensity: 9.1. Typical value (K or Jy): 0.5 K in all bands giving a peak signal-to-noise ratio of at least 20. 9.2. Required rms per channel (K or Jy): 9.3. Spectral dynamic range: Between 20 and 100 (Equal to the peak signal-to-noise ratio as we are trying to resolve the PDR edge). 9.4. Calibration requirements: Absolute: 5% The main goal of this project is a quantitative comparison of observations with PDR model predictions. We thus need as high as possible absolute precision. But making a large mosaic that associates ALMA, ACA and Single-Dish measurements is increasing the complexity of the calibration. We will thus pragmatically take what we will get but having a 5% absolute precision would be a tremenduous progress compared to today. We assume that a given absolute precision implies the same level of repeatability and relative precision. 10. Polarization: No 11. Integration time for each observing mode/receiver setting (hr): Due to Nyquist sampling of the mosaics, the pointings are not independent. The standard sensitivity formula to use in such a case implies to divide the number of pointings by 1.7. Using the ALMA time estimator, this gives: 7.5 hrs at 110 GHz (band 3). 3.8 hrs at 220 GHz (band 6). 10.0 hrs at 330 GHz (band 7). 27.0 hrs at 440 GHz (band 8). 33.7 hrs at 492 GHz (band 8). 21.2 hrs at 661 GHz (Band 9). 12. Total integration time for program (hr): 103 hrs. 13. Comments on observing strategy: We need an homogeneous data set to make precise comparisons with models. We thus propose to observe exactly the same field of view at the same resolution in all lines. The proposed resolution (1") ensures to use only the compact configuration at the highest frequency while it needs moderately extended configuration at the lowest frequency (largest baseline: 550 m). *************************************************************************** -------------------------------------------------- Review v2.0: DRSP (2.3.9): "Tracing the photoprocesses shaping the Horsehead nebula", and I have a following minor comment. This is an interesting program as a whole, but I cannot understand whether the resolution of 1" is necessary for all the species. The abundance gradient is different from molecule to molecule, and hence, only the total power map may be enough for some species. R.: ne of the goal of this project is to test the transition between CI and CO in the PDR. As shown in the figures of the contribution we wrote for the ALMA conference (attached at end of this email), the data from single-dish instruments and from Plateau de Bure of several of the species proposed in this DRSP is already available. It is clear that the single-dish resolution is not large enough to reach the above goal. Indeed, we know from emission map of 2.12 micron H2 line that the PDR profile is structured at scales up to at least 1". And PDR models predict a transition from C+/CI/12CO in a few arcsec. This is why our goal is a resolution of 1". We propose this resolution in all the observed species because this is the best way to ensure that we will not have to make any assumptions of the beam filling factor when modelling the different intensity brightness. Also it is important to accurately locate the position of the peak emission of the various lines in order to precisely constrain the steep temperature gradient (from 300~K to 30~K in about 10 arcsec). ===================================================================================== DRSP 2.4.1 Title CO surveys of disks around stars from 0.3 to 3 msun Pi A. Dutrey Time 2760 hrs 1) CO surveys of disks around stars from 0.3 to 3 msun Authors: A.Dutrey, S.Guilloteau 2. Science goal: Study the gaseous disk structure (temperature, density, Rout(CO), = turbulence) and kinematics from the CO lines. Measure the stellar mass of the = central object. Correlate disk properties with stellar properties. Needed: 12CO 2-1, 3-2, trace the temperature distribution at the disk surface 13CO 1-0, 2-1, 3-2, trace the temperature/density 1-2 scale heights = above the mid-plane C18O 2-1, 3-2, trace the temperature/density in the mid-plane according to Dartois, Dutrey, Guilloteau 2003 3. Number of sources: Roughly 40. 4. Coordinates: 4.1. 5 sources in Hyd (RA= , DEC=-60) 15 sources in ChaI (RA=11, DEC=-70) 20 sources in Oph (RA=16:30, DEC=-24) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.2-0.4 arcsec 5.2. Range of spatial scales/FOV: up to 8 arcsec 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3, Band 6, Band 7 6.2. Lines: 12CO 2-1, 3-2, 13CO 1-0, 2-1, 3-2, C18O 2-1, 3-2 A. Frequency: 110, lines 13CO & C18O 1-0, + 12CO 1-0 (if possible) B. Frequency: 219-220/230, lines 13CO & C18O 1-0 + 12CO 2-1 (required) C. Frequency: 329-330, lines 13CO & C18O 3-2 D. Frequency: 345, line 12CO 3-2 6.3. Spectral resolution (km/s): 0.1km/s (0.05 km/s to estimate the = turbulence) 6.4. Spectral coverage (km/s or GHz): ~30-40 km/s disk 7. Continuum flux density: 7.1. Typical value: 10-500 mJy, varying as nu^3 7.2. Continuum peak value: 0.2-5 mJy/beam, varying as nu^2 (resolving the disk) 7.3. Required continuum rms: Band dependent 7.4. Dynamic range in image: intrinsic range of order 1000, not required for this study. 8. Line intensity: limited by 13CO 1-0 & C18O 2-1, 3-2 8.1. Typical value: 0.5-40 K (depending on lines) 8.2. Required rms per channel: 0.5 K 8.3. Spectral dynamic range: low (in each channel...) 9. Polarization: YES if possible (12CO line + continuum) (integration time not based on polarization) 10. Integration time per setting: A (110 GHz) at 0.4", rms 1.8 K in hour, required 13 hrs per source B (220 GHz) at 0.2", rms 2.6 K in hour, required 27 hrs per source C (330 GHz) at 0.2", rms 2.7 K in hour, required 29 hrs per source 11. Total integration time for program: 69 hours per source X 40 sources = 2760 hours 12. Notes Time estimate can only be reduced by degrading angular resolution. At 1" (110 GHz) and 0.5" (220 and 330 GHz) as done currently at IRAM = PdB, required total time is 440 hours ************************************************************************* Review Phil Myers: Science case okay, but requested time for resolution 0.2-0.4 arcsec is equivalent to 345 8-hour tracks - impractical! -------------------------------------------------- Review v2.0: 1) CO surveys of disks around stars from 0.3 to 3 msun Authors: A.Dutrey, S.Guilloteau Reviewer: John Bally Too many transitions and sources are proposed. I recommend the selection of fewer targets. You could pick the closest disks associated with central-star masses of say 0.3, 1, and 3 Msol. In each mass-range, pick a nearly face-on example, and a nearly edge-on one. Why do we need to observe 40 sources? Reply: If you take sources at different ages, you very rapidly need 40 sources to sample reasonnably the astrophysical problems. Some specific targets such as the IRN in Cha I, or VLA1623 in rho-Oph should be emphasized. The line list should be pruned; do you really need three transitions in each isotopic variant of CO? Should the observations be obtained in scaled-arrays that produce matched beams? I would emphasize the highest frequency lines to maximize angular resolution. Reply: Only the generic distance (~150 pc = Taurus distance) is important since it is not a real proposal In addition to measuring scale-heights, rotation curves, and the disk and stellar masses, these ALMA observations should enable searches for second-second order structure parameters of the disks such as spiral density waves, gaps, and radial variations in the abundances of the various isotopes and observed molecular species by referencing the line-strengths to the continuum produced by dust. Multi-wavelength dust continuum fluxes and polarization may provide constraints on radial (and azimuthal) variations in grain sizes and magnetic field geometry. Reply: Of course, you are right! This is not a real proposal but a time estimate for a well define problem: CO surveys in TTauri disks. Rapid switching between sources should enable multiple targets to be observed within each 8-hour shift, contrary to the Phil Myers comment (DRSP 1.0 review). Reply: YES ===================================================================================== DRSP 2.4.2 Title Molecular surveys in 2-3 ``small'' samples from 0.5 to 3 msun Pi A. Dutrey Time 229 hrs Molecular surveys in 2-3 ``small'' samples from 0.5 to 3 msun Authors: A.Dutrey, M.Momose, S.Guilloteau, E. van Dishoeck 2. Science goal: Study observable chemistry as complete as possible in a few protoplanetary disks orbiting stars from 0.5 to 3 msun. The goal is to estimate abundance gradients, within the disk and from object to object. It is required to disentangle between excitation conditions and abundance gradients by observing several transitions of the same molecule. A frequency survey AS COMPLETE AS possible - using all the flexibility of the correlator - is required. The sensitivity required to complete such a survey is not easy to derive. As a first order, one can note that lines detected so far become optically thick inside a radius R1 ranging from 50 to 300 AU. With a power law of the surface density, a line with Tau=1 at 50 AU has Tau=0.07 at 300 AU. We thus select to work at an opacity limit of 0.05 (1 sigma per channel). Moreover, we include a few much deeper integrations in Band 6 to reach tau=0.02 and search for more complex molecules. We select an angular resolution of 0.4", allowing to partially resolve the optically thick core (60 AU at 150 pc). 3. Number of sources: 6 4. Coordinates: 4.1. 3 sources in Taurus (RA=04:30, DEC=+30) 3 sources in Oph (RA=16:30, DEC=-24) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.4 arcsec 5.2. Range of spatial scales/FOV: up to 8 arcsec 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3, 6, 7, 9 6.2. Lines: see table below as (an incomplete) example 6.3. Spectral resolution (km/s): 0.2km/s 6.4. Spectral coverage (km/s or GHz): ~30-40 km/s disk 7. Continuum flux density: see also 3) 7.1. Typical value: 50-200 mJy 7.2. Continuum peak value: 7.3. Required continuum rms: 7.4. Dynamic range in image: 8. Line intensity: 8.1. Typical value: opacity limit of 0.05 at Tk=10--40 K, i.e. 0.5--2 K (deeper integration down to tau=0.02 for Band 6) 8.2. Required rms per channel: 0.5 K (deeper for Band 6) 8.3. Spectral dynamic range: low (in each channel...) 9. Polarization: not in this proposal 10. Integration time per setting: Band 3: rms 1.7 K per hour, 12 hours per tuning, 2 tunings, 24 hours Band 6: rms 0.4 K per hour, 3.3 hour per tuning, 3 tunings, 10 hours Band 7: rms 0.5 K per hour, 1 hour per tuning, 3 tunings, 3 hours Band 9: rms 0.3 K per hour, 0.4 hour per tuning, 3 tunings, 1.2 hours Total: 38 hours per source, of which 14 at Band 6 and above. 11. Total integration time for program: For 6 sources, 229 hours. Column density with 1K km/s for each transition under LTE and optically thin condition (Courtesy of Takakuwa at CfA) Line transition Frequency 20 K 50 K HCO+ 1-0 89.188 1.39407967E+12 2.94454009E+12 CS 2-1 97.981 5.70174978E+12 1.11192032E+13 C18O 1-0 109.782 1.30730522E+15 2.70087115E+15 13CO 1-0 110.201 1.29839255E+15 2.68121637E+15 CO 1-0 115.271 1.1979902E+15 2.45996908E+15 C18O 2-1 219.560 5.3351956E+14 8.22277114E+14 13CO 2-1 220.399 5.30987708E+14 8.16971591E+14 CO 2-1 230.538 5.0249783E+14 7.57216339E+14 CS 5-4 244.935 3.56575535E+12 3.07323687E+12 HCO+ 3-2 267.558 4.27181797E+11 4.91656758E+11 C18O 3-2 329.331 5.16935379E+14 4.99454013E+14 13CO 3-2 330.588 5.1608577E+14 4.96851068E+14 CS 7-6 342.883 8.32157289E+12 2.88205239E+12 CO 3-2 345.796 5.07081138E+14 4.67465531E+14 HCO+ 4-3 356.734 5.62513526E+11 3.88788454E+11 ************************************************************************ Review Phil Myers:transitions proposed for observation include only CO and CS isotopomers, thus may not "completely" study "observable chemistry" in disks--no N species are included. Comment Ewine: Above table by Takakuwa is only illustrative for a few dominant species. Many more molecules can be covered in one correlator setting. -------------------------------------------------- Review v2.0: Molecular surveys in 2-3 ``small'' samples from 0.5 to 3 msun Authors: A.Dutrey, M.Momose, S.Guilloteau, E. van Dishoeck Reviewer: John Bally The Taurus fields are far north. Sources in Cha I or in one of the other southern SFRs would be more appropriate targets. It would be desirable to conduct full spectral scans of one or more entire windows to determine the contents of large molecules. The targets should be pre-selected for spectral richness using single-dish observations. These multi-species searches could trace the "snow-lines" for various species - at what radii do they disappear from the gas phase? If gaps or other disk structures are seen, do molecular abundances vary from the shadowed to the illuminated sides of gaps? Reply: You are too optimistic, the abundant molecules are already known, from single-dish obsevrations. Unfortunately, even with the ALMA sensitivity (eg see for example our PPV revieW), the chance to detect the snow-line is very very low... Idem for the shadowed to illuminated sides of gaps... Disks around double stars such as L1551 IRS5 which has both circumstellar and circumbinary disks should also be considered for such studies. Reply: YES, but this is not a proposal ===================================================================================== DRSP 2.4.3 Title Continuum survey from 80 to 900 GHz Pi S.Guilloteau Time 260 hrs 1. Title: Continuum survey from 80 to 900 GHz Authors: S.Guilloteau, A.Dutrey, M.Saito 2.Science Goals: Determine the dust evolution and coagulation processes. To disentangle grain properties from the disk properties, it is needed to map disks at several submm/mm wavelengths with sufficient angular resolution (0.1"-0.2"). In particular, obtaining the evolution of the dust emissivity as function of radius is a key parameter to constrain the dust coagulation process. To do so, it is required to resolve the optically thick at least at 2 frequencies, and to obtain sufficient brightness sensitivity at all frequencies up to some outer radius in order to derive the SED (and thus Beta) in a few radial bins. Optically thick radius for dust is about 20 - 50 AU at 1 mm. To get a few radial bins, we should detect the dust at least up to 300 AU, and observe with a resolution 0.1" (15 AU at 150 pc). At this resolution, there are 120 beams at a radius of 300 AU (for a face on disk). Goals: dust characterization (abs.coefficient, spectral index) dust disk properties (outer radius, surface density, temperature) 3.Number of sources: ~ 70 4.Coordinates: 4.1 5 sources in Hyd (RA= , DEC=-60) 15 sources in Taurus (RA=04, DEC=+25) 20 sources in ChaI (RA=11, DEC=-70) 20 sources in Oph (RA=16:30, DEC=-24) 10 sources in ONC (RA=05, DEC=-05) 4.2 Moving target: no 4.3 Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.1 arcsec 5.2. Range of spatial scales/FOV: up to 5 arcsec 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3, Band 6, Band 7, Band 10 6.2. Lines: no or CO if done in parallel with DRSP 2.4.1. 7. Continuum flux density: 7.1. Typical value: 50-200 mJy 7.2. Continuum typical brightness at 300 AU A. 110 GHz 30 mK B. 230 GHz 60 mK C. 350 GHz 90 mK D. 670 GHz 180 mK 7.3. Required continuum rms: Signal to noise of 10 on the brightness at 300 AU, where we have about 120 beams, so the required rms per beam is A. 110 GHz 33 mK B. 230 GHz 60 mK C. 350 GHz 0.1 K D. 670 GHz 0.2 K 7.4. Dynamic range in image: high in general (> 1000) 9. Polarization: Yes 10. Integration time per setting: A. rms in 1 hr: 60 mK 3.30 hrs per source B. rms in 1 hr: 30 mK 0.25 hrs per source C. rms in 1 hr: 40 mK 0.16 hrs per source D. rms in 1 hr: 35 mK 0.03 hrs per source Total 3.7 hours per source 11. Total integration time for program: 260hr 70(src)x(3.7 hrs)= 260 hrs ************************************************************************* Review Phil Myers: Good basic data program. Good for disk structure, may also be useful for dust evolution and coagulation. -------------------------------------------------- Review v2.0: 1. Title: Continuum survey from 80 to 900 GHz Authors: S.Guilloteau, A.Dutrey, M.Saito Reviewer: John Bally Unclear why 70 sources need to be observed. A well-chosen sub-set of the nearest disks should be selected for this program. Disk orientation should also be specified. Nearly face-on disks will provide the clearest perspective, but also have the lowest optical depths. Nearly edge-on disks will tend to have higher optical depths, but structure information will be sacrificed. ===================================================================================== DRSP 2.4.4 Title Disks in the sub-stellar regime Pi L. Testi Time 54 hrs ================================ 1. Name of program and authors Disks in the sub-stellar regime Authors: L.Testi 2. One short paragraph with science goal(s) Detect dust continuum and molecular line emission from a sample of young substellar systems. The goal is to constrain the disks fraction, mass distribution, size and gas content in the substellar regime. We need to detect dusty disks to a significative level (<=0.01 Mstar @ 10sig), and to resolve disks if radius greater than 20 AU. A separate proposal should address the dust emissivity in the detected sources. Comparison with more massive TTs will be done using literature data, observations from other ALMA programmes, and observations of TTs that will fall within the ALMA field of view (esp. in rho-Oph and ONC). Secondary: Detect CO and isotopes in these disks at the sensitivity limit provided by the main goal (the continuum). 3. Number of sources 10-100 objects per region in Taurus, Cha I, rho-Oph and Orion Nebula Cluster. 4. Coordinates: 4.1 10 sources in Taurus (RA=04, DEC=+25) 20 sources in ChaI (RA=11, DEC=-70) 30 sources in Oph (RA=16:30, DEC=-24) 100 sources in ONC (RA=05, DEC=-05) 4.2 Moving target: no 4.3 Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.2-0.1 arcsec (depending on distance) 5.2. Range of spatial scales/FOV: up to 5-10 arcsec 5.3. Required pointing accuracy: no critical constraints 6. Observational setup 6.1. Single dish total power data: no 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 6 and 7 7.2. Lines and Frequencies (GHz): CO and main isotopes in bands 6 and 7, as allowed by the hardware. 7.3. Spectral resolution (km/s): <=0.2 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): >=40 km/s 8. Continuum flux density: 8.1. Typical value (Jy): 0.1-0.3 mJy 8.2. Required continuum rms (Jy or K): 0.03 mJy/beam @ 230GHz; 0.25 mJy/beam @ 345GHz 8.3. Dynamic range within image: Low in general, but may be high in some regions (Ophiucus, ONC) 8.4. Calibration requirements: absolute ( 5% ) repeatability ( n/a ) relative ( 1-3% ) 9. Line intensity: sensitivity limited by continuum goals 9.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 5% ) repeatability ( n/a ) relative ( 1-3% ) 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 15min/obj @ Band6 = 40 hrs 5min/obj @ Band7 = 14 hrs 12. Total integration time for program (hr): 20min/obj = 54 hrs 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): ================================ -------------------------------------------------- Review v2.0: Disks in the sub-stellar regime Authors: L.Testi Reviewer: John Bally As with many other proposed disk programs, I advocate a pilot study using a compact configuration of ALMA (roughly 1" resolution) to identify the best candidates for high-resolution observations. The spectral-line contents of bright continuum detections should also be explored in this mode to find the best gas tracers since it is NOT obvious that in a disk, the usual lines such as CO are the best tracers. High angular resolution studies can then be done on the best candidates. While ONC is a great target, some closer clusters such as IC 348 or NGC1333 should be considered. ---------------------------------------------------------------------- Reply: I do not want to go for Cepheus (not observable from Chajnantor) or other barely observable northern sources like IC348 or NGC1333. The principle of doing the observations of BD disks at low angular resolution could be considered, although I do expect that this project can be done at the 0.1 arcsec level, which may well be not so oversuscribed and difficult to do... Having this resolution will help in figuring out the size of these disks, a key to test ejection scenarios. ===================================================================================== DRSP 2.4.5 Title Gaps in nearby protoplanetary disks Pi S.Guilloteau Time 13 hrs Gaps in nearby protoplanetary disks ================================== Authors: S.Guilloteau, A.Dutrey 2. Science goal: image gaps created by protoplanets in nearby dust protoplanetary disks. The goal is to measure the gap radius and the brightness contrast gap/disk in order to constrain hydrodynamics models of planet formation in disks. See also predictions by Wolf et al., 2002. We have to image to a significant brightness level at the highest possible angular resolution. For a proto-Jupiter, the gap width is about 1-2 AU. The highest possible angular resolution (0.013", i.e 1.8 AU at 140 pc) is therefore required. The proposed observed frequency is 345 GHz, high enough to provide high angular resolution, but not too high because otherwise even the gap would be optically thick to dust emission. At 5 AU from the star, the dust opacity at 345 GHz will be of order 8 to 20, but since the surface density contrast is expected to be of order 100, the gap will still be optically thin. A secondary goal would be to detect ``CO gaps'' in these disks at the sensitivity limit provided by the main goal (the continuum). 3 Number of sources: 5 objects 4.Coordinates: 4.1 2 sources in Taurus (RA=04, DEC=+25) 1 in Hya (TW Hya) (RA=11, DEC=-34) 2 sources in ChaI (RA=11, DEC=-70) 4.2 Moving target: no 4.3 Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.035 arcsec 5.2. Range of spatial scales/FOV: up to 1 arcsec 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 7 6.2. Lines: CO (3-2) line Frequency: 345 GHz 6.3. Spectral resolution (km/s): 1 km/s 6.4. Spectral coverage (km/s or GHz): >=100 km/s 7. Continuum flux density: 7.1. Typical value: N/A 7.2. Continuum peak brightness: 50 - 200 K 7.3. Required continuum rms: 1 K 7.4. Dynamic range in image: > 100:1 8. Line intensity: sensitivity limited by continuum goals 8.1. Typical value: 50 - 200 K (optically thick) 8.2. Required rms per channel: N/A 8.3. Spectral dynamic range: N/A 9. Polarization: no 10. Integration time per setting: rms in continuum : 1.6 K in 1 hour, so 2.6 hours required. in line. Note that this gives at 1 km/s resolution a brightness rms of 80 K. 11. Total integration time for program: 5 sources at 2.6 hours = 13 hours *********************************************************************** Review Phil Myers: for gap imaging, candidate disks should be more nearly face-on than edge-on, authors do not say how they would select face-on candidates (other than TW Hya). Time requested is remarkably short -- a bargain! -------------------------------------------------- Review v2.0: Gaps in nearby protoplanetary disks ================================== Authors: S.Guilloteau, A.Dutrey Reviewer: J. Bally I would add higher frequency data as well. Thought it is possible that gaps may become optically thick, we do not know for sure. The highest possible resolution should be sought for in this experiment. Furthermore, I would expect that the inner edge of a gap may be in shadow, and therefore colder than the outer edge which may be illuminated, and therefore warmer. Planets opening gaps are expected to be surrounded by circum-planetary disks and spiral waves. These features may be picked-up by the highest resolution ALMA images of the closest sources. Accreting proto-giant planets are also expected to have photospheres nearly an AU in diameter. ALMA may directly detect such objects as compact point sources within a gap. They may be hotter than surrounding dust due to accretion heating. ===================================================================================== DRSP 2.4.6 Title Transitions disks around CTTs/WTTs & near ZAMS stars. Pi A.Bacmann Time 88 hrs 1. Title: Transitions disks around CTTs/WTTs & near ZAMS stars. Authors: A.Bacmann, A.Dutrey 2. Science goal: To detect and map disks having a low flux density in continuum at 1.3mm (<=20-50 mJy) and found around CTTs (Classical TTauri stars), WTTS (Weak line T Tauri stars) and near ZAMS (Zero Age Main Sequence) stars in CO and in the continuum. The observations should allow to determine the disk properties, i.e. the gas disk, extent, disk mass, kinetic temperature, CO depletion with respect to the dust mass. The goal is to understand the dissipation of disks around pre-main sequence stars from 0.5 to 3 msun. 3. Number of sources: Taurus, Rho Oph., Scorpius, Chamaeleon, Lupus - = in total 50 objects 4. Coordinates 4.1. RA & DEC Taurus: RA=04 DEC=+25 - 10 Oph: RA=16:30 DEC=-24 - 20 ChaI: RA=11 DEC=-70 - 20 Lupus: RA=16 DEC=-35 ? Sco: RA=17 DEC=-40? 4.2. moving target: no 4.3. Time critical: no 5. Spatial scales 5.1 angular resolution: 0.3" (resolve disk to first order) 5.2 single field 5.3 total power: no 5.4 ACA no 5.5 subarrays: no 6. Frequencies 6.1 Frequency band: 6 and 7 6.2 Line and Frequencies (GHz) A. 12CO(2-1) 230.5 GHz and 13CO(2-1) 220.4 GHz (if tuning allows) B. 13CO(3-2) 330.6 GHz 6.3 Spectral resolution: 0.2 km/s 6.4 Bandwidth/Spectral coverage: 40 km/s 7. Continuum flux density 7.1 Typical value (Jy) 0.02 Jy 7.2 Required rms 0.1 mJy/Beam 7.3 Dynamic range within image: standard, low 8. Line intensity 8.1 typical value: in 12CO(2-1): 0.1 - 1 Jy.km/s (based on BP Tau) Expected linewidth is 3 - 5 km/s (small sources). 8.2 required rms per channel: 7 mJy (or 2 K in brightness) (about 5 sigma per channel) 8.3 spectral dynamic range 9. polarisation: no (too weak) 10. integration time per setting A. 12CO(2-1) 230.5 GHz and 13CO(2-1) 220.4 GHz (if tuning allows) 10 minutes per source for 12CO(2-1). The continuum sensitivity is 20 microJy. (Note: If a limit on 13CO is needed, 30 minutes per source to get a brightness sensitivity of 1 K; this will NOT be sufficient to detect 13CO in the optically thin sources.) B. Search for 13CO(3-2) in the most interesting sources. 13CO(3-2) opacity is 9/4 / 60 times the 12CO(2-1) opacity, i.e. 0.04 if the 12CO is marginally optically thick. The expected brightness is thus about 20 -- 50 K x 0.04 = 1 -- 2 K. The brightness sensitivity should be around 0.3 K. This requires 8 hours per source. (Note: using the 13CO(2-1) line, the needed sensitivity is 0.13 K, and requires 36 hours per source). 11. total integration time for program: A. Search for 12CO 50 x 10 minutes = 8 hours B. 13CO on the 10 most interesting sources = 80 hours Total = 88 hours. ***************************************************************************** Review Phil Myers: I suspect that more than 8 hours will be needed to detect 12CO 2-1 from most of the sample, especially the older members which will have a lot less gas than does the BP Tau disk. -------------------------------------------------- Review v2.0: 1. Title: Transitions disks around CTTs/WTTs & near ZAMS stars. Authors: A.Bacmann, A.Dutrey Reviewer: John Bally This should be a two-step program: First, detect disks with a compact configuration of AMLA that delivers a roughly 1" beam that is matched to the expected source diameter. Second, obtain high-resolution images of the best detected sources with a resolution of 0.1" to characterize the line and continuum emission. It is unclear if CO and its isotopes will be the best tracers of transition disks. I would expect that most CO will have frozen out or been processed into other compounds. On the other hand, it is also possible that rare isotopic variants (13CO, C18O, or C17O) may be better tracers than CO. Before large amounts of observing time are spend on observing many targets in these lines, a few selected objects should be subjected to an extensive spectral line search to identify the best tracers of the gas phase. I would not be surprised if some molecular ions or other exotic species served to trace the gas better. ===================================================================================== DRSP 2.4.7 Title Structure of Debris disks & Vega-type objects. Pi A. Dutrey Time 690 hrs Structure of Debris disks & Vega-type objects. ================================================= Authors: A.Dutrey, S.Guilloteau 2. Science Goals: search for large dust particles (~mm - cm size) and ``cold gas'' in nearby debris disks in order to characterize their physical properties and evolutionary scheme, taking into account the Mid-IR to optical properties of these systems. Needed: CO and dust mapping (mosaic for nearby systems, D< 30pc) 3. Number of sources: 5 4. Coordinates 4.1. Scattered in the sky - 5 objects (all famous) eg, Vega, Beta Pic, E Eri, etc... 4.2. moving target: no 4.3. Time critical: no 5. Spatial scales 5.1 angular resolution: 0.5 -- 1.5" (minimum possible) 5.2 mosaicing in most cases - 3-15 fields - depending on distance, = ang.size, inclination angle 5.3 total power: yes 5.4 ACA yes 5.5 subarrays: no 6. Frequencies 6.1 Frequency band: 6 (cold extended gas), 7, 9 6.2 Line and Frequencies (GHz) A. 230 GHz 12CO(2-1) and continuum GHz (and if possible 13CO(2-1) = 220.4 GHz) B. 345 GHz 12CO(3-2) and continuum C. 670 GHz continuum at 0.5 mm 6.3 Spectral resolution: 0.2 km/s 6.4 Bandwidth/Spectral coverage: 40 km/s 7. Continuum flux density 7.1 Typical value (Jy) 5- 10 mJy (over 100 -- 800 clean beams) 7.2 Required rms: A. 5 microJy/Beam - resolved B. 10 microJy/Beam C. 40 microJy/Beam (using a pessimistic SED in nu^2) 7.3 Dynamic range within image: standard 8. Line intensity 8.1 typical value: in 12CO(2-1): unknown! < 0.1 Jy.km/s ? 8.2 required rms per channel: as given by continuum requirement: A. 11 mK brightness for 0.2 km/s resolution B. 20 mK brightness for 0.2 km/s resolution C. N/A (no line) 8.3 spectral dynamic range: standard 9. polarisation: no (too weak) 10. integration time per setting / per object A. 7 hrs per field, total of 20--30 fields for the 5 objects B. 6 hrs per field, total of 40--60 fields for the 5 objects C. 10 hrs per field, total of 80--120 fields for the 5 objects for a blind search. 11. total integration time for program The number of fields can be more accurately specified once the part A. (Band 6) has been observed. We shall count in total 30 fields for A, 30 fields for B and C. Total 30 x (6+7+10) = 690 hours. ************************************************************************* Review Phil Myers: Useful goal to image nearby debris disks in several bands. But the authors say the typical 12CO line intensity is "unknown" and yet they request 690 hours or the equivalent of 86 8-hour periods. Too vague and an impractical time request. Comment Ewine: I expect that there will be large proposal pressure to do this type of program, so it is OK to keep in a large time request. -------------------------------------------------- Review v2.0: Structure of Debris disks & Vega-type objects. ================================================= Authors: A.Dutrey, S.Guilloteau Reviewer John Bally: The nearby debris disk, AU Mic (D= 12 pc) is a must. This provides the very best change for ALMA to observe dust structure on sub-AU scales. I would break this into a two-phase program: First, observe all targets in spectral line mode with a compact ALMA configuration that delivers a roughly 1" beam to search the spectrum for gas-phase tracers. It is unclear what species will be most easy to detect. Second, follow-up with line and continuum imaging at higher resolution in a configuration chosen on the basis of signal level found in the first phase of these observations. Reply: YES! note that even with 1'' resolution, you need to make mosaicing. ===================================================================================== DRSP 2.4.8 Title Structure and properties of disks around high-mass (proto-)stars Pi L. Testi Time 190 hrs Structure and properties of disks around high-mass (proto-)stars ================================================================ Authors: L. Testi, ... 2. Science goal: Study disk-outflow systems in the high-mass regime with the aim of comparing the results with better studied low-mass objects, to constrain competing formation mechanisms (coalescence vs.accretion) and infer disks dispersal timescales. To this effect one needs to observe suitable tracers for disks in these systems and suitable tracers for outflows. One will have to observe a sample of objects from embedded high mass protostars to young stars. Number of objects: 5/5/5/5/5 among cold protostars, warm massive cores, hot cores, UCHII regions, early Be stars and/or O stars in resolved UCHII. Total 25 objects. The disk tracers are continuum for dust (2 frequencies: 220 and 345 GHz), and rare molecules to probe the inner regions of the high-mass star forming cores [CH3CN for warm/hot cores (e.g. Cesaroni et al.), something fancier may be required for colder objects, deuterated molecules (suggestion by Caselli/Cesaroni). CO may probe disks around newly formed stars. The outflow tracers are: CO or isotopomers for embedded objects. [CO(1-0) or (2-1) from Beuther/Zhang/Molinari] 3. Number of sources: Roughly 25. 4. Coordinates: 4.1. Scattered, all on the galactic plane, most in the central regions of the Galaxy. 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.2-0.1 arcsec for disk; 2-4 arcsec for outflow 5.2. Range of spatial scales/FOV: up to 5 arcsec for disk; >20 arcsec for outflow 5.3. Single dish: yes for outflow 5.4. ACA: yes for outflow 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3, Band 6, Band 7 6.2. Lines: CO(1-0) for outflow, CH3CN(12-11)/N2D+(3-2), CO(3-2) Frequency: 115, 220/230, 345 GHz 6.3. Spectral resolution (km/s): 0.5km/s outflow; <=0.2 km/s disk 6.4. Spectral coverage (km/s or GHz): ~150 km/s outflow; <=20 km/s disk 7. Continuum flux density: 7.1. Typical value: several mJy 7.2. Continuum peak value: 1 mJy/beam (resolving the disk) 7.3. Required continuum rms: 0.1 mJy/beam 7.4. Dynamic range in image: Low in general, may be ~1000 in a few regions 8. Line intensity: 8.1. Typical value: outflow: >100 Jy (single dish); disk: few Jy (interf core) 8.2. Required rms per channel: outflow: 0.1K disk: ~1K (in both cases one will be interested in the line wings). 8.3. Spectral dynamic range: low (in each channel...) 9. Polarization: YES for continuum. 10. Integration time per setting: outflow (Band 3, low res, ACA, single dish): 10 min/pointing, typical size of these outflows may require up to 10 pointing = mosaics (see Shepherd/Gueth works): ~1.5 hrs/src (+ACA/+SD) disk (Band 6 and Band 7): 3hr/source/freq (single pointing) 11. Total integration time for program: 190h 25(src)x(1.5h+3h+3h)=~190h ********************************************************************** Review Phil Myers: Interesting for imaging of high-mass systems and their outflows, yet it seems unlikely to tell us much about disk dispersal timescales with only 5 members in each group. -------------------------------------------------- Review v2.0: Structure and properties of disks around high-mass (proto-)stars ================================================================ Authors: L. Testi, ... Reviewe John Bally: The nearest sources - those within 1 kpc need to be given top priority because these are where the highest resolution will be achieved. OMC1, OMC1-S, and Cepheus A (HW2 and HW3c) should be done in detail first. "Second tier" sources located within 1 to 3 kpc should be the second priority. Existing data already shows that all nearby bigh-mass SFRs that have suspected disks also contain multiple stellar sources within the projected extents of their disks. The highest AND lowest continuum frequencies should be used to search for point sources that may indicate companion stars. Spectral indices will be needed to distinguish dust emission from hyper-compact HII regions expected to surrounding stars more massive than 10 Solar masses. Continuum frequencies need to be selected carefully to minimize contamination from line emission. In regions like Orion it may be difficult to find portions of the spectrum that are truly emission-line free! ===================================================================================== DRSP 2.4.9 Title Dust and Gas distribution in multiple-systems Pi A. Dutrey Time 120 hrs Dust and Gas distribution in multiple-systems ============================================= Authors: A.Dutrey, M.Saito 2. Science Goals: Mapping the dust and gas distribution around multiple systems in order to estimate the frequency of CB ring and inner disks or binary system, the mass distribution, possible streamers flowing from the outer disk to the inner disks. Selected samples in clusters and in loose association such as Taurus. It is needed to detect low brightness dusty disks, or very small disks. Disks larger than 20 AU should be resolved. The angular separation of the stars range from 3" (450 AU) to 0.05" (8 AU). Inner disks in the closer binaries may be truncated to only 2 AU or so. Such inner disks, at 50 K, will have a flux around 75 microJy at 345 K. For the outer disks, the brightness may be low, e.g. 50 mK or so (corresponding to 45 microJy/beam at 345 GHz and 0.1" resolution). A secondary goal: Detect CO in these disks (kinematics) at the sensitivity limit provided by the main goal (the continuum). 3. Number of sources: 20 objects per region 4. Coordinates: 4.1 20 sources in Taurus, 20 sources in Rho Oph. (RA=04, DEC=+25) (RA=16:30, DEC=-24) 4.2 Moving target: no 4.3 Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.1-0.05 arcsec (depending on separation) 5.2. Range of spatial scales/FOV: up to 5-10 arcsec 5.3. Single dish: in some sources 5.4. ACA: In some sources 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: band 7 (best for continuum, not too bad for C18O = 3-2 line) 6.2. Lines: CO/13CO/C18O lines (depending on line opacity in cloud) Frequency: 345 GHz Note: 2 tunings required. We shall spend 1/3 time on 12CO, 2/3 on 13CO and C18O. 6.3. Spectral resolution (km/s): <=0.2 km/s 6.4. Spectral coverage (km/s or GHz): ~ 40 km/s 7. Continuum flux density: 7.1. Typical value: 5-200 mJy (warning: expected low flux density for CB rings) 7.2. Continuum peak value: 1--10 mJy/beam 7.3. Required continuum rms: 15 microJy/beam 7.4. Dynamic range in image: Low in general, but may be high in some regions 8. Line intensity: sensitivity limited by continuum goals 8.1. Typical value: (C18O 2-1) 8.2. Required rms per channel: in brightness, 2.7 K in 0.2 km/s at 0.1". Better sensitivity by smoothing to 0.5 km/s and slightly in angular resolution. 8.3. Spectral dynamic range: Low. 9. Polarization: YES in continuum 10. Integration time per setting: 3 hrs / pointing (1hr on 12CO, 2hr on 13CO and C18O) 11. Total integration time for program: 120h 20 x 3h=60h Taurus 20 x 3h=60h Ophiucus Note: In some cases (Rho.Oph.) many targets in small area, may be more efficient to do a mosaic. ************************************************************************ Review Phil Myers: Good program to study structure of young binaries and small disks, taking advantage of ALMA resolution. -------------------------------------------------- Review v2.0: Dust and Gas distribution in multiple-systems ============================================= Authors: A.Dutrey, M.Saito Reviewer: John Bally An initial program should use a compact ALMA configuration to identify the brightest multiple sources of continuum and line emission. This pilot program should also do a line search to identify the brightest emission lines for tracing the gas. R.: yes High-resolution observations should concentrate on the brightest and/or most interesting sources. I do not see justification for observing 40 sources in two clouds. R.: statistics Perhaps special emphasis should be placed on selecting tight clusters of multiple sources where a single pointing may be used to study many objects. Reply: The DRPS is not a proposal ===================================================================================== DRSP 2.4.10 Title Deuteration in Proto-Planetary Disks: DCO+ and HDO Pi A. Dutrey Time 25 hrs TEMPLATE 2: ================================ 1. Name of program and authors Deuteration in Proto-Planetary Disks: DCO+ and HDO Dutrey, Guilloteau et al., 2. One short paragraph with science goal(s) Measure deuteration in proto-planetary disks (DCO+ and HDO). The sensitivity estimates are based on the following paper. Guilloteau et al., 2006 - DM Tau 3. Number of sources We focus first on a single representative object located at 150 pc in Taurus (for example DM Tau). Then, we assume we make a survey of 20 sources. 4. Coordinates: 4.1. Rough RA and DEC If Taurus: RA = 04h and DEC = 30 deg 4.2. Moving target: no (e.g. comet, planet, ...) 4.3. Time critical: no (e.g. SN, GRB, ...) 5. Spatial scales: 5.1. Angular resolution (arcsec): ~ 1'' (150 AU at 150 pc) 5.2. Range of spatial scales/FOV (arcsec): single-field 5.3. Required pointing accuracy: (arcsec) standard 6. Observational setup 6.1. Single dish total power data: no 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9 Bands 4, 8 7.2. Lines and Frequencies (GHz): Band 4: DCO+ 2-1 at 144.07373 GHz Band 8: HDO 101 000 at 464.9425 GHz 7.3. Spectral resolution (km/s): 0.1 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 10 km/s 8. Continuum flux density: ~ 100 mJy at 1.3mm 8.1. Typical value (Jy): Band 4: ~ 60 mJy Band 8: ~ 450 mJy 9. Line intensity: Band 4: DCO+ 2-1 (peak) ~ 0.1 Jy DCO+ 2-1: 0.1Jy ~ 0.65K for a disk size of 3'' Band 8: HCO (peak, likely in absorption) ~ 0.1 Jy 9.1. Typical value (K or Jy): Note that only about 20% of the disk is emitting at a given velocity (see Guilloteau et al., 2006), hence the brightness is expected to be around ~ 3K 9.2. Required rms per channel (K or Jy): DCO+: Taking Tb = 3 K as representative, a 10 sigma detection per channel, should require: DCO+ 2-1: 0.3 K (for 1'' resolution) For mapping HDO 101-000: ~ 0.02Jy or ~ 0.12 K for a resolution of 1'' For 5 sigma detection/channel 9.3. Spectral dynamic range: standard 9.4. Calibration requirements: absolute ( 10%) repeatability ( 5%) relative ( 5%) 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): Band 4: DCO+ J=2-1: 0.5h per source - MAPPING Band 8: HDO 101-000: 1h per source - DETECTION (channel = 0.1 km/s) 12. Total integration time for program (hr): Band 4: 20 sources --> ~ 5h - MAPPING Band 8: 20 sources --> ~ 20h - DETECTION 13. Comments on observing strategy : standard mode ================================= -------------------------------------------------- Review v2.0: Deuteration in Proto-Planetary Disks: DCO+ and HDO Dutrey, Guilloteau et al., Reviewer: John Bally This is a nice modest proposal. However, high resolution (0.1") observations that may resolve potential gradients and other structures in the HCO+/DCO+ ratio may be of interest. ===================================================================================== DRSP 2.4.11 Title Search for CI in circumstellar disks around young stars Pi A. Dutrey Time 0.33 hrs TEMPLATE 3: ================================= 1. Name of program and authors Search for CI in circumstellar disks around young stars Dutrey, Guilloteau et al., 2. One short paragraph with science goal(s) This project proposes the detection and mapping of CI in circumstellar disks around A stars since CI can be a good tracer of gas in disks of moderate dust opacity such as transition disks (eg HD141569). In such objects, the opacity at 1mum is likely < 1 but the gas-to-dust ratio is still expected to be around ~100. Sensitivity estimates are given for a (gas+dust) disk mass ~ 80 M_earth and a spectral type B9.5. The assumed disk size 10'' at 100 pc (or 1000 AU). The angular resolution expected is 1'', spectral resolution is 0.1 km/s note: calculations are adapted from the modelling of HD141569 by Jonkheid et al., 2006 3. Number of sources We focus here on a single object, as example. 4. Coordinates: 4.1. Rough RA and DEC 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution (arcsec): ~ 1'' 5.2. Range of spatial scales/FOV (arcsec): single-field 5.3. Required pointing accuracy: (arcsec) standard 6. Observational setup 6.1. Single dish total power data: no 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9 Bands 8 7.2. Lines and Frequencies (GHz): Band 8: CI 3P1-3P0 at 492.2 GHz 7.3. Spectral resolution (km/s): 0.1 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 10 km/s 8. Continuum flux density: <= 10 mJy at 1.3mm 8.1. Typical value (Jy): Band 8: ~ 30 mJy ? 9. Line intensity: CI ~ 2 K per channel (Fig.9) for a source size of 10'' (conservative value because it is taken at the systemic velocity). 9.1. Typical value (K or Jy): Since only 20% of the disk is emitting at a given velocity (see Guilloteau et al., 2006), the expected brightness is ~ 10K. 9.2. Required rms per channel (K or Jy): A 10 sigma detection per channel, requires an rms CI: ~ 1 K 9.3. Spectral dynamic range: standard 9.4. Calibration requirements: absolute ( 10%) repeatability ( 5%) relative ( 5%) 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): (channel = 0.1 km/s) 10 sigma: CI ~ 2 minutes 12. Total integration time for program (hr): For a survey of 10 sources; 10 sigma: CI ~ 20 minutes or 0.33hrs 13. Comments on observing strategy : standard mode -------------------------------------------------- Review v2.0: Search for CI in circumstellar disks around young stars Dutrey, Guilloteau et al., Reviewer: John Bally Why not also observe the 810 GHz line? The combination of 492 & 810 GHz will provide excitation constraints. Also, can the isotopic 13CI line be separated from the 12CI? If the lines are bright, it would be very useful to obtain 0.1" resolution maps in CI (both lines) to search for excitation gradients and disk structure. Complimentary dust continuum and 13CO line observations should also be obtained to constrain the relative abundances of atoms, molecules, and dust and to search for localized variations. ===================================================================================== DRSP 2.4.12 Title Protoplanetary disks in Orion Pi J. Williams Time 90 hrs 1. Name of program and authors Protoplanetary disks in Orion Jonathan Williams 2. One short paragraph with science goal(s) Primary goal is to mosaic the Trapezium cluster in Orion and map the thermal dust continuum emission from protoplanetary disks (proplyds) around solar mass stars. Observations should be at submilllimeter wavelengths where the dust emission dominates the bremsstrahlung from the ionized gas cocoons around the disks. Secondary goal is to resolve selected disks to measure surface density profiles, possibly detect inner holes, and compare the emissivity with 10 micron absorption. Tertiary goal is to measure the thermal dust continuum at a shorter wavelength and determine the frequency dependence of the grain emissivity. There is also the potential to detect rotational and possibly vibrational lines from the disk and ionization front but the confusion with the background cloud will be high. 3. Number of sources There are over 2800 identified cluster members and 74 disks seen in silhouette against the HII region background by HST. 4. Coordinates: 4.1. Rough RA and DEC The cluster extends roughly 10' in each direction from the O6 star, Theta1C at RA 05:35:16.47, Dec -05:23:23.10 4.2. Moving target: yes/no (e.g. comet, planet, ...) no 4.3. Time critical: yes/no (e.g. SN, GRB, ...) no 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution (arcsec): A1. 2'' sufficient to distinguish individual proplyds from each other and measure a total mass A2. 0.1'' necessary to resolve disks, measure surface density profiles 5.2. Range of spatial scales/FOV (arcsec): Proplyds are densely packed, just a few arcseconds away from each other toward the cluster center. The entire cluster extends over approximately 20'x20'. 5.3. Required pointing accuracy: (arcsec) standard 6. Observational setup 6.1. Single dish total power data: no/beneficial/required no 6.2. Stand-alone ACA: no/beneficial/required no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no no 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9 Bands 7, 9 7.2. Lines and Frequencies (GHz): F1. 345 GHz continuum [center on CO(3-2) in LSB, many others in passband including HCN(4-3), H13CN(4-3), HC15N(4-3), CH3OH lines] F2. 691 GHz continuum [center on 12CO(6-5) in LSB, get H13CN(8-7) and CH3OH in pb] 7.3. Spectral resolution (km/s): [0.2 km/s] 7.4. Bandwidth or spectral coverage (km/s or GHz): 8 GHz 8. Continuum flux density: 8.1. Typical value (Jy): for Hildebrand kappa_nu = 0.1 cm2/g at 1200 GHz, beta=1, T=20K minimum solar mass nebula (MMSN; 0.02 Msun) has flux 30 mJy (345 GHz) and 200 mJy (691 GHz) Disk masses in Taurus with similar ~1 Myr age as Orion average 10% MMSN 8.2. Required continuum rms (Jy or K): Aim to detect 0.1 MMSN at 5-sigma Rms = 0.6 mJy (345 GHz), 4 mJy (691 GHz) 8.3. Dynamic range within image: The cloud-HII interface in the background is several Jy at 850 microns To be limited by noise and not the background requires a dynamic range > 1000:1 8.4. Calibration requirements: absolute 10% repeatability 5% relative 5% 9. Line intensity: The background may be considerably more variable in line emission, especially if optically thick, and it is likely to be difficult to distinguish proplyd emission. Line detection is therefore a lower priority than the continuum measurements as indicated by placing observational parameters related to this in square brackets. 9.1. Typical value (K or Jy): brightness temperature for optically thick emission = 30 K beam dilution in 2'' beam ~ 10 depending on disk inclination 9.2. Required rms per channel (K or Jy): [1 K in each band] 9.3. Spectral dynamic range: [10:1 for optically thick emission, possibly >1000:1 if thin] 9.4. Calibration requirements: absolute [10%] repeatability [5%] relative [5%] 10. Polarization: yes/no (optional) no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): Primary goal to image at 345 GHz at 1-2'' resolution and 0.6 mJy rms (A1/F1) requires 10 seconds per field. Mosaicking the central 20'x20' at 10'' (Nyquist) spacing of the cluster requires 14400 pointings, corresponding to 40 hours (not counting telescope slew times). Secondary goal to resolve selected disks (A2/F1) requires 30 minutes per object, assuming the flux is spread over 20 beams. Tertiary goal to image disks at high frequency (A1/F2) requires 10 seconds per field. The fov is about half the diameter of the 345 GHz fov so it may be prohibitive to map the entire cluster. To map the central 10'x10' region, which contains most of the young stars, would require 40 hours. 12. Total integration time for program (hr): To mosaic the entire cluster (20'x20') at 345 GHz, the central 10'x10' at 691 GHz, and to resolve 20 disks at 345 GHz, requires a total of 90 hours. 13. Comments on observing strategy : (optional) Given the large number of pointings and the short integration times per field, there may be a significant overhead to add. ===================================================================================== DRSP 3.1.1 Title Structure and Dynamics of the Chromosphere Pi A. O. Benz Time 10 hrs 1. Structure and Dynamics of the Chromosphere Arnold O. Benz, Tim S. Bastian, Sami K. Solanki 2. Most of the sub-millimeter emissions of the quiet sun originates from the low chromosphere. It is a thin layer above the temperature minimum region, where non-radiative heating first becomes manifest. Detailed semi-empirical models have been constructed. However, it has become apparent in recent years that these models must be thoroughly revised to reflect the highly inhomogeneous and dynamic nature of the chromosphere. Moreover, the models do not contain the physics of the heating process believed to be waves, shocks, thermal conduction, electromagnetic phenomena (flare-like events) or a combination thereof. The analysis of dynamical simulations predicts that the radio emission at millimeter and submillimeter wavelengths is extremely sensitive to the dynamic processes in the chromosphere, if these are spatially resolved. The opposing view predicts heating mostly by weak wave turbulence and little fluctuations in space and time. 3. Number of sources: one 4. Coordinates: Follow solar orbital motion and solar rotation ecliptic, i.e. +- 23 degrees declination moving target ! Time critical: no 5. Spatial scales: 5.1. Angular resolution (arcsec): better than 0.1" 5.2. Range of spatial scales/FOV (arcsec): single field (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 5.3. Single dish total power data: yes/no yes 5.4. ACA: if available 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3, 6, 7, or 9 3 6.2. Lines and Frequencies (GHz): continuum, two frequencies = 6.3. Spectral resolution (km/s): none 6.4. Bandwidth or spectral coverage (km/s or GHz): 10 GHz 7. Continuum flux density: 10^6 Jy 7.1. Typical value (Jy): (take average value of set of objects) 10^6 Jy 7.2. Required continuum rms (Jy or K): 100 Jy 7.3. Dynamic range within image: 10 db 9. Polarization: yes/no (optional) no 10. Integration time for each observing mode/receiver setting (hr): 1 second 11. Total integration time for program (hr): 10 hr 12. Comments on observing strategy: Start with short observing periods to test feasibility ******************************************************************** Review Chris Wilson: -------------------------------------------------- Review v2.0: 3.1.1 was unchanged. DRSP1.1 says review by Chris Wilson but no text. I really have nothing to add; Chris' review is crystalline. ===================================================================================== DRSP 3.1.2 Title Solar Radio Recombination Lines Pi A. O. Benz Time 10 hrs 1. Solar Radio Recombination Lines Arnold O. Benz, Christoph Keller 2. Clark et al. (1995) have reported the detection of the H19-alpha line in the 350?m band. No line in the millimeter band has been detected yet in the solarmillimeter or sub-mm radiation. The extremely high sensitivity of ALMA and its spatial resolution may help to discovered them. Their detection would represent direct verification of dielectronic recombination processes in the low corona and transition region, and would offer the unique possibility of measuring the magnetic field strength in those regions through the Zeeman effect. 3. Number of sources: one 4. Coordinates: Follow solar orbital motion and solar rotation ecliptic, i.e. +- 23 degrees declination moving target ! Time critical: no 5. Spatial scales: 5.1. Angular resolution (arcsec): better than 0.1" 5.2. Range of spatial scales/FOV (arcsec): small mosaic (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 5.3. Single dish total power data: yes/no yes 5.4. ACA: yes/no if available 5.5. Subarrays: yes/no no 6. Frequencies: 6.1. Receiver band: Band 3, 6, 7, or 9 6 6.2. Lines and Frequencies (GHz): one line 6.3. Spectral resolution (km/s): 0.1 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 1 GHz 7. Continuum flux density: 10^6 Jy 7.1. Typical value (Jy): (take average value of set of objects) 10^6 Jy 7.2. Required continuum rms (Jy or K): 100 Jy 7.3. Dynamic range within image: 10 db 9. Polarization: yes/no (optional) yes 10. Integration time for each observing mode/receiver setting (hr): 1 second 11. Total integration time for program (hr): 10 hr 12. Comments on observing strategy: Start with short observing periods to test feasibility ************************************************************************ -------------------------------------------------- Review v2.0: 3.1.2 unchanged Solar Radio Recombination Lines Benz This would use total power and would use the ACA but does not provide details. I would think that all of the flux would be important for this experiment. It aims at 0".1 resolution. It requests 0.1 km/s over 1 GHz, which is not available with the ALMA correlator. Closest (ref Memo 556) is Mode 8 which provides 0.32 km/s resolution: Mode8 16 1 GHz 4096 244 kHz 0.32 km/s 2-bit x 2-bit Nyquist 512 msec 0.88 This uses two polarizations. If sensitivity and polarizations are not an issue, Mode 2 will do: 2 16 1 GHz 8192 122 kHz 0.16 km/s 2-bit x 2-bit Nyquist 512 msec 0.88 which gains a factor of two in resolution. Reply: Mode 2 is a good start. There is no reason to change the DRSP. ===================================================================================== DRSP 3.2.1 Title Evolution of Magnetic Activity in Main Sequence Stars Pi M. Guedel Time 30 hrs 13.2.1: Single DRSP Evolution of Magnetic Activity in Main Sequence Stars ===================================================== M. Guedel et al. 1. Name of program and authors Chromospheres and transition regions of magnetically active stars emit optically thick thermal bremsstrahlung that is intrinsically weak but is of major importance to estimate the magnetic area. The coronal contribution is rather unimportant, reaching a brightness temperature of perhaps 1000 K at 80-90 GHz but less than 100 K outside active regions (White & Kundu 1992, Sol. Phys. 141, 347). The optically thick layer is reached at temperatures of ~7000 K at 3 mm. If density enhancements are present, then the optically thick layer may shift to larger heights, involving higher T up to several 10^4 K. Enhanced temperatures are found in magnetic active regions (W&S 1992). At 1 mm wavelength, the temperatures at the optically thick level may be significantly smaller, down to below 6000 K for solar chromospheric models. Although stellar surfaces will not be resolved, the integrated brightness will offer important information about the surface coverage with dense (active) chromospheric regions. The proposed observations will investigate trends for three stellar samples: a) Solar analogs back in time to the zero-age main sequence. As the magnetic activity (spot coverage, X-ray emission) largely increases toward younger stars, we expect a fundamental change in the magnetic structure of the chromosphere, providing information on the base magnetic fields and their distribution. A sample of about 5-10 nearby stars of ~1 solar mass with well known characteristics (rotation period, activity indicators, fundamental properties such as Teff and radius) will be observed at one or two millimetric wavelengths. Such observations complement information available from chromospheric/transition region ultraviolet studies. A long-term extension (~10 yrs) could look for magnetic cycles in the chromospheric emission by getting a snapshot every half year. b) M dwarfs. A similar question applies to very cool stars. Their dynamo may be fundamentally different. Polar active regions may be involved. A distributed (alpha^2) dynamo may be at work, leading to chromospheres at variance with the solar example. It is suggested to compare a series of very close M dwarfs, cutting through the parameter space both in mass (from M0 to possibly nearby brown dwarfs) and activity (comparing a couple of active dMe stars and inactive dM stars). c) L, T Dwarfs: Similar study, to investigate chromospheric structure of the lowest-mass stars. Should observe two classes: old, nearby BDs, and a few young examples in star-forming regions (eg, TMC, rho Oph). 3. Number of sources: ~ 10 nearby G dwarfs (solar analogs) ~ 5-10 nearby M dwarfs ~ 5 old BDs, 5 young BDs 4. Coordinates: G stars: 02 05 +77 16 (47 Cas) 14 39 +64 17 (EK Dra) 05 54 +20 16 (chi1 Ori) 08 39 +65 01 (pi1 UMa) 03 19 +03 22 (kappa1 Cet) 13 11 +27 52 (beta Com) 20 04 +17 04 (15 Sge) 14 39 -60 50 (alpha Cen A+B) 00 25 -77 15 (beta Hyi) M dwarfs 20 45 -31 20 (AU Mic) 07 34 +31 52 (YY Gem) 10 19 +19 52 (AD Leo) 01 39 -17 57 (UV Cet) inactive dM TBD BDs: various coordinates (e.g., eps Ind, and other nearby ones) 4.2. Moving target: yes/no (e.g. comet, planet, ...) no 4.3. Time critical: yes/no (e.g. SN, GRB, ...) no 5. Spatial scales: 5.1. Angular resolution (arcsec): point 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) N/A 5.3. Single dish total power data: yes/no no 5.4. ACA: yes/no no 5.5. Subarrays: yes/no no 6. Frequencies: 6.1. Receiver band: Band 3, 6, 7, or 9 <250 GHz 6.2. Lines and Frequencies (GHz): (continuum) 6.3. Spectral resolution (km/s): N/A 6.4. Bandwidth or spectral coverage (km/s or GHz): N/A 7. Continuum flux density: 7.1. Typical value (Jy): (take average value of set of objects) (optional: provide range of fluxes for set of objects) 30-100 uJy for G and M dwarfs (5-10 pc) at 100 GHz 300-1000 uJy for G and M dwarfs (5-10 pc) at 300 GHz 7.2. Required continuum rms (Jy or K): 5-20 uJy 7.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether e.g. weak objects next to bright objects) N/A; point sources, no nearby weaker objects expected 8. Line intensity: 8.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) 8.2. Required rms per channel (K or Jy): 8.3. Spectral dynamic range: 9. Polarization: yes/no (optional) 9.1. Required Stokes I, V 9.2. Total polarized flux density (Jy) unknown but probably very weak 9.3. Required polarization rms and/or dynamic range 5% 9.4. Polarization fidelity 10. Integration time for each observing mode/receiver setting (hr): 3 hrs per target 11. Total integration time for program (hr): 30 hr 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) ************************************************************************** Review Leonardo Testi: It is hard to figure out something here, as all the technical part is TBD. I could not figure out whether line emission is interesting or not. In the most optimistic view this is a full polarization Band 3 continuum project. Assuming a 10 uJy rms for all targets, then the total time required is 1hr/object or 30 hrs total. Comment Ewine: assumed 30 hr for program Reply Guedel: The integration times changed a little bit but are better justified. The emission is all continuum. -------------------------------------------------- Review v2.0: 3.2.1: Single DRSP Evolution of Magnetic Activity in Main Sequence Stars ===================================================== M. Guedel et al. DRSP 2.0 Review Leonardo Testi: I am still unsure whether 2 frequencies (e.g. bands 3/6 or 3/4 or 4/6) are required to determine spectral indices and, in this case, whether measurements should be close (how close) in time to be useful. Answer: Two frequencies should be the minimum requirement. A spectral index can thus be obtained to check for consistency with the optically thick model. Measurements at two (or more) freqencies should be obtained within max. 1 day for the rapid rotators and up to a few days for slow rotators, to ensure that the same active regions are in view. Best would we observations closer in time. ===================================================================================== DRSP 3.2.2 Title Magnetic Energy Release and High-Energy Particles in Stellar Atmospheres Pi M. Guedel Time 14 hrs 1. Name of program and authors Magnetic Energy Release and High-Energy Particles in Stellar Atmospheres Authors Manuel Guedel 2. Science goal(s) Millimetric flares have been observed on the Sun, with characteristics that do not reproduce flare emission at lower, centimetric wavelengths. The radiation is due to the gyrosynchrotron process and requires very high-energy electrons (MeV and higher). The suspicion therefore is that millimetric flares correspond to flares producing gamma-ray events from precipitating electrons and ions. However, all impulsive flares may accelerate electrons to the required MeV energies. We know from solar physics that the electron population responsible for mm bursts is most likely distinct from the electrons producing centimetric and hard X-ray flares. There is presently no hope to see gamma-ray flares from magnetically active stars, and even lower-energetic hard X-ray bursts will be extremely challenging for the INTEGRAL satellite. Short wavelength radio waves are an ideal proxy of particle acceleration to extreme energies. Magnetically active stars have shown bursts at radio wavelengths (as well as in X-rays) up to many orders of magnitude more luminous than solar flares. A T Tau star in the Orion complex (450 pc) was recently reported to flare up to 40 mJy at 86 GHz, for a duration of several days (Furuya et al., PASJ, in press). Some of the magnetospheres producing them or trapping the particles have been resolved by VLBI techniques, reaching sizes several times the stellar diameter. This project will test acceleration physics in extremely active stars that may accelerate particles for much longer periods and to much higher energies. 3. Number of sources: ~ 5-10 extremely active nearby single stars and Algol/RS CVn binaries ~ 5-10 extremely active young sources in star forming regions (150 pc for Taurus, 450 pc for Orion) 4. Coordinates: spread over the sky 4.2. Moving target: yes/no (e.g. comet, planet, ...) no 4.3. Time critical: yes/no (e.g. SN, GRB, ...) yes: should be coordinated with lower-frequency radio telescopes, and if possible with X-ray satellite observatories 5. Spatial scales: 5.1. Angular resolution (arcsec): point 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) typically point surces (wide-field mosaic advantageous for crowded star-forming regions (SFR) 5.3. Single dish total power data: yes/no no 5.4. ACA: yes/no no 5.5. Subarrays: yes/no no 6. Frequencies: 6.1. Receiver band: Band 3, 6, 7, or 9 continuum <250 GHz 6.2. Lines and Frequencies (GHz): (approximate; do NOT go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify e.g. "6 frequency settings in Band 3". Apply redshift correction yourself) (continuum) 6.3. Spectral resolution (km/s): N/A 6.4. Bandwidth or spectral coverage (km/s or GHz): 7. Continuum flux density: 7.1. Typical value (Jy): (take average value of set of objects) (optional: provide range of fluxes for set of objects) up to tens of mJy, in extreme cases up to a few 100 mJy 100 GHz (for nearby active stars, e.g. RS CVn binaries, and for T Tau stars in SFRs) 7.2. Required continuum rms (Jy or K): 0.1 mJy 7.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether e.g. weak objects next to bright objects) 10 - 1000 (not important - variable sources) 8. Line intensity: 8.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) N/A 8.2. Required rms per channel (K or Jy): N/A 8.3. Spectral dynamic range: N/A 9. Polarization: yes/no (optional) 9.1. Required Stokes I, V 9.2. Total polarized flux density (Jy) unknown but intermediate (few 10 of %) at best 9.3. Required polarization rms and/or dynamic range 5% 9.4. Polarization fidelity 10. Integration time for each observing mode/receiver setting (hr): 10 nearby single objects: 20 snapshots @ 2 minutes each, spread over 1-2 days => 7 hrs 10 SFR fields: 20 snapshots @ 2 minutes each, spread over 1-5 days => 7 hrs (Alternatives possible - shorter snaphshot integration but more snapshots) 11. Total integration time for program (hr): 14 hr 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) Should be coordinated with lower-frequency radio observations to measure spectral shape. ************************************************************************** Review Leonardo Testi: As 3.2.1, with the addition of a mysterious sentence about the requirement of an rms below 250 GHz of 0.1 mJy in one hour (?? if the goal was continuum it should be easy to go at least a factor of 10 below this number in one hour, maybe is more complicated than I think? Is the goal to obtain line observations?) Assuming as above (rms~0.01 mJy continuum full pol at 100 GHz): total time is 10 hrs total for 10 objects. Comment Ewine: assume 10 hr for program Reply Guedel: The integration times changed a little bit but are better justified. For the flare program, things are very uncertain. The more time the better, but it should come in snapshots spread over several days, so it is difficult to give a well justified number for the integration time, but I've put in a reasonable amount, I think. I've added YSOs to that program since they seem to flare in mm (recent paper on Orion). The emission is all continuum. Comment Ewine: new DRSP is baseline -------------------------------------------------- Review v2.0: 1. Name of program and authors Magnetic Energy Release and High-Energy Particles in Stellar Atmospheres Authors Manuel Guedel DRSP2.0 Review Leonardo Testi: Is this single frequency or (nearly simultaneous) multifrequency (which frequencies)? Answer: (Near-simultaneous) mutifrequency observations required to derive spectral indices and thus to characterize synchrotron spectra. Ideally, at least three frequencies should be included. It is difficult to predict which frequencies are optimum. Should try various combinations. ===================================================================================== DRSP 3.2.3 Title Thermal Emission from Red Giant and Supergiant Stars Pi K.M. Menten Time 100 hrs 13.2.1: Single DRSP Project: Thermal Emission from Red Giant and Supergiant Stars ================================================================== 1. Name of program and authors Thermal Emission from Red Giant and Supergiant Stars Authors Karl M. Menten 2. Science goal(s) As found by Reid & Menten (1997, ApJ, 476, 327 ; hereafter RM97) from multi-wavelength (8 - 22 GHz) VLA observations, red giant stars form a "radio photosphere" which is characterized by a (1) a size of ~2 times the (line free) optical photosphere, (2) temperature ~1500 K (lower than the 2000 - 2500 K stellar temperature), a thermal spectrum rising with the square of the frequency, and (3) little variability. Their technique involved (at 22 and 43 GHz) to observe simultaneously strong H2O (or, resp., SiO) masers in one narrow IF band and line-free continuum in another broad IF band. The maser emission was self-calibrated and the selfcal solutions were transferred to the continuum data, yielding perfect calibration for it, which otherwise, due to its weakness (a few mJy at 22 Jy) would have been impossible to image. RM97 successfully modeled this radiophotospheric continuum emission as due to free-free interactions of electrons released from low-ionization metals with neutral hydrogen atoms and molecules. In particular, they derived a spectrum that rises as frequency^1.9 from the lowest radio frequencies to mid-IR wavelengths until it peaks at 100 THz (3 microns) and turns over beyond. The existence of this radio photosphere also explains the lack of variations in the radio flux with stellar cycle. Observational data below 50 GHz, at 250 GHz, and above 10 THz are very well reproduced by this relationship (see, e.g. their Fig. 2). The size determinations, only marginally possible with the initial 22 GHz work, were later confirmed and refined by 43 GHz observations. The continuum emission from the radio photosphere will be of CENTRAL importance for ALL (continuum, molecular, and atomic) high resolution (better than 0.1") observations of circumstellar envelopes. This is because it will be possible to self-calibrate the continuum emission with itself at ALL ALMA frequencies. This is quite the opposite to radio frequencies, were maser observations are used to calibrate continuum data. Another important "use" of red giant continuum emission, will be (as already pointed out by MR9) that, given their well-determined spectra they will be excellent, maybe the best, point-like, absolute flux calibrators for ALMA. Finally, for all line observation, the continuum position will mark the position of the central star, whose knowledge is crucial, e.g. for model calculations, and frequently not will determinable given the often complicated, fragmented distributions of the line emission. 3. Number of sources: (see below for justifi cation of volume) Numbers of stars per kpc^3 (Jura & Kleinmann 1992, ApJS, 79, 105 All carbon 100 "Very dusty carbon" 30 S-type 30 O-rich miras (300 < P < 400 d) 210 O-rich miras (P<300 d) 35-60 "very dusty oxygen 30 This numbers should be regarded as strict lower limits of objects for which selfcal is easily possible. 4. Coordinates and expected fluxes (examples with measured radio data): (a) Stars with measured 22 GHz flux densities Star RA(J2000) Dec(J2000) D S(22.4 GHz) S(350 GHz) S(680 GHz) (pc) (mJy) (Jy) (Jy) o Cet 02 18 20.8 -02 58 37.4 128 2.6 0.48 2.4 normalized to D=100 pc: - 4.3 R Leo 09 47 33.5 +11 25 44 101 1.5 0.28 1.4 normalized to D=100 pc: - 1.5 W Hya 13 49 02.0 -28 22 03 115 3.0 0.56 2.8 normalized to D=100 pc: - 4.0 R Aql 19 06 22.3 +08 13 49 211 0.8 0.15 0.7 normalized to D=100 pc: - 3.5 chi Cyg 19 50 33.9 +32 54 51 106 1.6 0.30 1.5 normalized to D=100 pc: - 1.8 R Cas 23 58 24.7 +51 23 20 107 0.8 0.15 0.7 * normalized to D=100 pc: - 0.9 ---------------------------------------------------------------------------- adopt for D=100 pc: - 2.7 0.66 2.5 ALMA rms cont. sensitivity (in 10 s): - - 0.0005 0.003 Distance out to which star could be detected at 5 sigma (kpc): 1.6 1.3 * outside of ALMA declination range 4.2. Moving target: yes/no (e.g. comet, planet, ...) no 4.3. Time critical: yes/no (e.g. SN, GRB, ...) no 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.010-0.020 for resolution of emission, any for detection/selfcal 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) continuum only: <1", any for simultaneous line emission 5.3. Single dish total power data: yes/no no 5.4. ACA: yes/no no 5.5. Subarrays: yes/no no 6. Frequencies: 6.1. Receiver band: all 6.2. Lines and Frequencies (GHz): (approximate; do NOT go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify e.g. "6 frequency settings in Band 3". Apply redshift correction yourself) any 6.3. Spectral resolution (km/s): N/A 6.4. Bandwidth or spectral coverage (km/s or GHz): 7. Continuum flux density: 7.1. Typical value (Jy): (take average value of set of objects) (optional: provide range of fluxes for set of objects) 30-50 uJy for G and M dwarfs (5-10 pc) at 100 GHz 300-500 uJy for G and M dwarfs (5-10 pc) at `300 GHz 7.2. Required continuum rms (Jy or K): e.g. 0.5 mJy at 350 GHz 3 mJy at 680 GHz both in 10 s to allow selfcal 7.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether e.g. weak objects next to bright objects) N/A; no nearby weaker objects expected 8. Line intensity: 8.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) 8.2. Required rms per channel (K or Jy): 8.3. Spectral dynamic range: 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): Dictated by simultaneous line observations 11. Total integration time for program (hr): 100 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) ************************************************************************* Review Leonardo Testi: The project is interesting, but the estimate of the required time is obscure. The continuum does not require long integrations, but the time is set by lines, which are TBD. We can probably buy the quoted 100hrs with the idea that if more time is needed only a fraction of the sample will be done in the 3yrs covered by the DRSP. Priority: High -------------------------------------------------- Review v2.0: Project: Thermal Emission from Red Giant and Supergiant Stars ================================================================== 1. Name of program and authors Thermal Emission from Red Giant and Supergiant Stars Authors Karl M. Menten DRSP2.0 Review Leonardo Testi: It would be great to have some ideas on the lines/correlator setups... or to know that this is going to be a continuum only project. ===================================================================================== DRSP 3.2.4 Title The photospheres and proper motions of normal stars Pi Black Time 200 hrs 1. Name: The photospheres and proper motions of normal stars Authors: Black, Aalto et al 2. Science goal: Photospheric studies: Although the investigation of normal stars is usually considered the realm of UV, visible, and infrared astronomy, ALMA will afford sufficient sensitivity to observe photospheres of normal stars in the Galaxy. At first glance, one would think that stars in the Magellanic Clouds would lie beyond the reach even of ALMA. However, we know from IR surveys of red supergiants and AGB stars that the LMC and SMC contain several such stars with 10-$\mu$m magnitudes of the order of 5 or brighter. With a Rayleigh-Jeans extrapolation from 10 $\mu$m to mm/submm wavelengths, [10] = 5 mag corresponds to flux densities of 0.028 mJy at 250 GHz, 0.054 mJy at 345 GHz, and 0.22 mJy at 700 GHz. According to the ALMA sensitivity calculator, these continuum flux levels correspond to 2$\sigma$, 2$\sigma$, and 1 $\sigma$ at 250, 345 and 700 GHz, respectively, in 3600 seconds of integration. We can also estimate the observability of Galactic stars with known 250 GHz fluxes if moved to the 50 kpc distance of LMC. examples: star f250(mJy) D(kpc) f(250@D=50 kpc) S/N(after 1 hr) --------------------------------------------------------------- P Cyg 146 1.8 0.19 13sigma WR 147 379 0.63 0.060 4 VY CMa 338 1.1 0.16 11 VV Cep 45 0.86 0.013 0.9 --------------------------------------------------------------- Proper motions: Quasars behind the MC also provide astrometric reference for measurements of proper motion (see prop. on background QSOs). ALMA will have sufficient sensitivity at mm and submm wavelengths for direct measurements of stars in the MC. It may also be possible to achieve better astrometric precision on both MC stars and background quasars than is possible with optical techniques. Needless to say, measurement of proper motions in the MC will be an important step in a more accurate calibration of the first step in the cosmological distance ladder (Anguita, Loyola, \&\ Pedreros et al. 2000 and references therein). Measurements of such proper motions are also important for studying the internal dynamics of the LMC and SMC and the dynamics of the Magellanic Stream and Local Group. Systemic proper motions for the MC are expected to be of the order of a few milliarcsecond per year. With a beam of 16 mas we expect the positional accuracy to be at least 5 times better than that - enough to detect proper motion in a year or two. 3. Number of sources: 100 4. Coordinates: 4.1. 60 sources in 30 Doradus and N159, LMC (RA=05h40m, DEC=-69d) 40 sources in the SMC (RA=01h, DEC=-73d) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.0018" (in 2003: 0.016" but cannot be reached now) 5.2. Range of spatial scales/FOV: At 250 GHz (Band 6) the field-of-view is about 35" 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 250 GHz 6.1. Receiver band: Band 6 6.2. Lines: - Frequency: 6.3. Spectral resolution (km/s): - 6.4. Spectral coverage (km/s or GHz): - 7. Continuum flux density: 7.1. Typical value: 0.014-1 mJy 7.2. Continuum peak value: 7.3. Required continuum rms: 0.014 mJy 7.4. Dynamic range in image: 8. Line intensity: 8.1. Typical value:- 8.2. Required rms per channel: - 8.3. Spectral dynamic range: - 9. Polarization: no 10. Integration time per setting: 2 hrs (In 2003: 1 hr) 11. Total integration time for program: 100x2 hr=200 hrs repeat at end of three year period - add on another 200 hrs. ********************************************************** -------------------------------------------------- Review v2.0: 1. Name: The photospheres and proper motions of normal stars Authors: Black, Aalto et al DRSP2.0 Review Leonardo Testi: Why 250GHz? Most probably is the best tradeoff between sensitivity and angular resolution? Time estimate is uncertain, but we can have this program as baseline with 200hrs for the time being. ===================================================================================== DRSP 3.2.5 Title Millimeter observations of nonthermal emission from active stars Pi R. A. Osten Time 36 hrs 1. Name of program and authors "Millimeter observations of nonthermal emission from active stars" R. A. Osten 2. One short paragraph with science goal(s) This is a project to investigate the high frequency (86--116 GHz) end of the nonthermal electron distribution which manifests itself at centimeter wavelengths. These high frequencies will probe the most energetic electrons, where optically thin coronal conditions are expected. There will be a search for time variability, from minute timescales to longer. Previous observations of energetic flares from 5--40 GHz with the VLA (Bastian, unpublished) have shown a rising spectrum up to 40 GHz (with flux densities of order a few hundred mJys). Recently (Brown & Brown 2006, ApJ 638, L37) reported a large mm flare on an active binary at a frequency of 99 GHz with OVRO. Solar flare observations at mm wavelengths have cemented the relationship between these energetic particles and nonthermal hard X-ray emissions; stellar radio (cm and mm wavelengths) remain the most sensitive means of detecting these particles, and studying their dynamics. Observations at two frequencies, both of which are optically thin to gyrosynchrotron emission (86 and 116 GHz), can cement the index of the power-law electron distribution, a key component to beginning to understand the energetics of particle acceleration in non-solar stellar flares. The sample has been chosen to contain both active evolved stars and active dwarf stars; their properties at cm-wavelengths and X-ray wavelengths appear to be similar, implying a similarity in some fundamentals of coronal heating and nonthermal emission; this investigation will extend to the highest energy electrons currently detectable. In a sense this proposal could be split into two parts: a first one concentrating on detections (which can be done quickly given ALMA's sensivities) and a second one focussing on the detected objects to look for variability. 3. Number of sources (e.g., 1 deep field of 4'x4', 50 YSO's, 300 T Tauri stars with disks, ...; do NOT list individual sources or your "pet object", except in special cases like LMC, Cen A, HDFS) Radio bright, active stars distributed among three classes: (1) active binary systems with at least one evolved component (HR 1099, UX Ari, II Peg, sigma Gem), (2) single active dwarf stars (AD Leo, UV Cet, YZ CMi), and (3) single active evolved stars (FK Com, HD 32918). Total of 9. 4. Coordinates: 4.1. Rough RA and DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 30 in Lupus) Indicate if there is significant clustering in a particular RA/DEC range (e.g., if objects in one particular RA range take 90% of the time) HR 1099: 03 34 +00 25 UX Ari: 03 23 +28 32 II Peg: 23 55 +28 38 sigma Gem: 07 43 +28 53 AD Leo: 10 16 +20 07 UV Cet: 01 36 -18 12 YZ CMi: 07 42 +03 40 FK Com: 13 30 +24 13 HD 32918: 04 58 -75 16 4.2. Moving target: yes/no (e.g. comet, planet, ...) no 4.3. Time critical: yes/no (e.g. SN, GRB, ...) yes, need accompanying cm-wavelength observations. 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution (arcsec): pt. src. 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 5.3. Required pointing accuracy: (arcsec) 1 6. Observational setup 6.1. Single dish total power data: no/beneficial/required no Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no/beneficial/required no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no/beneficial/required no 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no no 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9 3, would like to be able to sample the low and high ends of this band simultaneously 7.2. Lines and Frequencies (GHz): (approximate; do _not_ go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify, e.g., "6 frequency settings in Band 3". Apply redshift correction yourself.) 7.3. Spectral resolution (km/s): n/a 7.4. Bandwidth or spectral coverage (km/s or GHz): few GHz 8. Continuum flux density: 8.1. Typical value (Jy): We expect a range from the tens of microJys to $>$ 100 mJy during major flares depending on the variability seen. As an example, extrapolating from the 15 GHz detection of EV Lac (dM3e; similar spectral type to the flare stars listed above) of Osten et al. (2006 ApJ 647, 1349) to 86 GHz using alpha=-0.55 gives an expected 86/116 GHz flux of 130/110 microJy. (take average value of set of objects) (optional: provide range of fluxes for set of objects) 8.2. Required continuum rms (Jy or K): To establish detections at the 8 sigma level, need 1 sigma rms of 15 microJy for the example given above. This can be achieved in 600 seconds. To establish variations of spectral index within flaring events, need 1 sigma rms of 50 (120) microJy, which can be achieved in 60 s at 86 (116) GHz. Note the observation will be longer than this. 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) >8 8.4. Calibration requirements: absolute ( 10% ) repeatability ( 5% ) relative ( 1-3% ) 9. Line intensity: 9.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10. Polarization: yes/no (optional) yes 10.1. Required Stokes parameters: I,V 10.2. Total polarized flux density (Jy): Expected Stokes V flux varies; percent circular polarization probably low, <10%. 10.3. Required polarization rms and/or dynamic range: Using example above, to detect 10% circular polarization with flux density (I) of 130 microJy requires 1 sigma rms of 4 microJy for a 3 sigma detection. This can be done in 2 hours. 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): for detections in total intensity: 0.17 hour (10 min.) for detections of circular polarization: 2 hours 12. Total integration time for program (hr): For detection phase of program, 2hrs x 9 sources = 18 hours. Additional time will be requested to pursue variability of detected sources. Assume four of the sources show strong (>20 sigma) detections, and follow each source for 5 hours. 4 x 5 = 20 hours. Total time =18+20 =36 hours. 13. Comments on observing strategy : (optional) For monitoring variability, we would observe in two sub-arrays, one using frequencies near 86 GHz and the other with frequencies near 116 GHz. (e.g. line surveys, Target of Opportunity, Sun, ...): -------------------------------------------------- Review v2.0: 1. Name of program and authors "Millimeter observations of nonthermal emission from active stars" R. A. Osten DRSP2.0 Review Leonardo Testi: ok with main driver for time from variability. Are there requirements for the time separation between observations at 86 and 115 GHz (cannot be observed simultaneously)? Why is single dish and ACA required? Which are the angular resolution and maximum angular scales requested for this programme? Reply: The 86 and 115 GHz observations should be performed simultaneously. ACA and single dish data are not required. These are point sources, in fields which are not confused, so there are no stringent constraints on angular resolution or maximum angular scale. For the active binaries, the orbital separation is only a few mas. ===================================================================================== DRSP 3.2.6 Title Millimeter survey of stellar disk emission from late-type giants and supergiants Pi R. A. Osten Time 3.5 hrs 1. Name of program and authors "Millimeter survey of stellar disk emission from late-type giants and supergiants" R. A. Osten 2. One short paragraph with science goal(s) The VLA resolved the supergiant Betelgeuse (Alpha Ori) at 7mm, providing crucial measurements for refining atmospheric models and investigating mass loss mechanisms in late-type stars. Sensitive measurements of the mm fluxes from such stars, combined with superb spatial resolution, will reveal intensity asymmetries and make vast improvements in the current spherically symmetric atmospheric models. This project is a survey of M supergiants and K giants, which show predominantly wind emission. Each object will be observed twice, separated by at least one month, to check for any mm variability (several objects show evidence of variability at cm wavelengths). This will provide some constraints on stellar pulsations and dust shell emission. 3. Number of sources (e.g., 1 deep field of 4'x4', 50 YSO's, 300 T Tauri stars with disks, ...; do NOT list individual sources or your "pet object", except in special cases like LMC, Cen A, HDFS) 20 4. Coordinates: 4.1. Rough RA and DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 30 in Lupus) scattered in RA and DEC 4.2. Moving target: yes/no (e.g. comet, planet, ...) no 4.3. Time critical: yes/no (e.g. SN, GRB, ...) no 5. Spatial scales: 5.1. Angular resolution (arcsec): 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 5.3. Single dish total power data: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3, 6, 7, or 9 band 3 and 6 6.2. Lines and Frequencies (GHz): 6.3. Spectral resolution (km/s): 6.4. Bandwidth or spectral coverage (km/s or GHz): few GHz at each end of the band 7. Continuum flux density: 7.1. Typical value (Jy): tens of mJy 7.2. Required continuum rms (Jy or K): 20 micro Jy 7.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether e.g. weak objects next to bright objects) >10 8. Line intensity: 8.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) 8.2. Required rms per channel (K or Jy): 8.3. Spectral dynamic range: 9. Polarization: yes/no (optional) no 9.1. Required Stokes 9.2. Total polarized flux density (Jy) 9.3. Required polarization rms and/or dynamic range 9.4. Polarization fidelity 10. Integration time for each observing mode/receiver setting (hr): 5 minutes per target will give 1 sigma sensitivities of 20 microJy 11. Total integration time for program (hr): 20 targets, each observed twice for 5 minutes: 3.5 hours (plus calibration) 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): (optional) ************************************************************************** Review Leonardo Testi: merge with 3.2.3 Comment Ewine: keep as separate for the moment; representative small program -------------------------------------------------- Review v2.0: 1. Name of program and authors "Millimeter survey of stellar disk emission from late-type giants and supergiants" R. A. Osten DRSP2.0 Review Leonardo Testi: ===================================================================================== DRSP 3.2.7 Title Flares from Young Stellar Objects: What we learned from 2003 January flare in GMR-A Pi R.S.Furuya Time 96 hrs 1. Name: Flares from Young Stellar Objects: What we learned from 2003 January flare in GMR-A Authors: R.S.Furuya (Caltech) Ref. Furuya et al. 2003, PASJ, 55, L83 2. Science goal: 1) To have better understanding of magnetically induced stellar surface activities in young stellar objects (YSOs) 2) To test validity of MHD magnetic reconnection models 3. Number of sources: ~10-100 (For Orion, see Sec.3.7 of Bower et al. 2003, in press) 4. Coordinates: 4.1. 100 sources distributed over sky (RA=any, DEC=any visible) Nearby (<450 pc) stellar clusters (e.g., Orion/Chameleon/Ophiucus/Serpens etc) 4.2. Moving target: no 4.3. Time critical: yes Time resolution : Ideally the same as those of X-ray satellites, Minimum requirement is 10 sec cf. In the GMR-A flare, shorter time variation than 15-min was detected. We think that 15-min was the upper limit from the sensitivity of the present millimeter array. a) Simultaneous observations with cm radio interferometers (e.g., E-VLA, ATCA) and X-ray satellites are essential to investigate physical properties of the flare. b) Perform monitor of IR flux is essential to identify whether the flaring object is star or background object (e.g., AGN). IR flux of the flare star is expected not to be time variable. c) Preferably with simultaneous observations VLBA/SKA because some classes of sources which are known to show flare activities are close binaries (e.g., RS CnV binaries, FK Comae(Giants) ) Monitoring period : < A few weeks cf. In the GMR-A flare, the overall flare activity lasted at least 13 days. 5. Spatial scales: 5.1. Angular resolution: <0.1" (ideally 0.01") - To have better estimate of flare's size scale, higher angular resolution is preferable. cf. Flare's size scale approx.= Time scale x Alfven velocity ~ (<)a few x 0.1 day x 0.05 c ~< a few x 0.9 AU ==> a few x 2 milliarcsecond (mas) @ d=450 pc a few x 7 mas @ d=130 pc ==> Comparable size scale to the highest 0.01" beam 5.2. Range of spatial scales/FOV: point source 5.3. Single dish: N/A 5.4. ACA: N/A 5.5. Subarrays: yes, To perform simultaneous multi-wavelengths observations Example Since it takes at least 1.5 second to switch to another band + time for calibration, we propose to divide the whole 64 element telescopes to 2-4 subarrays to observe 2-4 bands simultaneously with few second integration times. 6. Frequencies: 6.1. Receiver band: Minimum requirements : Bands 3, 6, and 7 Preferable-1 : Bands 1 and 2 Comments-1 : Since the turn over frequency of the 2003 January flare on GMR-A was estimated to be higher than 100 GHz at the flare peak phase, Bands 1 and 2 data would be important to the shift of turn over frequency as the flare decays Preferable-2 : Bands 9 (602-720 GHz) and 10 (787-950 GHz) Comments-2 : Analogous from solar flares observed at 212/405 GHz (Kaufman et al. 2002, ApJ 574, 1059), these high frequency flux measurements would be important to give constraints on flare decay models 6.2. Line: To be considered (not relevant for this proposal) 6.3. Spectral resolution (km/s): N/A 6.4. Spectral coverage (km/s or GHz): N/A 7. Continuum flux density: 7.1. Typical value: quiescent phase < 1 mJy 7.2. Continuum peak value: expected peak in flaring phase ~ order of 100 mJy 7.3. Required continuum rms: <100 micro Jy/beam with 10-sec integration at 100 GHz 7.4. Dynamic range in image: Ideally >10 with 2-sec integration 8. Line intensity: 8.1. Typical value: N/A 8.2. Required rms per channel: N/A 8.3. Spectral dynamic range: N/A 9. Polarization: Yes Measuring stokes I, Q, U, V fluxes are essential to determine emission mechanism ((gyro)synchrotron emission is expected). 10. Integration time per setting: For 10 seconds integration time, the sensitivities for the full array are: 90 230 345 650 GHz 0.10 0.25 0.47 2.5 mJy Even with factor ~4 reduction in sensitivity for subarrays, this appears sufficient if the source is flaring. At 650 GHz, longer integrations are needed in the quiescent state. It is assumed that data will be recorded on 1-2 second timescales. Strategy would be to select a ~2'x2' field in e.g. Orion cluster (or Serpens/Chameleon) containing of order 10 sources and monitor it with mosaicking for 4 hrs per day for 12 days at 90 and 230 GHz. If flaring source is detected, more continuous monitoring with high time resolution and all four bands will be proposed as TOO for a period of 2 weeks. 11. Total integration time for program: Step 1: 2'x2' field 4x12 hrs = 48 hrs Bands 3 and 6 Step 2: Follow-up TOO: 48 hrs Bands 3, 6, 7 and 9 ************************************************************************ Comment Ewine: proposal discussed and iterated with author; latest version dd. December 17. -------------------------------------------------- Review v2.0: 1. Name: Flares from Young Stellar Objects: What we learned from 2003 January flare in GMR-A Authors: R.S.Furuya (Caltech) Ref. Furuya et al. 2003, PASJ, 55, L83 DRSP2.0 review Leonardo Testi: ok, interesting case for science subarraying with (relatively) bright targets. ===================================================================================== DRSP 3.2.8 Title TOO Observations of Energetic Particles in Stellar Superflares Pi R. A. Osten Time 2 hrs 1. Name of program and authors TOO Observations of Energetic Particles in Stellar Superflares R. A. Osten S. Drake 2. One short paragraph with science goal(s) The recent detection of nonthermal hard X-ray emission from a stellar superflare (Osten et al., astro-ph/0609205) has made possible the study of energetics of accelerated particles during stellar flares. This is a project to investigate the time and spectral variability of the MeV particles which produce optically thin gyrosynchrotron emission at mm wavelengths. Simultaneous observations of the ~100 keV electrons producing the hard X-ray emission will be obtained through the use of triggered observations from an appropriate spacecraft (e.g. Swift). Comparison of the spectral index from radio observations and the spectral index derived by analysis of hard X-ray spectra will allow an investigation into whether there is a change in the distribution of electrons at these energies; their joint time variations can also be used to diagnose magnetic trapping and precipitation from the trap. 3. Number of sources (e.g., 1 deep field of 4'x4', 50 YSO's, 300 T Tauri stars with disks, ...; do NOT list individual sources or your "pet object", except in special cases like LMC, Cen A, HDFS) Initially, only two triggers will be requested. Sample includes all nearby active stars capable of producing stellar superflares. 4. Coordinates: 4.1. Rough RA and DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 30 in Lupus) Indicate if there is significant clustering in a particular RA/DEC range (e.g., if objects in one particular RA range take 90% of the time) distributed in RA and DEC 4.2. Moving target: yes/no (e.g. comet, planet, ...) no 4.3. Time critical: yes/no (e.g. SN, GRB, ...) yes, TOO 4.4. Scheduling constraints: (optional) need rapid response (<0.5 hour) to get on source and take data. 5. Spatial scales: 5.1. Angular resolution (arcsec): pt. src. 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 5.3. Required pointing accuracy: (arcsec) 1 6. Observational setup 6.1. Single dish total power data: no/beneficial/required no Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no/beneficial/required no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no/beneficial/required no 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no no 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8, or 9 3 7.2. Lines and Frequencies (GHz): (approximate; do _not_ go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify, e.g., "6 frequency settings in Band 3". Apply redshift correction yourself.) 7.3. Spectral resolution (km/s): n/a 7.4. Bandwidth or spectral coverage (km/s or GHz): few GHz 8. Continuum flux density: 8.1. Typical value (Jy): Based on extrapolations from SXR-microwave relations for active stars (Guedel & Benz 1993 ApJ 405, L63) we expect cm-wavelength fluxes to be several hundred mJy. Extrapolating to mm wavelengths with spectral index of -3, expected for a very soft electron distribution (and thus somewhat pessimistic, as solar flares and the nonthermal hard X-ray detection of a stellar flare indicate harder distributions), leads to expected flux densities of ~100 microJy or larger. More optimistic values assume alpha=-1.3, with extrapolated flux then ~5 mJy. (take average value of set of objects) (optional: provide range of fluxes for set of objects) 8.2. Required continuum rms (Jy or K): For the numbers given above, a detection can be achieved at the > 5$sigma$ level with 20 microJy rms. 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) >5 8.4. Calibration requirements: absolute ( 10% ) repeatability ( 5% ) relative ( 1-3% ) 9. Line intensity: 9.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10. Polarization: yes/no (optional) yes 10.1. Required Stokes parameters: I,V 10.2. Total polarized flux density (Jy): unknown, likely small (<10% Stokes I). Circular polarization at cm wavelengths in stellar flares is typically less than what is seen during quiescence, and we assume the same behavior here. 10.3. Required polarization rms and/or dynamic range: Unless polarization is larger than V/I =10% (or flare is brighter than minimum predicted flux), this will not be feasible within the 1 hour time frame. For 1 sigma rms similar to Stokes I, V/I can be constrained to <60% (3 sigma) for the pessimistic case, or <1\% for the more optimistic case. 10.4. Polarization fidelity: don't expect any linear polarization, but polarization leakage should be small. 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): Follow the source for an hour. Detection can be achieved in about 5 minutes (or less, for the more optimistic scenario), allowing for a study of temporal change in spectral index. This timescale is not set by ALMA's sensitivity constraints, but rather by the intrinsic properties of stellar flares. The activation phase of the flare, when particle acceleration is most important, can last for tens of minutes. 12. Total integration time for program (hr): Two triggers, one hour each trigger, total=2 hr 13. Comments on observing strategy : (optional) Target of Opportunity proposal, requiring rapid turn-around time. (e.g. line surveys, Target of Opportunity, Sun, ...): -------------------------------------------------- Review v2.0: 1. Name of program and authors TOO Observations of Energetic Particles in Stellar Superflares R. A. Osten S. Drake DRSP2.0 Review Leonardo Testi: Interesting Rapid Response ToO. Only one frequency required? May be feasible to sacrify some sensitivity in favour of simultaneous multifrequency observations. e.g. 2 subarrays of 25 antennas observing at 100 and 140 (bands 3 and 4) could achieve ~0.05mJy rms in 5 minutes. If sources are bright enough, otherwise it may require coordination with longer wavelength facility (I assume that the radio spectral index is an interesting quantity here). Reply: Yes, spectral index is an interesting quantity. I assumed, but did not state explicitly, that coordination with cm-wave facility would describe emission at lower frequencies. We have such a TOO program at the VLA now. Splitting the ALMA observations into two subarrays is interesting, but will depend on the sources being bright. While large radio flares from active stars have produced significant (>100 mJy) flux at mm wavelengths, it is unknown at this point what the response in the mm region would be from a superflare diagnosed from X-ray observations. Based on the L_X/L_R relation (Gudel & Benz 1993 ApJ 405, L63) we expect that there would be large enhancements. For now, we will leave the proposal as having coordination with cm-wave facilities to provide the spectral index constraints, but a future proposal might want to pursue the sub-array capabilities of ALMA for spectral index measurement, based on experience with high-frequency stellar flare behavior. ===================================================================================== DRSP 3.2.9 Program: Using ALMA to probe active regions in Sun like stars PI: G. Hussain Time: 60 hrs 2. One short paragraph with science goal(s) Using the polarization capabilities of ALMA, we will measure the magnetic fields in flaring coronal loops. These measurements will provide key information about the sizes of stellar coronae and their geometries. These observations will constrain 3D coronal models. We request observations of six nearby active stars over 10 hour timeperiods to follow the evolution of flares. 3. Number of sources Six nearby active stars 4. Coordinates: 4.1. Rough RA and DEC unknown 4.2. Moving target: no 4.3. Time critical: yes (?) 4.4. Scheduling constraints: none 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.1'' 5.2. Range of spatial scales/FOV (arcsec): 10'' 5.3. Required pointing accuracy: (arcsec) N/A 6. Observational setup 6.1. Single dish total power data: no Observing modes for single dish total power: 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5 7.2. Lines and Frequencies (GHz): 100,150, 190 7.3. Spectral resolution (km/s): N/A 7.4. Bandwidth or spectral coverage (km/s or GHz): 8 GHz 8. Continuum flux density: ? 8.1. Typical value (Jy): ? (take average value of set of objects) (optional: provide range of fluxes for set of objects) 8.2. Required continuum rms (Jy or K): 0.1 mJy assuming the full 8 GHz bandwidth: at 100 GHz, to get the required rms, it would take 27 seconds on source at 150 GHz, to get the required rms, it would take 46 seconds on source at 190 GHz, to get the required rms, it would take 22005 seconds on source (since there are only 5 antennas with band 5 receivers) 8.3. Dynamic range within image: ? 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 9. Line intensity: NA 9.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10. Polarization:yes 10.1. Required Stokes parameters: ? 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 10 hours per source (6 sources) at 100 GHz, the sample rate could be as high as a minute? at 150 GHz, the sample rate could be as high as 90 seconds? (do they have to have the same time resolution? because then the rms noises would be different) 12. Total integration time for program (hr): 60 hr 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): ===================================================================================== DRSP 3.3.1 Title Probing the Dust Formation Zone around Red Giant Stars Pi K. M. Menten Time 200 hrs 1. Project: Probing the Dust Formation Zone around Red Giant Stars =================================================================== 1. Name of program: Probing the Dust Formation Zone around Red Giant Stars Authors Karl M. Menten 2. Science goal(s) The closest vicinity of an O-rich red giant star has roughly the following radial structure: Region Outer diameter T n Resolved by (AU)(mas@200pc) (K) (cm^3) Optical photosphere: 4 20 2400 2E+14 IR interferometry chromosphere: 5 25 2000* 5E+13 --- molecular photosphere: 6 30 1600 1E+12 IR interferometry (e.g. TiO) radio photosphere: 8 40 1500 1E+11 VLA SiO masers: 12 60 1300 1E+10 VLA, VLBI dust formation: > 12 60 1200 3E+09 IR interferometry and molecular depletion * The chromosphere's temperature is highly inhomogeneous with shocks creating partially much higher temperatures). (see Fig 12 of Reid & Menten (1997, ApJ, 476, 327 ; hereafter RM97) ---- So far the ONLY information on densities and temperatures in this important region in which molecules condense into dust grains comes from models of SiO maser emission, and is, thus, quite uncertain. In C-rich stars, similar scales are probed by HCN masers, as well as by (probably) quasi-thermal vibrationally excited HCN emission. Again, such observations are difficult to interpret. Plateau de Interferometry of the low-lying SiO (2-1) transition from the vibrational ground state by Lucas et al. (1992, A&A, 262, 491) has revealed SiO emission regions with (brightness) temperatures between a few and several 100 K and sizes of 40 - 400 AU, much larger and cooler than the SiO maser regions and definitely outside of the dust formation zone. The inescapable conclusion is that enough SiO survives depletion to still produce extended, optically thick emission. Because their emission is optically thick, low excitation lines will do little to probe the inner region. For example, the critical density of the 694.3 GHz 16-15 SiO line (which is 250 K above ground) is 1000 times higher than that of the 2-1 line and thus samples 10^8 - 10^9 cm-3 gas, approaching the densities in the dust formation zone. Observations at the highest ALMA resolution are easily possible, since continuum emission in all frequency bands can , as explained in sect. x.x of this document, be used for self calibration and, also, will provide the exact stellar position as a reference point. 3. Number of sources: Numbers of stars per kpc^3 (Jura & Kleinmann 1992, ApJS, 79, 105 All carbon 100 "Very dusty carbon" 30 S-type 30 O-rich miras (300100 8. Line intensity: 8.1. Typical value: 5-500 K for the inner layers of AGBs (angular scales 0.05"-1" for IRC+10216) 8.2. Required rms per channel: 1 K for observations of the inner layers. Better than 0.05 K for the external layers (structures resolved with the 30m; cold gas) 8.3. Spectral dynamic range: 3 (for species which are barely detected) >100 (for brightest lines) 9. Polarization: Yes, for paramagnetic molecules formed in the zone of a few stellar radii around the star. Yes, for masers (HCN, H2O,...) 10. Integration time per setting: 10 min/Bd 3, 20 min/Bd 6 30 min/Bd 7, 9 - for 0.3 arcsec resolution and 0.2-0.3 k (1 sigma) sensitivity 11. Total integration time for program: 6 x 60 x 10m : 60 h Band 3 6 x 64 x 20m: 128 h Band 6 6 x 95 x 30m: 285 h Band 7 6 x 69 x 30m: 207 h Band 9 ------------------------------------------- 680 h total ***************************************************************************** Review Peter Schilke: Both scientifically very convincing and technically well constructed proposal. The source list could be commented on a bit further, but that's a detail. The observing time is well justified and reasonable. -------------------------------------------------- Review v2.0: 1. Name: Line surveys in evolved stars DRSP 2.0 Reviewer Leonardo Testi: Nothing to add wrt previous review. Well developed program ===================================================================================== DRSP 3.3.3 Title Resolving the Molspheres of M supergiants Pi G. Harper Time 18,4 hrs 29 September 2006 1. Name of program and authors Resolving the Molspheres of M supergiants Graham Harper Colorado gmh@casa.colorado.edu Alexander Brown Colorado ab@casa.colorado.edu Matthew Richter California richter@physics.ucdavis.edu Nils Ryde Uppsala ryde@astro.uu.se Takashi Tsuji Tokyo ttsuji@ioa.s.u-tokyo.ac.jp Keiichi Ohnaka Bonn kohnaka@mpifr-bonn.mpg.de Rachel Osten GSFC rosten@milkyway.gsfc.nasa.gov 2. One short paragraph with science goal(s) Multi-wavelength and very high spatial-resolution continuum observations with ALMA will resolve nearby M supergiant MOLspheres, the quasi-static dynamically detached molecular envelopes that may be the formation site for nascent dust. These observations will map the temperature and density structure in the MOLspheres and thereby provide constraints on unknown mechanisms that control the atmospheric energy and momentum balance. These observations will also empirically constrain the wavelength dependence of silicate dust emissivity by separating the stellar and optically thin envelope contributions. ALMA will make a unique contribution to the study atmospheres surpassing the spatial resolution of HST UV observations that sample the same spatial regions. 3. Number of sources 3 stellar systems with a field of view < 25''x25'' 4. Coordinates: 4.1. Rough RA and DEC RA DEC Betelgeuse (M2 Iab) 05 55 10 +07 24 25 Antares (M1 Iab + B4 V) 16 29 25 -26 25 55 alpha Her (M5 II + ) 17 14 39 +14 23 25 4.2. Moving target: no 4.3. Time critical: no (unless we coordinate with other observatories) 4.4. Scheduling constraints: The different frequency bands should be observed as close together in time as possible to avoid interpretation complications resulting from stellar variability 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.006-0.090 5.2. Range of spatial scales/FOV (arcsec): 0.006 - 25.000 scales reflect highest possible resolution of stellar source optional: single-field 5.3. Required pointing accuracy: 0.6 (arcsec) 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: on-the-fly mapping 6.2. Stand-alone ACA: beneficial 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3, 4, 6, 7, 8, and 9 7.2. Lines and Frequencies (GHz): maximum transmission for each band - see highest continuum sensitivity 7.3. Spectral resolution (km/s): N/A 7.4. Bandwidth or spectral coverage (km/s or GHz): 8 GHz 8. Continuum flux density: 8.1. Typical value (Jy): Average total system fluxes (unresolved) 350 GHz 0.3 Jy 666 GHz 0.9 Jy 8.2. Required continuum rms (Jy or K): Criterion S/N of 10 at 2nd peak in visibility. Use model of Harper, Brown and Lim (2001 ApJ 551, 1073) For Betelgeuse 0.1*(2nd vis. peak) are mJy GHz Band 3: 1.4 100 Band 4: 2.2 150 Band 6: 3.2 250 Band 7: 5.1 350 Band 8: 7.1 400 Band 9: 15.1 660 8.3. Dynamic range within image: weakly resolved source in clear field (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) 8.4. Calibration requirements: absolute ( 5%) repeatability ( 1-3%) relative ( 1-3%) 9. Line intensity: N/A 9.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10. Polarization: No 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): Assumes a factor of two overhead for fast switching. GHz hrs Band 3: 100 0.8 + 1.0 Band 4: 150 0.8 + 1.0 Band 6: 250 2.0 + 1.0 Band 7: 350 2.4 + 1.0 Band 8: 400 2.4 + 1.0 Band 9: 660 4.0 + 1.0 For the on-the-fly mapping we assume 20 min per star, per band, for one telescope. 12. Total integration time for program (hr): 18.4 hours 13. Comments on observing strategy : (optional) To obtain the highest spatial resolution with as wide a range of observing frequencies as possible, and to obtain the total system flux on spatial scales larger than the array FOV. Use maximum bandwidth to observe the stellar thermal continuum emission for maximum sensitivity. Each source should be observed at as many frequencies as possible at the same time to avoid interpretation problems causes by source variability. In addition to observing the highest frequencies in "best weather", this will/may require that the lower frequencies also be observed under "best weather" conditions. Preferably the observations should be obtained within a couple of days, and not more than a week. We will make preparatory observations with CARMA and APEX to examine the dust structure outside the narrow ALMA interferometer FOV, which will lead to more reliable time estimates for the on-the-fly mapping. -------------------------------------------------- Review v2.0: Resolving the Molspheres of M supergiants Graham Harper Colorado gmh@casa.colorado.edu Alexander Brown Colorado ab@casa.colorado.edu Matthew Richter California richter@physics.ucdavis.edu Nils Ryde Uppsala ryde@astro.uu.se Takashi Tsuji Tokyo ttsuji@ioa.s.u-tokyo.ac.jp Keiichi Ohnaka Bonn kohnaka@mpifr-bonn.mpg.de Rachel Osten GSFC rosten@milkyway.gsfc.nasa.gov DRSP 2.0 Review Leonardo Testi: I am not familiar with this science, so it is difficult for me to figure out exactly what is needed here. So it is not clear to me why all frequencies are required and why for all of them the full range of resolutions is necessary. At the low frequencies t will not be possible to obtain the 0.006 arcsec resolution, thus it will not be possible to obtain temperature and density maps at this resolution. If the goal is to compute these maps, then one should probably limit to a lower resolution (which will also be less demanding at the highest frequencies). Presumably OTF total power mapping will be required only for band 8 and 9 (given the primary beam size at lower frequencies). It is not clear to me whether the correct range of configurations (to cover the range of resolutions) have been considered in the computation of the observing times. I have some problems in figuring out the computation for the integration times. If the sensitivity is to be computed for individual (u,v) points (2 antennas) at the second visibility peak as mentioned, then in 1hr (with no overheads) at 660 GHz I only get a S/N=3 (sort of) for 15 mJy. ...There is something I did not understand. R.: The proposed observations of M supergiants make major demands on the proposed capabilities of ALMA, both in terms of available bandwidth and spatial resolution, and this is why we have submitted this DRSP2.0. Below we provide supplemental text to help clarify the project for the reviewers. Note on the exposure times (last comment in review): The thermal continuum emitting source of the M supergiant can be characterized as a disk with diffuse edges because the density scale heights are small compared to the stellar radius, and the visibilities reflect this. We require for each relevant antenna pair a S/N of 10 at the 2nd peak of the visibility curve. In section 8.2 we listed the flux at 1/10 of the 2nd peak, i.e. the required 1 sigma. For the example given by the reviewer: at 660 GHz the 2nd peak has a estimated flux of 150 mJy and 1/10 of this is 15 mJy. Using the ALMA Sensitivity Calculator it takes 600 sec (10 mins) to achieve a 1 sigma (with default parameters) of 15.1 mJy. This is 1/10 of the 2nd Peak, and so a S/N=10. If this interpretation of the sensitivity tool is incorrect please let us know and we will modify accordingly. ===================================================================================== DRSP 3.4.1 Title Post-AGB Stars: proto-planetary and planetary nebulae Pi P. Cox Time 238 hrs Project: Post-AGB Stars: proto-planetary and planetary nebulae ================================================================== 1. Name of program and authors Probing the physical and chemical properties of proto-planetary nebulae Authors: Pierre Cox 2. Science goal(s) The physical mechanisms which govern the evolution of proto-planetary nebulae (PPNe) are poorly documented because relatively few objects are known to be in this rapid transition between the AGB and planetary nebula phase. The role played by high-velocity winds which interact with the slowly expanding AGB envelope during the PPN phase has been recognized as essential in the shaping of the planetary nebulae. However, the details of the interaction and the precise evolution from the symmetric AGB envelope to the asymmetries which characterize planetary nebulae are still not well understood. The rapid erosion of the AGB envelope through multiple high-velocity outflows and UV photons is not only structural but is also reflected in the unusual rich chemistry observed in PPN. In the inner zones, the UV photons from the central star photodissociate the molecular species produced during the AGB phase initiating a chemistry which is radically different from the AGB photochemistry and is now dominated by ion-neutral reactions. Such reactions allow the formation of O-bearing molecules in the inner regions of carbon-rich environments, including water and OH. The effect of the UV radiation on the acetylene and methane, which are still available in the gas phase, can produce new hydrocarbons, including benzene as observed in CRL618. The main goals of the program are to observe all know PPN accessible from the sourthern skies, in order to improve our knowledge on the mechanisms responsible for the onset of high-velocity winds after the AGB phase, probe the inner dense regions of PPN, which trace the last mass-loss event of the AGB phase, and to study the unusual chemistry by obtaining line surveys of a few sources. 3. Number of sources: 16 PPN observable in the southern hemisphere (from catalogue of Bujarrabal et al. 2001) 4. Coordinates and expected fluxes (examples with measured radio data): 4.1 Rough RA and DEC Name RA Dec (J2000.0) Frosty Leo 09:39:54.0 11:58:54 He3-1475 17:45:14.1 -17:56:47 IRC+10240 19:26:48.0 11:21:17 IRAS19500-1709 19:52:52.6 -17:01:50 IRAS07134+1005 07:16:10.3 09:59:48 Hen3-401 10:19:32.5 -60:13:29 Robert22 10:21:33.8 -58:05:48 HD101584 11:40:58.8 -55:34:26 Boomerang 12:44:45.5 -54:31:12 He2-113 14:59:53.5 -54:18:08 Mz-3 16:17:13.6 -51:59:06 M2-9 17:05:37.9 10:08:32 CPD-568032 17:09:00.9 -56:54:48 IRAS17150-3224 17:18:19.7 -32:27:21 OH17.7-2.0 18:30:30.7 -14:28:57 R Sct 18:47:29.0 -05:42:19 4.2. Moving target: yes/no (e.g. comet, planet, ...) no 4.3. Time critical: yes/no (e.g. SN, GRB, ...) no 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.10-0.20 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) Most sources have sizes of about 20 arcsec. 5.3. Single dish total power data: yes/no no 5.4. ACA: yes/no no 5.5. Subarrays: yes/no no 6. Frequencies: 6.1. Receiver band: Bans 3 Band 6 Band 7 Band 9 6.2. Lines and Frequencies (GHz): multi-line: with multi (TBD) freqency settings. 6.3. Spectral resolution (km/s): 1-3 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 100 to 500 km/s 7. Continuum flux density: 7.1. Typical value (Jy): a few 10 to 100 mJy 7.2. Required continuum rms (Jy or K): 0.01 Jy 7.3. Dynamic range within image: >100 N/A; no nearby weaker objects expected 8. Line intensity: 8.1. Typical value (K or Jy): The CO lines are normally bright in bright in PPN. The less abundant molecules will have a few K. 8.2. Required rms per channel (K or Jy): 1 K for most of the objects. 8.3. Spectral dynamic range: >100 for brightest lines 9. Polarization: yes for a few sources 10. Integration time for each observing mode/receiver setting (hr): 10 min/Bd 3, 20 min/Bd 6 30 min/Bd 7, 9 - for 0.3 arcsec resolution and 0.2-0.3 K (1 sigma) sensitivity Number of settings per Band will be 10. 11. Total integration time for program: 16 x 10 x 10m : 26 h Band 3 16 x 10 x 20m: 52 h Band 6 16 x 10 x 30m: 80 h Band 7 16 x 10 x 30m: 80 h Band 9 ------------------------------------------- 238 h total ************************************************************************** Review Peter Schilke: High scientific interest. Can certainly lead to a proposal, but isn't really one. There is only a vague idea which and how many lines should be observed, so the time estimate is very uncertain. Line surveys are mentioned in the justification, but there is no time allocated for them in this proposal. The need for the spectral/spatial resolution used isn't justified. Reply Cox: I agree with the remark by Peter re the line survey and a more detailed proposal should indeed be written. For the spectral/spatial resolution requested, the lines can be narrow (in the central regions unaffected by the outflows) so that 1-3 km/s is mandatory. For spatial resolution, sub-arcsecond resolution is needed to study the detailed morphology in poarticular in the central regions. -------------------------------------------------- Review v2.0: 3.4.1 Post-AGB stars: PPN and PN Cox 238 Band 7 and 9 are requested, which have fields of view of 20" and 10" respectively though no single dish/ACA data are required. I think that these datasets for larger sources do in fact need shorter spacings or interpretation could be quite complex. Probably, data in Bands 4, 5, 8 and 10 would be of interest also, though the project was not updated. It is hard to justify as the specifically targeted lines are not detailed although the source list is quite detailed. ===================================================================================== DRSP 3.4.2 Title Molecular and atomic gas in planetary nebulae Pi P. Cox Time 73.2 hrs Molecular and atomic gas in planetary nebulae Authors Pierre Cox 2. Science goal(s) In spite of the wind interaction and the onset of photo-ionization through the post-AGB phase, a significant component of molecular gas is found in many bone fide PNe, even in highly evolved ones such as the Helix nebula. CO and H$_2$ have been detected in more than 50 PNe and other molecular species have been detected in a few PNe indicating an on-going chemistry. In most cases, the molecular gas is found around the waist of the ionized gas in toroid-like shapes and represent a main structural feature of the nebula and an important key to its morphology. In addition to molecular gas, there is evidence for neutral atomic gas in PNe, e.g., from observations of the fine-structure lines of carbon. This gas is at the interface between the molecular and ionized gas, and in envelopes that are essentially completely atomic. The masses in these components are substantial but they have not been studied in large numbers of PNe or at high angular resolution. The detailed structure of the molecular gas in PNe is of great interest since it contains information on the physical processes that produce the nebulae. The molecular gas in PNe is characterized be a high degree of fragmentation. For instance, the envelope of the Helix is found to be made of thousands of small (a few arcsec), dense, i.e. 10(5) cm(-3) clumps slowly evaporating in the radiation of the central white dwarf. The origin of these tiny structures is still debated. Another aspect of the distribution of molecular gas is its global structure which preserves imprints of the early interaction of the envelope with collimated, bipolar outflows or jets just after the AGB phase. The increase in sensitivity and angular resolution provided by ALMA will allow us to study the molecular and atomic gas in many more PNe. In addition, due to its possibility to measure at high frequencies and to its flexibility in frequency set-up, ALMA will open up the exciting possibility to observe at high spatial resolution the warm dense gas as well as the dust continuum in planetary nebulae. The proposed observations will provide key information to further explore the physical and chemical conditions pertaining in the fragmented, neutral equatorial structures which have been only recently realized to be common and important features of planetary nebulae. 3. Number of sources: PN in southern hemisphere, including the Helix due to its proximity (200 pc) will be a prime target to study in detail the properties of the cometary globules. The PN should span the range from young PN to fully developed such as the Helix. Number TBD: should be of order 10 list to be defined 4. Coordinates and expected fluxes (examples with measured radio data): 4.1 Rough RA and DEC Name RA Dec (J2000.0) Helix nebula 22:29;38.7 -20:50:15 4.2. Moving target: yes/no (e.g. comet, planet, ...) no 4.3. Time critical: yes/no (e.g. SN, GRB, ...) no 5. Spatial scales: 5.1. Angular resolution (arcsec): <0.10 5.2. Range of spatial scales/FOV (arcsec): (optional: indicate whether single-field, small mosaic, wide-field mosaic...) The Helix is extended and highly fragmented. mapping of the northern and western ridges of the nebular envelope in the CO(2-1) transition - need of mosaicing (2 x 20 fields at 230 GHz) 5.3. Single dish total power data: yes/no no 5.4. ACA: yes/no no 5.5. Subarrays: yes/no no 6. Frequencies: 6.1. Receiver band: Band 3, Band 6, Band 7, Band 9 6.2. Lines and Frequencies (GHz): Transitions of CO, CN, HCN and HCO+ 6.3. Spectral resolution (km/s): 0.1 (for the Helix nebula) to 1 km/s 6.4. Bandwidth or spectral coverage (km/s or GHz): 10 km/s 9for Helix) to about a 100-200 km/s 7. Continuum flux density: 7.1. Typical value (Jy): (take average value of set of objects) (optional: provide range of fluxes for set of objects) 10 mJy to 1 Jy 7.2. Required continuum rms (Jy or K): 0.01 Jy 7.3. Dynamic range within image: >100 8. Line intensity: 8.1. Typical value (K or Jy): For CO, typically 1 K 8.2. Required rms per channel (K or Jy): of order 0.01 K 8.3. Spectral dynamic range: > 100 (for brightest lines) 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): Per source: 10 min/Bd 3, 20 min/Bd 6 30 min/Bd 7, 9 - for 0.3 arcsec resolution and 0.2-0.3 K (1 sigma) sensitivity Number of settings per Band will be 4. For Helix, mosaic in CO(2-1) of two 100x100 arcsec^2 fields (north and west). 11. Total integration time for program (hr): 10 x 4 x 10m : 6.6 h Band 3 10 x 4 x 20m: 13.3 h Band 6 10 x 4 x 30m: 20.0 h Band 7 10 x 4 x 30m: 20.0 h Band 9 2 x 20 x 1 x 20m: 13.3 h Band 6 ------------------------------------------- 73.2 h total ***************************************************************************** Review Peter Schilke: Scientifically well justified proposal, although I don't understand how one wants to get information of the atomic gas by observing just molecules - atomic carbon in the Japanese extension would be interesting. I am surprised that, for the large-field mosaicing of the Helix, neither ACA nor Single Dish data are needed - are just the clumps interesting? The time estimate is again very sketchy and uncertain. The need for the spectral/spatial resolution used isn't justified. Reply Cox: For the atomic gas, I had in mind the Japanese contribution to study the [CI]. As for the Helix, the molecular emission is indeed concentrated in the small (arcsecond) globules which carry all the molecular mass. There is therefore no need for ACA nor single dish. For the spectral and spatial resolution, the need for high resolution is even more important than in the case of PPN, since the lines are sub-km/s (as in the Helix) and the cometary globules have sizes on the sub-arcsecond scale. The time estimate could be improved indeed. -------------------------------------------------- Review v2.0: 3.4.2 Molecular and atomic gas in PN Cox 73 This project should be updated to include B8 as per the response to referee comments included in the previous DRSP. Would the ~600.2 GHz line of [O II] (2Do-2Do 5/2 - 3/2) be observable? ===================================================================================== DRSP 3.4.3 Title The Heart of Eta Carinae Pi S. M. White Time 1. Name of program and authors: The Heart of Eta Carinae S. M. White, J. Chapman and B. Koribalski 2. One short paragraph with science goal(s) Eta Carinae is a famous southern system consisting of two very massive stars in a 5.5-year-period binary orbit. The primary is a luminous blue variable (LBV) with a mass loss rate of .001 solar masses per year in a wind at 500 km/s. The secondary has never been seen, but is believed to be a very hot luminous star supplying ionizing photons to the dense LBV outflow. The binary orbit is highly elliptical, and every 5.5 years the system undergoes an eclipse in X-rays and radio emission. The millimeter emission from this system consists of many Janskies of (varying) thermal continuum from a subarcsecond-size source together with very strong masing recombination lines. Scientific goals of the millimeter continuum observations will be to resolve the heart of the binary system and study the interaction of the two components and the outflowing gas. At 3 mm wavelengths the smallest structure seems to be about 0.2 arcseconds, but in the higher ALMA bands the optically thick surface in the outflow will be smaller, particularly at the flux minimum at periastron, allowing more detailed mapping of the gas. The strongest masing recombination line is now identified with the "Weigelt blobs", relatively slowly moving dense ejecta with odd ionization states lying outside the binary orbit (by about 0.3 arcseconds) and irradiated by the hot stars. This recombination line maser is very different from the accretion disk maser in MWC 349, and measurements of transitions at different n and their changes with the 5.5 year cycle as the radiation field illuminating the gas changes will allow us to investigate physical conditions in the gas in detail. The non-masing recombination line emission is also strong and can be mapped by ALMA at high spatial resolution over a broad velocity range (hundreds of km/s), allowing us to investigate motions of gas in the outflow from the system with much better spatial resolution than is presently possible. 3. Number of sources: 1 4. Coordinates: 4.1. Eta Carinae - 10:45:03, -59:41 4.2. Moving target: no 4.3. Time critical: yes: the system has a 5.5 year cycle and both continuum and line fluxes and the spatial morphology change by large factors over this timescale. 5. Spatial scales: 5.1. Angular resolution (arcsec): .005" is the size of the binary orbit. The size of the optically thick surface is somewhat larger at lower ALMA frequencies. There is sufficient flux for ALMA to map Eta Car on all spatial scales, although it may be resolved out on the longest baselines, particularly at apastron. We re-emphasize that the relevant angular scales change with orbital phase. 5.2. Range of spatial scales/FOV (arcsec): For the core region a single pointing should be adequate. The spatial scales range from the optically thin outer Homunculus nebula, at 18 arcsec across, through the Little Homunculus, about 3 arcsec across and prominent at microwaves, down to the Weigelt blob separation of 0.3 arcsec and then the binary orbit dimension of 0.005 arcsec. 5.3. Required pointing accuracy: Mosaic should not be needed but high dynamic range imaging will be achieved with Eta Car: the source itself can be used for reference pointing, so no extreme pointing precision is required of the antennas for this project. 6. Observational setup 6.1. Single dish total power data: no 6.2. Stand-alone ACA: beneficial but not necessary 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: beneficial but not necessary 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver bands: all. Source is optically thick so different bands penetrate to different depths in the source. The source flux rises with frequency. 7.2. Lines and Frequencies (GHz): Continuum and recombination lines: there are at most 1 or 2 H-alpha lines per band, so for the purposes of the initial study we can limit ourselves to one per high-priority band: H39a 106.737 GHz H30a 231.901 GHz H26a 353.623 GHz H21a 662.404 GHz 7.3. Spectral resolution (km/s): The narrow masing recombination line is at +60 km/s and is about 20 km/s wide. For it, a resolution of 2 km/s is ultimately desirable. The broad non-masing recombination line from the outflowing gas is known to be over 1000 km/s wide (emission over the range from -200 to +1200 km/s has been seen in microwave observations; at 3 mm emission is seen over at least -50 to 350 km/s). 10 km/s resolution should be sufficient for it. With the initial one-quadrant correlator, mode 71 will cover 2000 km/s at 10 km/s resolution in band 6: this means that we would only have limited resolution for the narrow masing line, but it should be sufficient to separate the narrow line from the continuum and broad line in order for it to be mapped separately. 7.4. Bandwidth or spectral coverage (km/s or GHz): require 1500 km/s overall, but a narrower high-resolution window can be placed on the masing line when more correlator quadrants are available. 8. Continuum flux density: at 3 mm wavelength the flux ranges from 2.2 Jy at periastron to about 30 Jy at apastron. 8.1. Typical value (Jy): 10 Jy 8.2. Required continuum rms (Jy or K): .001 Jy 8.3. Dynamic range within image: 10000 8.4. Calibration requirements: absolute 1-3% for time variability studies repeatability 1-3% relative 1-3% 9. Line intensity: the narrow masing line ranges from 1 Jy with 20 km/s width at periastron to 15 Jy with 20 km/s width at apastron. The broad component is about 5 Jy at apastron. 9.1. Typical value (K or Jy): 5 Jy 9.2. Required rms per channel (K or Jy): .02 Jy 9.3. Spectral dynamic range: 1000 9.4. Calibration requirements: absolute 1-3% repeatability 1-3% relative 1-3% 10. Polarization: no (as far as we presently know) 10.1. Required Stokes parameters: I 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): a full track for sampling of all spatial scales to achieve high dynamic range imaging. If we alternate between the 4 high-priority bands within a single track then 10 hours per track is needed. 12. Total integration time for program (hr): for time variability 1 track every 6 months away from periastron, at 20 hours per year. For the "spectroscopic events" that will be the subject of large multiwavelength campaigns at periastron, one track every 2 months for 10 months around periastron (5.5 year orbit). 13. Comments on observing strategy : Primary target for high-spatial-resolution and high-dynamic-range capabilities of ALMA since it has a large flux in a compact region, appropriate for self-calibration. Emission over a range of spatial and flux scales requires high dynamic range. Continuum subtraction an issue for imaging of line emission. ===================================================================================== DRSP 3.4.4 Progect: Pulsar Wind Nebulae PI: V. Kaspi Time: 10 hrs 2. One short paragraph with science goal(s) Young, energetic pulsars (and some older pulsars) produce extended wind nebulae that radiate synchrotron emission from radio up to TeV gamma rays. The spectra of these objects are interesting as they provide information about the ambient magnetic field and the pulsar wind itself. There is an expected spectral break in/near the ALMA bands that has strong diagnostic potential. So observing a large sample of PWNe (ie a pulsar wind nebula survey) with ALMA is one obvious project to undertake. 3. Number of sources 16--22 PWNe (detected by Chandra observations) 4. Coordinates: 4.1. Rough RA and DEC Along the Galactic plane, RA: 05--20 hour; Decl: -70--60 degree. 4.2. Moving target: yes/no (e.g. comet, planet, ...) No. 4.3. Time critical: yes/no (e.g. SN, GRB, ...) No. 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution (arcsec): ~1 arcsec. 5.2. Range of spatial scales/FOV (arcsec): 10--100 arcsec. 5.3. Required pointing accuracy: (arcsec) 6. Observational setup 6.1. Single dish total power data: no 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: 3, 6, 9 7.2. Lines and Frequencies (GHz): 7.3. Spectral resolution (km/s): 7.4. Bandwidth or spectral coverage (km/s or GHz): 8. Continuum flux density: 8.1. Typical value (Jy): 0.01--0.1 Jy. two examples Size Surface flux in (band) time* Pulsar 1: 6" 8.84e2 mJy (3) 77s 6" 2.97e2 mJy (6) 75s 6" 8.72e1 mJy (9) 483s Pulsar 2: 30" 2.30e1 mJy (3) 25.7hr 30" 9.01e1 mJy (6) 23.3hr 30" 3.15e0 mJy (9) 120hr *time estimate based on 1" resolution, and 10 sigma detections 8.2. Required continuum rms (Jy or K): 0.001-0.01 Jy 8.3. Dynamic range within image: assume SNR of 10 8.4. Calibration requirements: Absolute, 10%. 9. Line intensity: 9.1. Typical value (K or Jy): 9.2. Required rms per channel (K or Jy): 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): for the bright source listed above (Pulsar 1), 77 s in band 3, 75 s in band 6 and 483 s in band 9 (total of 10.6 minutes on this source) 12. Total integration time for program (hr): for 15 source (of which Pulsar 1 is one of the brightest), estimate 10 hours of observations 13. Comments on observing strategy : (optional) A number of example pulsars were given as part of this DRSP. ===================================================================================== DRSP 3.5.1 Title Structure of the Molecular Gas Shocked by Supernova Remnatns Pi K. Tatematsu Time 206 hrs 1. Name: Structure of the Molecular Gas Shocked by Supernova Remnatns Authors: K. Tatematsu, .... 2. The interation of supernova remnants with molecular clouds is one of the most important phenomena in astrophysics, because it control local energetics in the interstellar medium and the evolution of the global interstellar matter. It is also suggested that SNR-cloud interaction may trigger the next-generation star formation. Furthermore, it will serve as a laboratory to test the theoretical studies of interstellar shocks. It becomes clear that intense syncrotron radiation, intense far infrared emission, 1720-MHz OH maser emission, and some X-ray feature are the indication of the interaction. Arikawa, Tatematsu, et al. (1999, PASJ 51, L7) has shown that there is shocked molecular gas in the supernova remnant W28, and its distribution is correlated with 1720-MHz OH maser, radio synchrotron, and far infrared emission. Structure of unshocked and shocked gas has been observed. However, we need higher angular resolution to study the structure of the interstellar shock due to the supernova remnant. By carrying out multi-J CO observations, we will be able to derive the variation of the gas properties across the shock front precisely. Multi-J CO observations will provide us with detailed kinetic temperature and density information across the shock front. We plan to observe regions near OH masers and other regions to study the physics of the SNR-cloud shock. From detailed observations, we will make clear the physical condition for 1720-MHz OH maser emission. 3. Number of sources: 3 4. Coordinates: 4.1. 3 sources distributed at l = 330 to 30 degrees which are known to interact with molecular clouds 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.15" 5.2. Range of spatial scales/FOV: 50" We need mosaic observation with B6 and B7. 5.3. Single dish: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 3 Band 6 Band 7 Band 8 6.2. Line: CO 1-0, 2-1, 3-2, 4-3 Frequency: 115, 230, 345, and 460 GHz 6.3. Spectral resolution (km/s): 1 km/s 6.4. Spectral coverage (km/s or GHz): 100 km/s 7. Continuum flux density: 7.1. Typical value: N/A 7.2. Continuum peak value: N/A 7.3. Required continuum rms: N/A 7.4. Dynamic range in image: N/A 8. Line intensity: 8.1. Typical value: 6-20 K (B3) 10-30 K (B6) 20-40 K (B7) 10-20K (B8) 8.2. Required rms per channel: 1.2 K (B3,6,7, 8) 8.3. Spectral dynamic range: >5 9. Polarization: no 10. Integration time per setting: 3 sources x 1 field x 20 hrs (B3) 3 sources x 5 fields x 1.5 hrs (B6) 3 sources x 13 fields x 0.7 hrs (B7) 3 sources x 16 fields x 2 hrs (B8) 11. Total integration time for program: 206 hr ***************************************************************** Review Leonardo Testi: Sounds good. Maybe there is no need to have all of the sources in the first three years. One or two well selected candidates can already give important answers. -------------------------------------------------- Review v2.0: 3.5.1 rev Structure of the Molecular Gas shocked by SNR Tatematsu Shocked gas in W28 was described twenty years before the reference given. This proposal targets all low order CO transitions--do we really need every transition? This is a shock, and the energies of the relevant levels are only a few K separated. Suggest CO2-1, 4-3 and perhaps 6-5; I suspect even here 4-3 might be overkill and the essential science would be contained in say 3-2 and 6-5. 1-0 perhaps; it would show the lay of the molecular gas which had not been disturbed. No other lines (than OH) are mentioned, though HCO+ was also shown to be interesting more than 20 years ago. Answer: The pair of CO 1-0 and 2-1 will provide the physical properties of the unshocked gas and the pair of CO 3-2 and 4-3 will provide those of the shocked gas. This program is aimed at very high angular resolution of 0.15" of the thermal gas, which is not possible with existing radio telescope, to see the detailed structure over the shock front. I made LVG calculations for CO and HCN for relevant parameter space. CO 6-5 intensity is 4-40 K and HCN intensity is of order 1 K at most. Then, the total observation time becomes huge. We can reduce the angular resolution, but it will change the scope of the program. Here we like to stick to very high angular resolution. ===================================================================================== DRSP 3.5.2 Title SNR-cloud interaction search in LMC Pi K. Tatematsu Time 86 hrs 1. Name: SNR-cloud interaction search in LMC Authors: K. Tatematsu, Y. Fukui,.... 2. LMC contains many supernova remnants (e.g. Mathewson et al. 1985). It is of our interest how supernova remnants affect the global properties in a galaxy. SNRs will input enrmous energy into the interstellar medium, and this will affect the evolution of the interstellar medium and the star formation activity. Then this will caracterize the evolution of the galaxy. Because LMC is the galaxy closest to us, this provides us with a great opportunity for a detailed scrutiny. With ALMA, we will be able to study the SNR-cloud interaction with appropriate angular resolution for the first time. Previouslly, SNR-cloud interaction was studied with SEST (Banas et al. 1997), but the angular resolution is too low to see the direct evidence of the interaction. We will take a census of the SNR-cloud in a galaxy with sufficient angular resolution and sensitivity for the first time. Arikawa, Tatematsu et al. (1999, PASJ 51, L7) have studied the supernova remnant W28 by using JCMT (beam size is about 15"=0.25 pc at 3 kpc). This study showed that CO 3-2 is one of the best tracers of the shocked molecular gas. The linear resolution of 0.25 pc corresponds to 1" at the distance of LMC, and with ALMA we will reach even better angular resolution. We can carry out a very promising statistical study of SNR-cloud interaction in LMC. This study will help our understanding the dynamical and thermal evolution of a galaxy. For a comparison, we will also observe CO 1-0 to distinguish the shocked and unshocked gas. References Arikawa et al. 1999 Banas et al. 1997 Mathewson et al. 1985 3. Number of sources: 30 4. Coordinates: 4.1. 30 sources in LMC (RA=05:30, DEC=-69:45) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 1.5" at 115GHz, 0.5" at 345 GHz 5.2. Range of spatial scales/FOV: 1' (16-field mosaic at 345 GHz) 5.3. Single dish: yes 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Bands 3 and 7 6.2. Line: CO 1-0 and 3-2 Frequency: 115 GHz and 345 GHz 6.3. Spectral resolution (km/s): 0.5 km/s 6.4. Spectral coverage (km/s or GHz): 100 km/s 7. Continuum flux density: 7.1. Typical value: N/A 7.2. Continuum peak value: N/A 7.3. Required continuum rms: N/A 7.4. Dynamic range in image: N/A 8. Line intensity: 8.1. Typical value: 2-10 K 8.2. Required rms per channel: 0.3 K 8.3. Spectral dynamic range: 10-30 9. Polarization: no 10. Integration time per setting: 115 GHz: 30 sources x 4 mosaic x 3min 345 GHz: 30 sources x 16 mosaic x 10min 11. Total integration time for program: 86 hr ===================================================================================== DRSP 3.5.3 Title The populations of relativistic particles and magnetic field structure in the Crab Nebula and other plerions Pi R. Bandiera Time 229 hrs 1. Name of program and authors Name: The populations of relativistic particles and magnetic field structure in the Crab Nebula and other plerions. Authors: R. Bandiera, R. Cesaroni, L. Testi 2. One short paragraph with science goal(s) Map at high angular resolution and sensitivity the polarized continuum emission at 1.3 and 3mm of the Crab nebula and other plerions. Recent single dish 1.3mm observations of the Crab nebula at ~10 arcsec resolution have shown evidence for: 1. a second synchrotron component in the continumm emission whose presence challenges the existing models; 2. smaller-scale spatial variations of the radio-mm spectral index across the nebula that may be an indication of filaments of stronger magnetic field (Bandiera et al. 2002). The single dish observations do not have the spatial resolution and polarimetric capabilities needed to confirm these indications. Equally important would be the possibility of a careful measurement of the variation of the spectral index across the nebula in the mm range (at nu<250GHz in order to measure the synchrotron emission and not the dust). ALMA will offer the required sensitivity, spatial resolution and calibration accuracy needed to perform a detailed study of the Crab and of other plerions, which may show similar features. Beyond the Crab nebula, plerions with a synchrotron spectral break around 100 GHz have been selected, since they are more likely to show morphological differences between the mm and the radio range, which could be used a diagnostic tool for the nebular physical conditions. Need to: Map the SNRs (size ~7' Crab, ~1' the others) at: <=0.5 arcsec resolution and rms~0.03 mJy/beam, for the Crab (scaling Bandiera et al. 2002 numbers); <=0.2 arcsec and 0.01 mJy/beam for the others. Polarization maps. 3. Number of sources 3 Source Name R.A.(1950) Dec.(1950) Crab Neb. 05:31:30.0 +21:59:00 (pure plerion, size 7'x5') G0.9+0.1 17:44:12.0 -28:08:00 (composite. plerionic core of 2' diam.) G21.5-0.9 18:30:47:0 -10:36:30 (pure plerion, of 1.2' diam.) 4. Coordinates: 4.1. Rough RA and DEC Source Name R.A.(1950) Dec.(1950) Crab Neb. 05:31:30.0 +21:59:00 (pure plerion, size 7'x5') G0.9+0.1 17:44:12.0 -28:08:00 (composite. plerionic core of 2' diam.) G21.5-0.9 18:30:47:0 -10:36:30 (pure plerion, of 1.2' diam.) 4.2. Moving target: no 4.3. Time critical: no 4.4. Scheduling constraints: no 5. Spatial scales: 5.1. Angular resolution (arcsec): ~0.5 arcsec Crab, ~0.2 arcsec the others 5.2. Range of spatial scales/FOV (arcsec): up to 7 arcmin (Crab); up to 1.2 arcmin (G21.5-0.9); up to 2 arcmin (G0.9+0.1) 5.3. Required pointing accuracy: 0.05 PrimaryBeam 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: on-the-fly mapping 6.2. Stand-alone ACA: required 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: beneficial (mainly for cross-calibration and accuracy) 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3, 6 7.2. Lines and Frequencies (GHz): N/A (approximate; do _not_ go into detail of correlator set-up but indicate whether multi-line or single line; apply redshift correction yourself; for multi-line observations in a single band requiring different frequency settings, indicate e.g. "3 frequency settings in Band 7" without specifying each frequency (or give dummies: 340., 350., 360. GHz). For projects of high-z sources with a range of redshifts, specify, e.g., "6 frequency settings in Band 3". Apply redshift correction yourself.) 7.3. Spectral resolution (km/s): 7.4. Bandwidth or spectral coverage (km/s or GHz): 8. Continuum flux density: 8.1. Typical value (Jy): Total Flux ~300 Jy (Crab), but low surface brightness (up to 10 mJy/beam at the required resolution) 8.2. Required continuum rms (Jy or K): 0.010-0.015 mJy/beam 0.03 mJy/beam for the Crab (Note the Crab is so large that it is very time consuming to do at 1.3mm, it should attempted only if the results of the 3mm map guarantee a good S/N with 0.03mJy/beam rms). 8.3. Dynamic range within image: <~1000 8.4. Calibration requirements: absolute ( 5% ) repeatability ( n/a ) relative ( 1-3% ) 9. Line intensity: N/A 9.1. Typical value (K or Jy): (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10. Polarization: yes 10.1. Required Stokes parameters: I, U, Q, V 10.2. Total polarized flux density (Jy): 10% of unpolarized flux 10.3. Required polarization rms and/or dynamic range: (<~1000) 0.010-0.015 mJy/beam 0.03 mJy/beam for the Crab 10.4. Polarization fidelity: ? 10.5. Required calibration accuracy: 10% 11. Integration time for each observing mode/receiver setting (hr): Crab: 16m/pointing at 3mm for a 200 pointings mosaic at 3mm. 200x16m/sqrt(2)=38hrs (sqrt(2) is for the sampling). The 1.3mm observations depend on the result of the 3mm, if the surface brightness is high enough, one could use the same integration time as for 3mm but on a 800 points grid, with a corresponding total integration time of ~155hrs. G21.5/G0.9, each: 1h/pointing at 1.3mm; 15min/point at 3mm ~16 point mosaic at 1.3mm (16h); ~8 point at 3mm (~2h) 12. Total integration time for program (hr): 38h Crab at 3mm, 36hrs G21/G0.9 = 74hrs (+ 155 hrs for the Crab at 1mm) 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...):-------------------------------------------------- Review v2.0: 3.5.4 rev The populations of relativistic particles and the magnetic field structure in the Crab Nebular and other pleions Bandiera 229 ALMA can provide key reference images of these important objects. This proposal looks good to me. ===================================================================================== DRSP 3.5.4 Title ToO Observing of Radio Supernovae - Pi S. Van Dyk Time 50 hrs per semester 1. Name: ToO Observing of Radio Supernovae -- Schuyler Van Dyk, Kurt Weiler et al. 2. One short paragraph with science goal(s) The radio emission from supernovae (SNe) is one of the best probes of the final stages of evolution for the stellar progenitors. The nonthermal synchrotron arises from the interaction of the SN shock with the pre-supernova, wind-established, circumstellar medium (CSM). Knowledge of the CSM provides strict constraints on the progenitor's nature and evolution. However, the particle acceleration process is still not known, and the absorption mechanism, which arises from the CSM, is not completely obvious. Although progress has been made at centimeter wavelengths over the last two decades, little has been accomplished in the mm and submm due to the sensitivity constraints and difficulty in scheduling ToOs. Observing radio SNe (RSNe) at high frequencies will help constrain both the emission and absorption processes. RSNe turn on quickly, within hours, and become optically thin within days in the ALMA bands. It is essential and indeed possible (with early SN warning arrangements) to observe with ALMA the early hours of a SN's evolution. A Virgo Cluster analog to the well-studied SN 1993J would reach ~2 mJy at max within 10 days; this analog easily could be detected out to a distance of ~60-70 Mpc. Of special interest are Type Ia RSNe, which evolve extremely fast and have yet to be detected at cm wavelengths. We also need to be prepared for the next Galactic or Local Group SN. The precise astrometry afforded by ALMA will also allow, in many cases, the pinpointing of the optical progenitor. This ToO would identify targets for the Monitoring program is also proposed as a standing program for followup studies of the light curve at later times. 3. Number of sources Based on current supernova searches, we anticipate approximately 2 to 20 per semester. 4. Coordinates: 4.1. All over the sky. 4.2. Moving target: no 4.3. Time critical: very 5. Spatial scales: 5.1. Angular resolution (arcsec): any ALMA resolution 5.2. Range of spatial scales/FOV (arcsec): point sources 5.3. Single dish total power data: no 5.4. ACA: no 5.5. Subarrays: could do 6. Frequencies: 6.1. Receiver band: 3, 6, 7, optionally 9 6.2. Lines and Frequencies (GHz): --- continuum 6.3. Spectral resolution (km/s): --- N/A 6.4. Bandwidth or spectral coverage (km/s or GHz): --- 8 GHz 7. Continuum flux density: 7.1. Typical value (Jy): 0.001-0.1 (detection, based on current RSN detections) 7.2. Required continuum rms (Jy or K): 0.00006 (.06 mJy) 7.3. Dynamic range within image: >4 8. Line intensity: 8.1. Typical value (K or Jy): N/A 8.2. Required rms per channel (K or Jy): N/A 8.3. Spectral dynamic range: N/A 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): typically 1/60 hr for Band 3 3/60 hr for Band 6 10/60 hr for Band 6 0.5 hr Band 9 (only if detected) 11. Total integration time for program (hr): 0.5 hr for null detection, if detected total ToO monitoring time over 2 weeks is 10-20 hrs Estimated ToO time every semester: on average, 50 hours, based on current monitoring programs at the VLA. 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): This is a target of opportunity proposal. The ToO window is very small for mm to submm emission from RSNe, hours at best. The higher the frequency, the shorter the rise time for the emission; models of SN1993J predict a peak emission 2-3 days after optical peak for band 7, and ~10 days after peak for band 3. The investigators would notify ALMA staff immediately of the detection of a SN and would have an observe file ready to go for bands 3, 6, and 7. This observe file would be 0.5-1 hr in length, depending on the distance to the host galaxy. If a solid detection is made, then this ToO program would request additional monitoring observations, including Band 9. The ToO monitoring program would extend up to 2 weeks, observing for 2-4 hours for the first 4 days, (1 hr observe file every 4 hrs), and then daily to day 14. After 2 weeks, the light curve is changing slowly enough that a standing RSN monitoring program would kick in. The scheduling of this ToO requires a significant amount of input from the observing team. The number of hours of ToO monitoring depends on the source: for a source like SN 1993J, in M81 at a distance of 3.5 Mpc, this could amount to observations every 4 hours for the first 4 days, and every 0.5 day for the next two weeks, for a total of 36 hrs for the light curve of the first two weeks. However, nearby supernovae like SN1993J are rare, occurring perhaps once every four years. More typical are RSN at the detection limit. Since the radio light curve falls to half its peak within ~8 days at 330 GHz (Band 7), within ~ 14 days at 230 GHz (Band 6), and ~20 days at 110 GHz (Band 3), the number of hours would be fewer for weaker sources, perhaps only 20, since they would quickly fall below detectability. This project could be done with a subarray, but the observing files would then increase in length from 0.5-1 hour to several hours. *********************************************************************** Review Leonardo Testi (programs 3.5.5 and 3.5.6): The first (3.5.5) is a ToO to measure mm fluxes of SN close to maximum, the second (3.5.6) requires monitoring of a few SN. I could not really tell which is and if there is any difference in the targets between the two projects. I would think that one finds a bright supernova and then will want to follow it in the framework of the first project (? maybe I am missing the point here?). I think these should be combined in a single project that finds and follows the supernovae. Total time, for the three years (is it really required? how many SN you need?) would be a total of 2semx50hx3y=300h for the first part and 2semx30hx3y=150h for the second, and a grand total of 450 hrs. Following the time estimates, this time will correspond to approx 6-10 supernovae for the "first part" and 10 per semester for "second part". Taking into account the "visibility" of SN for the monitoring, the time requested will allow to monitor approx 15 SN/yr, so it appears oversized compared to the first part (one finds 10 SN in 3 yrs, not all will be bright enough for monitoring, then how one selectes the ~45 SN for the monitoring?). I would say that, given the time requested for finding candidates, the monitoring should not exceed a total of at most 50hrs. This programme challenges operations, information- and data-flow. What is particularly critical is programme 3.5.5 (obviously). It is important to have this programme in to set the appropriate requirements on software and operations plan. Reply Jean Turner: Leonardo raises some good points. I attach slightly modified DRSPs. The first point is regarding why these are two DRSPs: the basic answer is that they are different kinds of scheduling. One is dynamic, the other not. I think the ToO should be separate from the monitoring. This is currently how it is handled at the VLA. The second is regarding the relative time estimate of the ToO and monitoring programs; Leonardo is making the reasonable assumption that they are the same sources, when in fact, they are not necessarily. Some RSN are detectable for nearly a decade, others fade within months. It is my impression that there are more RSN than can currently be monitored at the VLA, so only the "best" are followed. Generally the monitoring programs will be following RSN discovered outside the 3 yr time frame here (and this will be true for ALMA, which will initially be following up RSN discovered with the VLA). At some level the amount of time devoted to both of these programs, the ToO and the subsequent monitoring, is somewhat arbitrary. One can't monitor all the RSN. These numbers are roughly consistent with what is currently done at the VLA. It could be different for ALMA. The change I made to the DRSPs was to include in the total time request "based on current VLA programs" to explain the time estimate, which would address the 2nd point Leonardo raised. Comment Ewine: new DRSP is now baseline -------------------------------------------------- Review v2.0: 3.5.5 ToO Observing of Radio Supernovae van Dyk 50 Did not change from earlier proposal, wich was extensively refereed. ===================================================================================== DRSP 3.5.5 Title Monitoring of Radio Supernovae Pi S. Van Dyk Time 30 hrs per semester 1. Name: Monitoring of Radio Supernovae -- Schuyler Van Dyk, K. Weiler et al. 2. One short paragraph with science goal(s) The radio emission from supernovae (SNe) is one of the best probes of the final stages of evolution for the stellar progenitors. The nonthermal synchrotron arises from the interaction of the SN shock with the pre-supernova, wind-established, circumstellar medium (CSM). Knowledge of the CSM provides strict constraints on the progenitor's nature and evolution. However, the particle acceleration process is still not known, and the absorption mechanism, which arises from the CSM, is not completely obvious. Although progress has been made at centimeter wavelengths over the last two decades, little has been accomplished in the mm and submm due to the sensitivity constraints and difficulty in scheduling ToOs. Observing radio SNe (RSNe) at high frequencies will help constrain both the emission and absorption processes. Once a SN is detected in the mm and submm, it is vital to maintain nearly constant monitoring in all bands over the course of days to months. Such monitoring details the evolution of the RSN through maximum and into the exponential decline in each band. Together with cm wavelength monitoring, the well-developed radio light curves across the gamut of radio bands provide an accurate picture of the CSM, the mass-loss history of the progenitor prior to explosion, and the nature of the progenitor itself. The well-studied RSN SN1993J in M81 would have been visible for many years in all ALMA bands, but these local RSNe are relatively rare. A Virgo Cluster analog to SN 1993J would reach ~2 mJy at max within 10 days, and will be visible for ~100 days in Band 7 and ~600 days in Band 3. This analog easily could be detected out to a distance of ~60-70 Mpc. This is a standing program for the long-term monitoring of RSNe. 3. Number of sources Based on current supernova searches, we anticipate approximately 2 to 20 per semester. 4. Coordinates: 4.1. All over the sky. 4.2. Moving target: no 4.3. Time critical: very 5. Spatial scales: 5.1. Angular resolution (arcsec): any ALMA resolution 5.2. Range of spatial scales/FOV (arcsec): point sources 5.3. Single dish total power data: no 5.4. ACA: no 5.5. Subarrays: could do 6. Frequencies: 6.1. Receiver band: All. 6.2. Lines and Frequencies (GHz): --- continuum 6.3. Spectral resolution (km/s): --- N/A 6.4. Bandwidth or spectral coverage (km/s or GHz): --- 8 GHz 7. Continuum flux density: 7.1. Typical value (Jy): 0.001-0.1 7.2. Required continuum rms (Jy or K): 0.00006 (.06 mJy) 7.3. Dynamic range within image: >4 8. Line intensity: 8.1. Typical value (K or Jy): N/A 8.2. Required rms per channel (K or Jy): N/A 8.3. Spectral dynamic range: N/A 9. Polarization: no 10. Integration time for each observing mode/receiver setting (hr): typically 1/60 hr for Band 3 3/60 hr for Band 6 10/60 hr for Band 7 0.5 hr Band 9 (only if detected) 11. Total integration time for program (hr): total ToO monitoring time every month = 5 hrs (0.5 hr/source x 10 sources) Estimated ToO time every semester: on average, 30 hours, based on current monitoring programs at the VLA. 12. Comments on observing strategy (e.g. line surveys, Target of Opportunity, Sun, ...): This is a standing program to monitor the light curves of nearby known RSN, with scheduled observing files to be executed every month. ************************************************************************* Review Leonardo Testi (programs 3.5.5 and 3.5.6): The first is a ToO to measure mm fluxes of SN close to maximum, the second requires monitoring of a few SN. I could not really tell which is and if there is any difference in the targets between the two projects. I would think that one finds a bright supernova and then will want to follow it in the framework of the first project (? maybe I am missing the point here?). I think these should be combined in a single project that finds and follows the supernovae. Total time, for the three years (is it really required? how many SN you need?) would be a total of 2semx50hx3y=300h for the first part and 2semx30hx3y=150h for the second, and a grand total of 450 hrs. Following the time estimates, this time will correspond to approx 6-10 supernovae for the "first part" and 10 per semester for "second part". Taking intop account the "visibility" of SN for the monitoring, the time requested will allow to monitor approx 15 SN/yr, so it appears oversized compared to the first part (one finds 10 SN in 3 yrs, not all will be bright enough for monitoring, then how one selectes the ~45 SN for the monitoring?). I would say that, given the time requested for finding candidates, the monitoring should not exceed a total of at most 50hrs. This programme challenges operations, information- and data-flow. What is particularly critical is programme 3.5.5 (obviously). It is important to have this programme in to set the appropriate requirements on software and operations plan. Reply Jean Turner: Leonardo raises some good points. I attach slightly modified DRSPs. The first point is regarding why these are two DRSPs: the basic answer is that they are different kinds of scheduling. One is dynamic, the other not. I think the ToO should be separate from the monitoring. This is currently how it is handled at the VLA. The second is regarding the relative time estimate of the ToO and monitoring programs; Leonardo is making the reasonable assumption that they are the same sources, when in fact, they are not necessarily. Some RSN are detectable for nearly a decade, others fade within months. It is my impression that there are more RSN than can currently be monitored at the VLA, so only the "best" are followed. Generally the monitoring programs will be following RSN discovered outside the 3 yr time frame here (and this will be true for ALMA, which will initially be following up RSN discovered with the VLA). At some level the amount of time devoted to both of these programs, the ToO and the subsequent monitoring, is somewhat arbitrary. One can't monitor all the RSN. These numbers are roughly consistent with what is currently done at the VLA. It could be different for ALMA. The change I made to the DRSPs was to include in the total time request "based on current VLA programs" to explain the time estimate, which would address the 2nd point Leonardo raised. Comment Ewine: new DRSP is now baseline -------------------------------------------------- Review v2.0: 3.5.6 Monitoring of Radio Supernovae van Dyk 30 Did not change from earlier proposal, wich was extensively refereed. ===================================================================================== DRSP 4.1.1 Title The dynamics of Mars' and Venus' middle atmopheres Pi E. Lellouch Time 120 hrs 1. Name of program and authors Title: The dynamics of Mars' and Venus' middle atmopheres Authors: E. Lellouch 2. One short paragraph with science goal(s) Abstract: Mapping CO lines is a powerful tool to study the dynamics of the middle atmospheres of Mars (~30-70 km) and Venus (70-110 km) because their observation allows a simultaneous determination of (i) the local CO abundance (ii) the local thermal field (iii) the wind velocity from Doppler shift. All three parameters are related. The great originality is provided by the direct wind measurements which are out of reach to space missions. The high spatial resolution and the possibility to quickly acquire images will provide snapshots of the atmospheric circulation and the possibility of measuring local structures (e.g. jets, waves....). 3. Number of sources : 2 Venus Mars 4. Coordinates: 4.1. Rough RA and DEC Variable 4.2. Moving target: yes/no (e.g. comet, planet, ...) Yes 4.3. Time critical: yes/no (e.g. SN, GRB, ...) Yes (Mars opposition, Venus maximum elongation and/or inferior conjunction) 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.5 5.2. Range of spatial scales/FOV (arcsec): FOV = 10-60 (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 5.3. Required pointing accuracy: (arcsec) 0.5 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: wobbler switch (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: required 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3, 6, 7 7.2. Lines and Frequencies (GHz): CO and 13CO J=1-0, 2-1, and 3-2 7.3. Spectral resolution (km/s): 0.05 7.4. Bandwidth or spectral coverage (km/s or GHz): 0.5 GHz 8. Continuum flux density: 8.1. Typical value (Jy): Venus : 300 K Mars : 200 K 8.2. Required continuum rms (Jy or K): 0.1 K 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) 8.4. Calibration requirements: absolute ( 10% ) repeatability ( 10% ) relative ( 10% ) 9. Line intensity: 9.1. Typical value (K or Jy): 10 K (13CO) - 100 K (12CO) 9.2. Required rms per channel (K or Jy): 0.2 K 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 10% ) repeatability ( 10% ) relative ( 10% ) 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 10 hr per planet and line. Mars should be done at several seasons. 12. Total integration time for program (hr): 120 hr + 13. Comments on observing strategy : -------------------------------------------------- Review v2.0: Review 4.1.1-4.1.8 The only question I have with regards to these projects is the use of ACA cross-correlated with ALMA-12m. Several projects list this option as 'required' or as 'beneficial', but no arguments are given. - When listed as 'required' does this mean that the observations are mosaics, and that the ACA is needed to provide the intermediate scales? If so, are the cross-correlations with the ALMA-12m antennas needed, or could simultaneous ACA-7m-only observations also suffice? - When listed as 'beneficial' is this purely for S/N reasons or also for uv-coverage? The cross-correlation option is fairly demanding on the scheduling, and unlikely to be used unless absolutely necessary. ===================================================================================== DRSP 4.1.2 Title The three-dimensional water cycle of Mars Pi E. Lellouch Time 320 hrs 1. Name of program and authors Title: The three-dimensional water cycle of Mars Authors: E. Lellouch 2. One short paragraph with science goal(s) Abstract: The water cycle on Mars is a key subject in martian research and a focus of space missions to Mars. As compared to space missions, the great interest of ALMA will be the possibility to determine the vertical profile of water (through H2O, H2O18, and HDO), i.e. to retrieve true 3-D fields of water, and their variability with season. The ultimate goal is the understanding of exchanges and interactions between the atmosphere and the sources of water (regolith, polar caps). Spatial variations in the D/H ratio will also be searched for. 3. Number of sources : 1 Mars 4. Coordinates: 4.1. Rough RA and DEC Variable 4.2. Moving target: yes/no (e.g. comet, planet, ...) Yes 4.3. Time critical: yes/no (e.g. SN, GRB, ...) Yes. Needs to be done at several Mars seasons 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.2-0.5 5.2. Range of spatial scales/FOV (arcsec): FOV = 2-20 (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 5.3. Required pointing accuracy: (arcsec) 0.2 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: wobbler switch (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: required 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 5, 6, 7, 8 7.2. Lines and Frequencies (GHz): H2O 183 or 325 GHz HDO 226, 242, 464 GHz H2O18 at 204 GHz (e.g.) 7.3. Spectral resolution (km/s): 1 7.4. Bandwidth or spectral coverage (km/s or GHz): 0.5 GHz for HDO and H2O18 8 GHz for H2O. 8. Continuum flux density: 8.1. Typical value (Jy): Mars : 200 K 8.2. Required continuum rms (Jy or K): 0.1 K 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) 8.4. Calibration requirements: absolute ( 10% ) repeatability ( 10% ) relative ( 10% ) 9. Line intensity: 9.1. Typical value (K or Jy): 2 K (HDO and H2O18) - 100 K (H2O) 9.2. Required rms per channel (K or Jy): 0.1 K 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 10% ) repeatability ( 10% ) relative ( 10% ) 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 2 hr - 40 h per line, depending on Mars' size. Observations should be performed at least at four Mars seasons 12. Total integration time for program (hr): ~ 320 hours (4 seasons x 4 lines x 20 hours in average) 13. Comments on observing strategy : For Mars, should be combined with DRSP 4.1.1. because temperature profile is needed to retrieve water vapor and with DRSP 4.1.3 to search for correlations between water and other minor species. -------------------------------------------------- Review v2.0: Review 4.1.1-4.1.8 The only question I have with regards to these projects is the use of ACA cross-correlated with ALMA-12m. Several projects list this option as 'required' or as 'beneficial', but no arguments are given. - When listed as 'required' does this mean that the observations are mosaics, and that the ACA is needed to provide the intermediate scales? If so, are the cross-correlations with the ALMA-12m antennas needed, or could simultaneous ACA-7m-only observations also suffice? - When listed as 'beneficial' is this purely for S/N reasons or also for uv-coverage? The cross-correlation option is fairly demanding on the scheduling, and unlikely to be used unless absolutely necessary. ===================================================================================== DRSP 4.1.3 Title Chemistry in the atmospheres of Venus and Mars Pi E. Lellouch Time 70 hrs 1. Name of program and authors Title: Chemistry in the atmospheres of Venus and Mars Authors: E. Lellouch 2. One short paragraph with science goal(s) Abstract: The chemistry of Mars and Venus atmospheres remains poorly understood, as in particular, few species have been detected while photochemical models predict more are present. Species such as O2, O3, H2O2, H2CO, NO should be observed on Mars. For those species for which detection is certain (O2, O3, H2O2), spatial and seasonal variability, and correlation with water vapor variations should be studied. On Venus, species such as HCl, H2S, SO2, SO must be observed and monitored as possible tracers of active volcanism. 3. Number of sources : 2 Mars Venus 4. Coordinates: 4.1. Rough RA and DEC Variable 4.2. Moving target: yes/no (e.g. comet, planet, ...) Yes 4.3. Time critical: yes/no (e.g. SN, GRB, ...) Yes. Needs to be done at Mars opposition, and Venus inferior conjunction and/or maximal elongation. Needs to be done at several Mars seasons (at least four) and repeated on Venus (once a year or so). 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution (arcsec): 1 5.2. Range of spatial scales/FOV (arcsec): FOV = 10-60 (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 5.3. Required pointing accuracy: (arcsec) 1 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: wobbler switch (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: required 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 6, 7, 9 7.2. Lines and Frequencies (GHz): SO2, H2S: 216.7 GHz SO: 220 GHz O3, H2O2: 363 GHz O16O18,H2CO: 234 GHz NO: 350 GHz HCl: 626 GHz 7.3. Spectral resolution (km/s): 1 for Venus, 0.1 km/s for Mars 7.4. Bandwidth or spectral coverage (km/s or GHz): 0.1 GHz for Mars, 8 GHz for Venus. 8. Continuum flux density: 8.1. Typical value (Jy): Mars : 200 K Venus : 300 K 8.2. Required continuum rms (Jy or K): 0.1 K 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) 8.4. Calibration requirements: absolute ( 10% ) repeatability ( 10% ) relative ( 10% ) 9. Line intensity: 9.1. Typical value (K or Jy): 2 K 9.2. Required rms per channel (K or Jy): 0.05 K 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 10% ) repeatability ( 10% ) relative ( 10% ) 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 1 hr per line for Venus, 2 h per line for Mars 12. Total integration time for program (hr): ~ 70 hours (2 planets x 4 epochs x 6 freqs x 1.5 hour in average) 13. Comments on observing strategy : Should be combined with DRSP 4.1.1 (thermal profile measurements) and for Mars with DRSP 4.1.2 (water measurements) -------------------------------------------------- Review v2.0: Review 4.1.1-4.1.8 The only question I have with regards to these projects is the use of ACA cross-correlated with ALMA-12m. Several projects list this option as 'required' or as 'beneficial', but no arguments are given. - When listed as 'required' does this mean that the observations are mosaics, and that the ACA is needed to provide the intermediate scales? If so, are the cross-correlations with the ALMA-12m antennas needed, or could simultaneous ACA-7m-only observations also suffice? - When listed as 'beneficial' is this purely for S/N reasons or also for uv-coverage? The cross-correlation option is fairly demanding on the scheduling, and unlikely to be used unless absolutely necessary. ===================================================================================== DRSP 4.1.4 Title Composition and dynamics of giant planet stratospheres Pi E. Lellouch Time 160 hrs 1. Name of program and authors Title: Composition and dynamics of giant planet stratospheres Authors: E. Lellouch 2. One short paragraph with science goal(s) Abstract: ALMA can tackle a variety of problems related to giant planet stratospheres: (i) composition - search for new species, in particular CO in Saturn and Uranus (ii) atmospheric dynamics from mapping of tracer species (including CO, HCN on Neptune, and CO, HCN,CS, injected from SL9 impact, on Jupiter) (iii) dynamics from direct wind measurements (iv) origin of external water from HDO search. 3. Number of sources : 4 Jupiter, Saturn, Uranus, Neptune 4. Coordinates: 4.1. Rough RA and DEC variable 4.2. Moving target: yes 4.3. Time critical: yes for Jupiter, no otherwise 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.2" (Neptune) to 2" (Jupiter) 5.2. Range of spatial scales/FOV (arcsec): 2" (Neptune) to 50" (Jupiter) (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 5.3. Required pointing accuracy: 0.2" 6. Observational setup 6.1. Single dish total power data: required (Jupiter/Saturn) Observing modes for single dish total power: wobbler switch (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: required (Jupiter/Saturn) 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 5, 6, 7, 8, 9 7.2. Lines and Frequencies (GHz): CO: 230, 345, 460, 806 GHz CS: 244 GHz HCN: 354 GHz H2O: 183 and/or 325 GHz HC3N,CH3CN: 255 GHz TBD molecular searches near 250, 350, 650 GHz 7.3. Spectral resolution (km/s): 1 km/s in general. 0.05 km/s for wind measurements 7.4. Bandwidth or spectral coverage (km/s or GHz): 0.2 GHz 8. Continuum flux density: 8.1. Typical value (Jy): Jupiter: 160 K, Saturn: 110 K, Uranus and Neptune: 80 K (take average value of set of objects) (optional: provide range of fluxes for set of objects) 8.2. Required continuum rms (Jy or K): 0.1 K 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) 8.4. Calibration requirements: absolute 5 % repeatability 1-3% relative 1-3% 9. Line intensity: 9.1. Typical value (K or Jy): 20 mK - 20 K (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): 0.03 K - 0.5 K 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute 5 % repeatability 1-3% relative 1-3% 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): Typically 1 h per line, except 10 hr for HDO, and 5 h for high-resolution studies on CO or HCN for wind measurements In total, 2x10h (HDO) + 15 other molecular lines X 1 h + 5h = 40 h 12. Total integration time for program (hr): About 160 hours (40 h x 4 planets) 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): -------------------------------------------------- Review v2.0: Review 4.1.1-4.1.8 The only question I have with regards to these projects is the use of ACA cross-correlated with ALMA-12m. Several projects list this option as 'required' or as 'beneficial', but no arguments are given. - When listed as 'required' does this mean that the observations are mosaics, and that the ACA is needed to provide the intermediate scales? If so, are the cross-correlations with the ALMA-12m antennas needed, or could simultaneous ACA-7m-only observations also suffice? - When listed as 'beneficial' is this purely for S/N reasons or also for uv-coverage? The cross-correlation option is fairly demanding on the scheduling, and unlikely to be used unless absolutely necessary. ===================================================================================== DRSP 4.1.5 Title Search for broad lines in the tropospheres of the giant planets Pi E. Lellouch Time 16 hrs 1. Name of program and authors Title: Search for broad lines in the tropospheres of the giant planets Authors: E. Lellouch 2. One short paragraph with science goal(s) Abstract: A few molecular lines are expected to be formed in giant planet tropospheres (at 0.1-1 bar), and as such, to be broad (several GHz). Observing them would provide new information on the composition of giant planet tropospheres. Species will include CO, PH3, and HCl. In addition, continuum measurements at a variety of wavelengths can elucidate belt-zone structure and temperature at different altitudes. Such studies are already performed in the cm range and need to be extended to the mm/submm. Seasonal variability will be investigated by repeating the observations 6 times over several years. 3. Number of sources : 4 Jupiter, Saturn, Uranus, Neptune 4. Coordinates: 4.1. Rough RA and DEC variable 4.2. Moving target: yes 4.3. Time critical: yes (seasonal variability will be investigated) 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.2" (Neptune) to 2" (Jupiter) 5.2. Range of spatial scales/FOV (arcsec): 2" (Neptune) to 50" (Jupiter) (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 5.3. Required pointing accuracy: 0.2" 6. Observational setup 6.1. Single dish total power data: required (Jupiter/Saturn) Observing modes for single dish total power: wobbler switch (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: required (Jupiter/Saturn) 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 6, 7, 9 7.2. Lines and Frequencies (GHz): CO: 230, 345 GHz PH3: 267 HCl: 626 GHz 7.3. Spectral resolution (km/s): 20 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 8 GHz 8. Continuum flux density: 8.1. Typical value (Jy): Jupiter: 160 K, Saturn: 110 K, Uranus and Neptune: 80 K (take average value of set of objects) (optional: provide range of fluxes for set of objects) 8.2. Required continuum rms (Jy or K): 0.1 K 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) 8.4. Calibration requirements: absolute 1-3% repeatability 1-3% relative 1-3% 9. Line intensity: 9.1. Typical value (K or Jy): 3 K - 20 K (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): 0.03 K 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute 1-3% repeatability 1-3% relative 1-3% 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): Typically 10 min per line. 12. Total integration time for program (hr): About 16 hours (10 min x 4 lines x 4 planets x 6 repetitions) 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): -------------------------------------------------- Review v2.0: Review 4.1.1-4.1.8 The only question I have with regards to these projects is the use of ACA cross-correlated with ALMA-12m. Several projects list this option as 'required' or as 'beneficial', but no arguments are given. - When listed as 'required' does this mean that the observations are mosaics, and that the ACA is needed to provide the intermediate scales? If so, are the cross-correlations with the ALMA-12m antennas needed, or could simultaneous ACA-7m-only observations also suffice? - When listed as 'beneficial' is this purely for S/N reasons or also for uv-coverage? The cross-correlation option is fairly demanding on the scheduling, and unlikely to be used unless absolutely necessary. ===================================================================================== DRSP 4.1.6 Title Chemical-dynamical couplings and meteorology in Titan's atmosphere Pi E. Lellouch Time 160 hrs 1. Name of program and authors Title: Chemical-dynamical couplings and meteorology in Titan's atmosphere Authors: E. Lellouch 2. One short paragraph with science goal(s) Abstract: Titan's atmosphere, rich in hydrocarbons, nitriles and oxygenated compounds, is the place for strong chemical-dynamical couplings at these species exhibit strong seasonal variability, are influenced by the global circulation patterns, and participate in the atmospheric thermal balance. ALMA will map at 0.2" species such as CO, HCN, HC3N, CH3CN. Search for new species like CH3CCH, CH2NH, DCN, CxHyCN etc... will be performed. Stratospheric winds will be measured and thermal profiles retrieved in all strong lines. In additon, continuum measurements at a series of frequencies will allow one to map the tropospheric temperature and possible methane humidity. 3. Number of sources : 1 Titan (satellite) 4. Coordinates: 4.1. Rough RA and DEC variable 4.2. Moving target: yes. Satellite ephemerides need to be implemented. 4.3. Time critical: yes (seasonal variability will be investigated) 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.2" 5.2. Range of spatial scales/FOV (arcsec): 0.8" (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 5.3. Required pointing accuracy: 0.2" 6. Observational setup 6.1. Single dish total power data: no Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: beneficial 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 5, 6, 7, 8, 9 7.2. Lines and Frequencies (GHz): CO: 230, 345 GHz HCN: 354 GHz H2O: 183 and/or 325 GHz HDO: 226, 464 GHZ HC3N,CH3CN: 255 GHz TBD molecular searches near 250, 350, 650 GHz 7.3. Spectral resolution (km/s): 0.05 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 2 GHz for broad CO, HCN lines. 0.5 GHz may be sufficient for other trace species. 8. Continuum flux density: 8.1. Typical value (Jy): 80 K (take average value of set of objects) (optional: provide range of fluxes for set of objects) 8.2. Required continuum rms (Jy or K): 0.01 K 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) 8.4. Calibration requirements: absolute 1-3% repeatability 1-3% relative 1-3% 9. Line intensity: 9.1. Typical value (K or Jy): 3 K - 30 K (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): 0.5 K 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute 5 % repeatability 1-3% relative 1-3% 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): Typically 10 hours per line. Wind measurements will be repeated a few (4) times to search for seasonal variability. 12. Total integration time for program (hr): About 160 hours 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): -------------------------------------------------- Review v2.0: Review 4.1.1-4.1.8 The only question I have with regards to these projects is the use of ACA cross-correlated with ALMA-12m. Several projects list this option as 'required' or as 'beneficial', but no arguments are given. - When listed as 'required' does this mean that the observations are mosaics, and that the ACA is needed to provide the intermediate scales? If so, are the cross-correlations with the ALMA-12m antennas needed, or could simultaneous ACA-7m-only observations also suffice? - When listed as 'beneficial' is this purely for S/N reasons or also for uv-coverage? The cross-correlation option is fairly demanding on the scheduling, and unlikely to be used unless absolutely necessary. ===================================================================================== DRSP 4.1.7 Title Io's volcanism Pi E. Lellouch Time 100 hrs 1. Name of program and authors Title: Io's volcanism Authors: E. Lellouch 2. One short paragraph with science goal(s) Abstract: Io's atmosphere is dominated by active volcanism that directly injects species like SO2, SO, NaCl into the atmosphere. This atmosphere shows unique spatial and temporal variability, which remains poorly characterized. ALMA can map the detected species, measure Doppler shifts that are due to planetary-wide circulation regimes, to plasma interactions, or to volcanic plume injection, and search for many new potential atmospheric molecules (OCS, S2O, KCl, Cl0...) as well as determine chlorine and sulfur isotopic ratios. All this bears implications on the composition of ionian lavae, magmas and interior. 3. Number of sources : 1 Io (satellite) 4. Coordinates: 4.1. Rough RA and DEC variable 4.2. Moving target: yes. Satellite ephemerides need to be implemented. 4.3. Time critical: yes (need to observe Io sufficiently away from Jupiter) 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.2" 5.2. Range of spatial scales/FOV (arcsec): 1.2" (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 5.3. Required pointing accuracy: 0.2" 6. Observational setup 6.1. Single dish total power data: no Observing modes for single dish total power: (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: beneficial 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 6, 7 7.2. Lines and Frequencies (GHz): Many lines at 1.3 mm and 0.8 mm 7.3. Spectral resolution (km/s): 0.05 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 30 km/s is sufficient to correct for orbital motions of Io. Large bandwidth (up to several GHz) is desirable to optimize serendipitous line searches. 8. Continuum flux density: 8.1. Typical value (Jy): 100 K (take average value of set of objects) (optional: provide range of fluxes for set of objects) 8.2. Required continuum rms (Jy or K): 0.1 K 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) 8.4. Calibration requirements: absolute 10 % repeatability 5 % relative 5 % 9. Line intensity: 9.1. Typical value (K or Jy): 2 K - 30 K (take average value of set of objects) (optional: provide range of values for set of objects) 9.2. Required rms per channel (K or Jy): 0.5 K 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute 5 % repeatability 1-3% relative 1-3% 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): Typically 10 hours per line. 12. Total integration time for program (hr): About 100 hours 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): If a volcanic "event" occurs, it could be a ToO. -------------------------------------------------- Review v2.0: Review 4.1.1-4.1.8 The only question I have with regards to these projects is the use of ACA cross-correlated with ALMA-12m. Several projects list this option as 'required' or as 'beneficial', but no arguments are given. - When listed as 'required' does this mean that the observations are mosaics, and that the ACA is needed to provide the intermediate scales? If so, are the cross-correlations with the ALMA-12m antennas needed, or could simultaneous ACA-7m-only observations also suffice? - When listed as 'beneficial' is this purely for S/N reasons or also for uv-coverage? The cross-correlation option is fairly demanding on the scheduling, and unlikely to be used unless absolutely necessary. ===================================================================================== DRSP 4.1.8 Title The atmospheres of Triton, Pluto and other transneptunians (TNO) Pi E. Lellouc Time 432 hrs 1. Name of program and authors Title: The atmospheres of Triton, Pluto and other transneptunians (TNO) Authors: E. Lellouch 2. One short paragraph with science goal(s) Abstract: Triton and Pluto have detectable tenuous atmospheres with ~10 microbar pressure. These primarily N2 atmospheres exhibit slow time variation due to volatile migration and surface temperature changes. ALMA can search for new species in these atmospheres, in particular CO and HCN. Similarly the largest known TNOs, whose sizes are ~2000 km, may be able to retain atmospheres, and search for CO is warranted. This search could include Pluto's satellite Charon. If, as expected, CO is detected on Pluto and Triton, atmospheric circulation might be measured from Doppler shifts. 3. Number of sources : ~5-10 Pluto Triton Charon Eris 2003 EL61 2003 FY9 4. Coordinates: 4.1. Rough RA and DEC Variable 4.2. Moving target: yes/no (e.g. comet, planet, ...) Yes. Comet-like ephemerides may need to be implemented 4.3. Time critical: yes/no (e.g. SN, GRB, ...) No 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.03-0.1 Note: In general, the resolution here is not what is required during observation, but rather the size of the body, which is what is needed for the brightness temp rms calculation. These are point source detections - i.e., we don't *want* the body resolved (any resolution *worse* than this is OK). For Pluto and Triton (0.1" in size), though, a ~0.03" resolution would be needed to map CO and investigate winds from Doppler shifts. 5.2. Range of spatial scales/FOV (arcsec): FOV = 0.03-0.1 (optional: indicate whether single-field, small mosaic, wide-field mosaic...) 5.3. Required pointing accuracy: (arcsec) 0.1 6. Observational setup 6.1. Single dish total power data: no Observing modes for single dish total power: wobbler switch (e.g., nutator switch; frequency switch; position switch; on-the-fly mapping; and combinations of the above) 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: beneficial 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 6, 7 7.2. Lines and Frequencies (GHz): CO J=2-1 and 3-2 HCN J=3-2 and 4-3 7.3. Spectral resolution (km/s): 0.05 7.4. Bandwidth or spectral coverage (km/s or GHz): 0.5 GHz 8. Continuum flux density: 8.1. Typical value (Jy): 30-40 K 8.2. Required continuum rms (Jy or K): 0.1 K 8.3. Dynamic range within image: (from 7.1 and 7.2, but also indicate whether, e.g., weak objects next to bright objects) 8.4. Calibration requirements: absolute ( 10% ) repeatability ( 10% ) relative ( 10% ) 9. Line intensity: 9.1. Typical value (K or Jy): 10 K (?) 9.2. Required rms per channel (K or Jy): 1 K 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 10% ) repeatability ( 10% ) relative ( 10% ) 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 24 hr per planet and line. 12. Total integration time for program (hr): 432 hr (~3 lines x 6 objects x 24 hours) 13. Comments on observing strategy : -------------------------------------------------- Review v2.0: Review 4.1.1-4.1.8 The only question I have with regards to these projects is the use of ACA cross-correlated with ALMA-12m. Several projects list this option as 'required' or as 'beneficial', but no arguments are given. - When listed as 'required' does this mean that the observations are mosaics, and that the ACA is needed to provide the intermediate scales? If so, are the cross-correlations with the ALMA-12m antennas needed, or could simultaneous ACA-7m-only observations also suffice? - When listed as 'beneficial' is this purely for S/N reasons or also for uv-coverage? The cross-correlation option is fairly demanding on the scheduling, and unlikely to be used unless absolutely necessary. ===================================================================================== DRSP 4.2.1 Title Albedos, sizes and surface properties of transneptunian objects Pi E. Lellouch Time 140 hrs Title: Albedos, sizes and surface properties of transneptunian objects Authors: E. Lellouch Abstract: The distribution of size in the Kuiper Belt is an indicator of formation and collisional evolution processes. Knowledge of the albedo of the objects is needed to correctly interpret their spectra, and to search for possible correlations in the albedo-size-color space that would trace their dynamical and collisional history. This can be obtained by measuring the continuum thermal flux of these objects. For the largest of these objects, mm lightcurves (i.e. the variation of the thermal flux with the object rotational phase) can be obtained, providing additional information on the object surface properties, particularly the thermal inertia. contin line poln name RA&DEC m T SD CA sub resn size freq line dfreq BW fd rms fd rms fd rms time ------- ----------- - - -- -- --- ---- ---- ---- ---------- -------- ------- ------------ ----------- --------- ------- many ~ecliptic Y Y N N N .05 ~.05 345 N/A N/A 16 GHz 1 mJy .1 K N/A N/A 140x1 h total 140 h Notes: The resolution here is not what is required during observation, but rather the size of the body, which is what is needed for the brightness temp rms calculation. These are point source detections - i.e., we don't *want* the body resolved (any resolution *worse* than this is OK). Each detection (to .1 K rms) takes about an hour. There might be 100 or so bodies, then some monitoring for the larger ones. **************************************************************************** See program 4.1.1 for general comments Butler and Gurwell Review Mark Gurwell: OK.-------------------------------------------------- Review v2.0: Review of 4.2.1-4.2.8 (no DRSP 2.0 updates received) These projects still remain scientifically valid. Do the additional ALMA bands offer something new (e.g., for projects 4.2.4, 4.2.5)? The integration times are probably still ok eventhough the number of antennas has gone from 64 to 50 - or at least close enough. Several of these projects focus on objects larger than the ALMA primary beam, and mosaicing is needed. Here the ACA and also the ACA in crosscorrelation with the ALMA-12m antennas may be beneficial. ===================================================================================== DRSP 4.2.2 Title Mapping the surfaces of the Moon, Mercury and Mars Pi B. Butler Time 66 hrs Title: Mapping the surfaces of the Moon, Mercury and Mars Authors: B. Butler Abstract: ALMA will be able to map with unprecedented accuracy and fidelity the millimeter wavelength emission from the solid surfaces of the terrestrial planets (with the exception of Venus). Such maps will provide us with information on the thermal and electrical properties of the surface and near-surface, as well as the surface texture - see e.g. Rudy et al. 1987; Mitchell & de Pater 1994. For Mercury, the question of the presence of a molten liquid core may be answered if the accuracy is good enough. In addition, the temperature can be determined in the polar cold traps, which might be locations of water ice stability (this will require high resolution). For Mars, results will be compared to those returned from spacecraft in orbit at the time. This might also be true for the Moon. Maps should be made at all wavelengths, many of which will have to be mosaics because of the large size of the bodies (notably the Moon). contin line poln name RA&DEC m T SD CA sub resn size freq line dfreq BW fd rms fd rms fd rms time ------- ----------- - - -- -- --- ---- ---- ---- ------ -------- ----- ------------ ----------- --------- ---- Moon ecliptic Y Y Y Y N 2 1800 90 N/A N/A 8 GHz 200 K 2 K N/A 5 K .1 K 6 h Moon ecliptic Y Y Y Y N 2 1800 230 N/A N/A 8 GHz 200 K 2 K N/A 5 K .1 K 6 h Mars ecliptic Y Y Y Y N .1 10 90 N/A N/A 8 GHz 200 K 2 K N/A 5 K .1 K 6 h Mars ecliptic Y Y Y Y N .1 10 230 N/A N/A 8 GHz 200 K 2 K N/A 5 K .1 K 6 h Mars ecliptic Y Y Y Y N .1 10 345 N/A N/A 8 GHz 200 K 2 K N/A 5 K .1 K 6 h Mars ecliptic Y Y Y Y N .1 10 650 N/A N/A 8 GHz 200 K 2 K N/A 5 K .1 K 6 h Mercury ecliptic Y Y Y Y N .1 10 90 N/A N/A 8 GHz 450 K 2 K N/A 10 K .1 K 6 h Mercury ecliptic Y Y Y Y N .1 10 230 N/A N/A 8 GHz 450 K 2 K N/A 10 K .1 K 6 h Mercury ecliptic Y Y Y Y N .1 10 345 N/A N/A 8 GHz 450 K 2 K N/A 10 K .1 K 6 h Mercury ecliptic Y Y Y Y N .1 10 650 N/A N/A 8 GHz 450 K 2 K N/A 10 K .1 K 6 h Mercury ecliptic Y Y Y Y N .05 10 345 N/A N/A 8 GHz 450 K 2 K N/A 10 K .1 K 6 h total 66 h Notes: The mosaics of the Moon will contain some million or so pointings and must be done in OTF interferometer mode. The noise in 10 msec is plenty good enough though, even to get the 0.1 K in polarized brightness. Mercury should be observed at conjunction, which occurs frequently enough that it shouldn't be a problem. ************************************************************************** See program 4.1.1 for general comments Butler and Gurwell Review Mark Gurwell: OK. -------------------------------------------------- Review v2.0: Review of 4.2.1-4.2.8 (no DRSP 2.0 updates received) These projects still remain scientifically valid. Do the additional ALMA bands offer something new (e.g., for projects 4.2.4, 4.2.5)? The integration times are probably still ok eventhough the number of antennas has gone from 64 to 50 - or at least close enough. Several of these projects focus on objects larger than the ALMA primary beam, and mosaicing is needed. Here the ACA and also the ACA in crosscorrelation with the ALMA-12m antennas may be beneficial. ===================================================================================== DRSP 4.2.3 Title Mapping the surfaces of large icy bodies Pi B. Butler Time 104 hrs Title: Mapping the surfaces of large icy bodies Authors: B. Butler Abstract: ALMA will be able to map with unprecedented accuracy and fidelity the millimeter wavelength emission from the solid surfaces of the larger icy bodies in the solar system, including jovian, saturnian, uranian and neptunian satellites, Pluto & Charon, and the larger of the TNOs. Such maps will provide us with information on the thermal and electrical properties of the surface and near-surface, as well as the surface texture - which may hold clues to composition - see, e.g., Muhleman & Berge 1991; Jewitt 1994; Lellouch et al. 2000. contin line poln name RA&DEC m T SD CA sub resn size freq line dfreq BW fd rms fd rms fd rms time ------------ -------- - - -- -- --- ---- ---- ---- ------ -------- ----- ------------ ----------- --------- ------ icy sat/TNO ecliptic Y Y N N N .1 .1-1 345 N/A N/A 8 GHz 50-100 K 1 K N/A 1 K .1 K 40x2 h Pluto/Charon ecliptic Y Y N N N .01 .1 345 N/A N/A 8 GHz 40 K 1 K N/A 1 K .1 K 4x6 h total 104 h ************************************************************************** See program 4.1.1 for general comments Butler and Gurwell Review Mark Gurwell: OK. -------------------------------------------------- Review v2.0: Review of 4.2.1-4.2.8 (no DRSP 2.0 updates received) These projects still remain scientifically valid. Do the additional ALMA bands offer something new (e.g., for projects 4.2.4, 4.2.5)? The integration times are probably still ok eventhough the number of antennas has gone from 64 to 50 - or at least close enough. Several of these projects focus on objects larger than the ALMA primary beam, and mosaicing is needed. Here the ACA and also the ACA in crosscorrelation with the ALMA-12m antennas may be beneficial. ===================================================================================== DRSP 4.2.4 Title Structure and composition of Saturn's rings Pi B. Butler Time 48 hrs Title: Structure and composition of Saturn's rings Authors: B. Butler Abstract: Observations at millimeter wavelengths will constrain the size distribution and properties of the rings of Saturn - see, e.g., Grossman et al. 1989; van der Tak et al. 1999. In addition, structures (density waves, e.g.) will be observed, allowing for constraints on their formation mechanism. contin line poln name RA&DEC m T SD CA sub resn size freq line dfreq BW fd rms fd rms fd rms time ------ -------- - - -- -- --- ---- ---- ---- ------ -------- ----- -------------- ----------- --------- ----- Saturn ecliptic Y Y Y Y N .1 15 90 N/A N/A 8 GHz 10-100 K .5 K N/A 1 K .1 K 4x4 h Saturn ecliptic Y Y Y Y N .1 15 345 N/A N/A 8 GHz 10-100 K .5 K N/A 1 K .1 K 4x4 h Saturn ecliptic Y Y Y Y N .1 15 650 N/A N/A 8 GHz 10-100 K .5 K N/A 1 K .1 K 4x4 h total 48 h ***************************************************************************** See program 4.1.1 for general comments Butler and Gurwell Review Mark Gurwell: I am not sure if "size" of 15" is right for the Saturn ring DRSP...Saturn's rings generally extend much more than this... but otherwise ok Reply Butler: I just put in the size of Saturn, and the rings about double the size. I don't think it matters too much for the purposes of the DRSP, but you are right to point it out and i've corrected it. of course it depends on where it is in its orbit too. Comment Ewine: updated DRSP is now baseline -------------------------------------------------- Review v2.0: Review of 4.2.1-4.2.8 (no DRSP 2.0 updates received) These projects still remain scientifically valid. Do the additional ALMA bands offer something new (e.g., for projects 4.2.4, 4.2.5)? The integration times are probably still ok eventhough the number of antennas has gone from 64 to 50 - or at least close enough. Several of these projects focus on objects larger than the ALMA primary beam, and mosaicing is needed. Here the ACA and also the ACA in crosscorrelation with the ALMA-12m antennas may be beneficial. ===================================================================================== DRSP 4.2.5 Title Mapping the surfaces of larger asteroids Pi B. Butler Time 105 hrs Title: Mapping the surfaces of larger asteroids Authors: B. Butler Abstract: The larger main belt asteroids can be mapped in a way similar to the terrestrial planets, yielding similar information (see that abstract). Information on the structure of the surface and near-surface will help constrain the formation history of these bodies. This kind of observation will also be a requirement for using these bodies (those with diameter >~ 200 km) as secondary calibrators, as their brightness distribution (or at the very least their millimetric light curve) will have to be well known. contin line poln name RA&DEC m T SD CA sub resn size freq line dfreq BW fd rms fd rms fd rms time ---- -------- - - -- -- --- ---- ---- ---- ------ -------- ----- -------------- ----------- --------- ------ MBA ecliptic Y Y N N N .05 .1-1 345 N/A N/A 8 GHz ~100 K 1 K N/A 3 K .1 K 60x1 h MBA ecliptic Y Y N N N 1 .1-1 90 N/A N/A 8 GHz ~100 K 1 K N/A 3 K .1 K 15x1 h MBA ecliptic Y Y N N N 1 .1-1 230 N/A N/A 8 GHz ~100 K 1 K N/A 3 K .1 K 15x1 h MBA ecliptic Y Y N N N 1 .1-1 650 N/A N/A 8 GHz ~100 K 1 K N/A 3 K .1 K 15x1 h total 105 h Note: In an hour, you can do about 10 of the mapping obsns, as the sensitivity in 5 minutes is enough to get 1 K. With roughly 150 of these bodies, and 4 or so observations for each of them for full surface coverage, that gives about 60 1 hour sessions. ************************************************************************ See program 4.1.1. for general comments Butler and Gurwell Review Mark Gurwell: : I am not sure why the 90, 230 and 650 observations are all at much coarser resolution compared to 345. I would suggest similar resolution at at least 90 GHz to the 345 GHz. Reply Butler: The 345 GHz ones were mapping - the others were light curves. I didn't make that very clear. In principle, they could all be high resolution and the light curve drops out of the mapping naturally - I just wanted to distinguish between the two types of observations. -------------------------------------------------- Review v2.0: Review of 4.2.1-4.2.8 (no DRSP 2.0 updates received) These projects still remain scientifically valid. Do the additional ALMA bands offer something new (e.g., for projects 4.2.4, 4.2.5)? The integration times are probably still ok eventhough the number of antennas has gone from 64 to 50 - or at least close enough. Several of these projects focus on objects larger than the ALMA primary beam, and mosaicing is needed. Here the ACA and also the ACA in crosscorrelation with the ALMA-12m antennas may be beneficial. ===================================================================================== DRSP 4.2.6 Title Sizes and albedoes of NEAs Pi B. Butler Time 20 hrs Title: Sizes and albedoes of NEAs Authors: B. Butler Abstract: Thermal emission observations of NEAs, when combined with optical/NIR observations, will provide accurate measures of their sizes and albedoes. This is very similar to the situation with MBAs, where early sizes and albedoes determined from optical observations were found to be seriously in error in many instances when confronted with the more accurate determination from observations of the emission (the crossover wavelength for emission vs. reflection is of order 10 microns). There are generally ~10 NEA opportunities per year. contin line poln name RA&DEC m T SD CA sub resn size freq line dfreq BW fd rms fd rms fd rms time ---- -------- - - -- -- --- ---- ----- ---- ------ -------- ----- -------------- ----------- --------- ------ NEA ecliptic Y Y N N N any small 345 N/A N/A 8 GHz ~200 K 1 K N/A 3 K .1 K 30x1 h total 20 h Note: These will be mostly TOO observations, occurring at truly unpredictable times. ********************************************************************* See program 4.1.1 for general comments Butler and Gurwell Review Mark Gurwell: OK. -------------------------------------------------- Review v2.0: Review of 4.2.1-4.2.8 (no DRSP 2.0 updates received) These projects still remain scientifically valid. Do the additional ALMA bands offer something new (e.g., for projects 4.2.4, 4.2.5)? The integration times are probably still ok eventhough the number of antennas has gone from 64 to 50 - or at least close enough. Several of these projects focus on objects larger than the ALMA primary beam, and mosaicing is needed. Here the ACA and also the ACA in crosscorrelation with the ALMA-12m antennas may be beneficial. ===================================================================================== DRSP 4.2.7 Title Astrometry of NEAs and TNOs Pi B. Butler Time 30 hrs Title: Astrometry of NEAs and TNOs Authors: B. Butler Abstract: ALMA will provide valuable input on the positions, and hence orbits, of NEAs and TNOs - a valuable tool in determining the formation and orbit history and evolution of these bodies. For NEAs, this is particularly important, as observations can be carried out in daytime. contin line poln name RA&DEC m T SD CA sub resn size freq line dfreq BW fd rms fd rms fd rms time ------- -------- - - -- -- --- ---- ----- ---- ------ -------- ----- -------------- ----------- --------- ------- NEA/TNO ecliptic Y Y N N N any small 345 N/A N/A 8 GHz 40-200 K 1 K N/A 3 K .1 K 60x.5 h total 30 h Note: These will be mostly TOO observations, occurring at truly unpredictable times. ***************************************************************** See program 4.1.1. for general comments Butler and Gurwell Review Mark Gurwell: Excellent choice for NEAs but don't see the advantage for TNOs over optical, really. Reply Butler: TNOs are also daytime objects, and the astrometry of ALMA should be *much* better than optical... -------------------------------------------------- Review v2.0: Review of 4.2.1-4.2.8 (no DRSP 2.0 updates received) These projects still remain scientifically valid. Do the additional ALMA bands offer something new (e.g., for projects 4.2.4, 4.2.5)? The integration times are probably still ok eventhough the number of antennas has gone from 64 to 50 - or at least close enough. Several of these projects focus on objects larger than the ALMA primary beam, and mosaicing is needed. Here the ACA and also the ACA in crosscorrelation with the ALMA-12m antennas may be beneficial. ===================================================================================== DRSP 4.2.8 Title Radar observations of NEAs Pi B. Butler Time 12 hrs Title: Radar observations of NEAs Authors: B. Butler Abstract: Radar observations are a powerful way to measure surface and near-surface properties of solid bodies. In addition, orbit and spin state are accurately measured this way - see, e.g., de Pater et al. 1994. contin line poln name RA&DEC m T SD CA sub resn size freq line dfreq BW fd rms fd rms fd rms time ---- -------- - - -- -- --- ---- ----- ---- ------ -------- ------ ---------- --------------- -------------- ----- NEA ecliptic Y Y N N N .05 small 90 radar ~1 Hz 10 kHz N/A 1000 Jy 10 mJy 100 Jy 10 mJy 4x3 h total 12 h Note: These will be purely TOO observations, occurring at unpredictable times. This presumes the existence of a radar transmitting 100 kW through a 50-m aperture at 90 GHz, and that the NEA comes by at the right time (when the array is in spread out configuration). ********************************************************************* See program 4.1.1 for general comments Butler and Gurwell Review Mark Gurwell: Really cool...we should try to keep the radar reception BW needed as a correlator specification! Reply Butler: I need to track this down -------------------------------------------------- Review v2.0: Review of 4.2.1-4.2.8 (no DRSP 2.0 updates received) These projects still remain scientifically valid. Do the additional ALMA bands offer something new (e.g., for projects 4.2.4, 4.2.5)? The integration times are probably still ok eventhough the number of antennas has gone from 64 to 50 - or at least close enough. Several of these projects focus on objects larger than the ALMA primary beam, and mosaicing is needed. Here the ACA and also the ACA in crosscorrelation with the ALMA-12m antennas may be beneficial. ===================================================================================== DRSP 4.3.1 Title A complete picture of an Earth-grazing short-period comet Pi D. Bockelee-Morvan Time 168 hrs 1. Name of program and authors A complete picture of an Earth-grazing short-period comet Authors: D. Bockelee-Morvan, N. Biver, J. Crovisier, J. Boissier 2. One short paragraph with science goal(s) With ALMA it will be possible to determine the relative abundances of a number of species in the coma of a short-period Earth-grazing comet, for comparison with determinations in Oort cloud (long-period) comets. All species identified in comet Hale-Bopp should be detected, leading to the first extensive chemical characterisation of a Jupiter family comet. In addition, several isotopic species will be detected (e.g. HDO, DCN, H13CN, HC15N, CS C- and S isotopes), whose abundances are key indicators of the origin of cometary material. Mapping of a few key lines will be made for comparison of the gas jets morphology to dust jets, and to identify molecules released by grains or formed by molecule decomposition in the coma. Simultaneous monitoring of CO and HCN over a few days is crucial to investigate sublimation and gas dynamic processes at the surface and above the nucleus as the nucleus is rotating. Continuum maps will provide the dust distribution of large sized particles and the dust-to-gas ratio. Attempt will be made to detect the nucleus (probably of order ~1 km radius) on the largest baselines. 3. Number of sources Year dependent. One in 2010 (103P/Hartley 2), one in 2011 (45P/Honda-Mrkos-Padjusakova) though full ALMA not available at that time. 4. Coordinates: 4.1. Rough RA and DEC 4.2. Moving target: yes 4.3. Time critical: yes 4.4. Scheduling constraints: 5. Spatial scales: 5.1. Angular resolution (arcsec): -Compact configuration (1-2 arcsec)for lines -Typically 5 km baselines for nucleus continuum observations (for nucleus/coma contrast > 10) - For weak lines, auto-correlation measurements may be more sensitive 5.2. Range of spatial scales/FOV (arcsec): 5.3. Required pointing accuracy: (arcsec) 0.5" 6. Observational setup 6.1. Single dish total power data: beneficial Observing modes for single dish total power: frequency switch 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: beneficial 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7 7.2. Lines and Frequencies (GHz): multi-line observations 7.3. Spectral resolution (km/s): < 0.1 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 8 GHz in continuum mode depends upon frequency setup in spectroscopic range (e.g. large coverage for covering many lines at the same time) 8. Continuum flux density: Continuum in parallel to line observations 8.1. Typical value (Jy) nucleus : a few mJy for the 2010 and 2011 targets taken as exemples 8.2. Required continuum rms (Jy or K): 8.3. Dynamic range within image: 8.4. Calibration requirements: absolute ( 10% ) repeatability ( 10% ) relative ( 10% ) 9. Line intensity: 9.1. Typical value (K or Jy): depends upon line, from 0.1 to 20 K km/s (HCN4-3) in compact configuration 9.2. Required rms per channel (K or Jy): depends upon line 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute (10%) repeatability (10%) relative (10%) 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): several frequency setup, with different integration times 12. Total integration time for program (hr): 168h 13. Comments on observing strategy : Line mapping requires ALMA to be in compact configuration. Nucleus investigation requires more extended configurations. So, depending of the priority given to one or the other topic, and given the fact that the passage of short-period comets is predictable (in contrast to long-period comets), it would highly desirable to have ALMA in the desired (or as close as possible) configuration at the time of the comet passage. -------------------------------------------------- Review v2.0: Review of 4.3.1-4.3.9 These projects have all been updated to v2.0 and a new, timely project on D/H has been added. One issue that all projects share is their use of the ACA in crosscorrelation with the ALMA-12m antennas. Are the common baselines really essential, or would *simultaneous* (but standalone) ACA observations also work? This might be much easier on the system (slewing times; correlator; ...). Fully standalone (and therefore separate in time) ACA observations for comets obviously make little sense (...although, one could think of cases where some large-scale monitoring could be useful). Comment: the integration times do not seem to be worked out in much detail, although the total times listed seem of the correct magnitude. This may be the best that is currently feasible. (cf. v1.1 where more detailed estimates are given). ===================================================================================== DRSP 4.3.2 Title A TOO observation of an Oort cloud comet Pi D. Bockelee-Morvan Time 168 hrs 1. Name of program and authors A TOO observation of an Oort cloud comet Authors: D. Bockelee-Morvan, N. Biver, J. Crovisier, J. Boissier 2. One short paragraph with science goal(s) This is a target-of-opportunity program for observing a bright new comet with a water production rate of 1.E29 mol/s. Statistically, such a comet appears once per year. With ALMA it will be possible to determine the relative abundances of a number of species in its coma, for comparison with other Oort cloud comets and Jupiter family comets. Minor species identified in comet Hale-Bopp should be detected. In addition, several isotopic species will be observed (e.g. HDO, DCN, H13CN, HC15N, CS C- and S isotopes), whose abundances are key indicators of the origin of cometary material. The observations are very similar to the Earth-grazing comet example. 3. Number of sources Typically one per year 4. Coordinates: 4.1. Rough RA and DEC 4.2. Moving target: yes 4.3. Time critical: yes 4.4. Scheduling constraints: 5. Spatial scales: 5.1. Angular resolution (arcsec): -Compact configuration (1-2 arcsec)for lines -Typically 5 km baselines for nucleus continuum observations (for nucleus/coma contrast > 10) - For weak lines, auto-correlation measurements may be more sensitive 5.2. Range of spatial scales/FOV (arcsec): 5.3. Required pointing accuracy: (arcsec) 0.5" 6. Observational setup 6.1. Single dish total power data: beneficial Observing modes for single dish total power: frequency switch 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: beneficial 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8 7.2. Lines and Frequencies (GHz): multi-line observations 7.3. Spectral resolution (km/s): < 0.1 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 8 GHz in continuum mode depends upon frequency setup in spectroscopic range (e.g. large coverage for covering many lines at the same time) 8. Continuum flux density: 8.1. Typical value (Jy) nucleus : ~ 2 mJy for 10 km size comet nucleus at 1 AU from Earth 8.2. Required continuum rms (Jy or K): 8.3. Dynamic range within image: 8.4. Calibration requirements: absolute ( 10% ) repeatability ( 10% ) relative ( 10% ) 9. Line intensity 9.1. Typical value (K or Jy): depends upon line : 0.1 to 12 K km/s in 2 km/s velocity range for compact comfiguration. 9.2. Required rms per channel (K or Jy): depends upon line 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute (10%) repeatability (10%) relative (10%) 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): several frequency setup, with different integration times 12. Total integration time for program (hr): 168h 13. Comments on observing strategy : Target of Opportunity Line mapping requires ALMA to be in compact configuration. Nucleus investigation requires more extended configurations. So the observing strategy will depend upon Alma configuration at time of comet perihelion. -------------------------------------------------- Review v2.0: Review of 4.3.1-4.3.9 These projects have all been updated to v2.0 and a new, timely project on D/H has been added. One issue that all projects share is their use of the ACA in crosscorrelation with the ALMA-12m antennas. Are the common baselines really essential, or would *simultaneous* (but standalone) ACA observations also work? This might be much easier on the system (slewing times; correlator; ...). Fully standalone (and therefore separate in time) ACA observations for comets obviously make little sense (...although, one could think of cases where some large-scale monitoring could be useful). Comment: the integration times do not seem to be worked out in much detail, although the total times listed seem of the correct magnitude. This may be the best that is currently feasible. (cf. v1.1 where more detailed estimates are given). ===================================================================================== DRSP 4.3.3 Title Observations of the great comet of the decade Pi D. Bockelee-Morvan Time 200 hrs 1. Name of program and authors Observations of the great comet of the decade Authors: D. Bockelee-Morvan, N. Biver, J. Crovisier, J. Boissier 2. One short paragraph with science goal(s) Bright new comets (here referred as comets A), with water production rates ~5E29 molecules/s at perihelion (q~1AU), can be observed statistically once every decade at geocentric distances of typically 1 AU. Active comets (QH2O~1E29 molecules/s) coming close to Earth (~0.1 AU) might be as well expected (comets B) during the first years of operation of ALMA. Observations with ALMA will allow: 1) to characterize their molecular and isotopic composition. New isotopic and molecular species will be searched for. 2) to map the spatial distribution of dust and molecular species with ALMA with unprecedented spatial resolution (specially for comets B), and study its evolution with nucleus rotation. 3) for the most productive comets (comets A), to monitor their dust and gaseous activity as a function of heliocentric distance. 3. Number of sources One of each of type A & B comets might be observed over a 3 year period (plus monitoring). These will be truly TOO observations, occurring at a completely unpredictable time. 4. Coordinates: 4.1. Rough RA and DEC 4.2. Moving target: yes 4.3. Time critical: yes 4.4. Scheduling constraints: 5. Spatial scales: 5.1. Angular resolution (arcsec): -Compact configuration (1-2 arcsec)for lines -Typically 5 km baselines for nucleus continuum observations (for nucleus/coma contrast > 10) - For weak lines, auto-correlation measurements may be more sensitive 5.2. Range of spatial scales/FOV (arcsec): 5.3. Required pointing accuracy: (arcsec) 0.5" 6. Observational setup 6.1. Single dish total power data: beneficial Observing modes for single dish total power: frequency switch 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: beneficial 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8 7.2. Lines and Frequencies (GHz): multi-line observations 7.3. Spectral resolution (km/s): < 0.1 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 8 GHz in continuum mode depends upon frequency setup in spectroscopic range (e.g. large coverage for covering many lines at the same time) 8. Continuum flux density: 8.1. Typical value (Jy) nucleus : ~2 mJy for 10 km size comet nucleus at 1 AU from Earth 8.2. Required continuum rms (Jy or K): 8.3. Dynamic range within image: 8.4. Calibration requirements: absolute ( 10% ) repeatability ( 10% ) relative ( 10% ) 9. Line intensity 9.1. Typical value (K or Jy): depends upon line At perihelion: 0.1 to 50 K km/s for compact configuration in 2 km/s velocity range. 9.2. Required rms per channel (K or Jy): depends upon line 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute (10%) repeatability (10%) relative (10%) 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): several frequency setup, with different integration times 12. Total integration time for program (hr): 200 h 13. Comments on observing strategy : Target of Opportunity Line mapping requires ALMA to be in compact configuration. Nucleus investigation requires more extended configurations. So the observing strategy will depend upon Alma configuration at time of comet perihelion. Line monitoring : can be done in single-dish mode -------------------------------------------------- Review v2.0: Review of 4.3.1-4.3.9 These projects have all been updated to v2.0 and a new, timely project on D/H has been added. One issue that all projects share is their use of the ACA in crosscorrelation with the ALMA-12m antennas. Are the common baselines really essential, or would *simultaneous* (but standalone) ACA observations also work? This might be much easier on the system (slewing times; correlator; ...). Fully standalone (and therefore separate in time) ACA observations for comets obviously make little sense (...although, one could think of cases where some large-scale monitoring could be useful). Comment: the integration times do not seem to be worked out in much detail, although the total times listed seem of the correct magnitude. This may be the best that is currently feasible. (cf. v1.1 where more detailed estimates are given). ===================================================================================== DRSP 4.3.4 Title Characterization of the Jupiter-family comet population Pi D. Bockelee-Morva Time 200 hrs 1. Name of program and authors Characterization of the Jupiter-family comet population Authors: D. Bockelee-Morvan, N. Biver, J. Crovisier, J. Boissier 2. One short paragraph with science goal(s) About 30 comets have been observed by millimetre/submillimetre spectroscopy. A large diversity is observed in the relative abundances of parent molecules, such as HCN, CO, H2S, H2CO ... etc. However, only a few Jupiter-family comets could have been investigated because of their low activity, while they may present distinct composition with respect to Oort cloud comets. The sensitivity of ALMA opens a new window for establishing their composition. We propose to observe a few Jupiter-family comets (other than Earth-grazers) spectroscopically. We also propose to observe at least a few of them for thermal emission from the nucleus, at least Comet 81P/Wild 2 (target of NASA Stardust mission) and 10P/Tempel 2. 3. Number of sources one every two years 4. Coordinates: 4.1. Rough RA and DEC 4.2. Moving target: yes 4.3. Time critical: yes 4.4. Scheduling constraints: 5. Spatial scales: 5.1. Angular resolution (arcsec): -Compact configuration (1-2 arcsec)for lines -Typically 5 km baselines for nucleus continuum observations (for nucleus/coma contrast > 10) - For weak lines, auto-correlation measurements may be more sensitive 5.2. Range of spatial scales/FOV (arcsec): 5.3. Required pointing accuracy: (arcsec) 0.5" 6. Observational setup 6.1. Single dish total power data: beneficial Observing modes for single dish total power: frequency switch 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: beneficial 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 3, 4, 5, 6, 7, 8 7.2. Lines and Frequencies (GHz): multi-line observations 7.3. Spectral resolution (km/s): < 0.1 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 8 GHz in continuum mode depends upon frequency setup in spectroscopic range (e.g. large coverage for covering many lines at the same time) 8. Continuum flux density: 8.1. Typical value (Jy) nucleus : 0.02 mJy for 1 km size comet nucleus at 1 AU from Earth 8.2. Required continuum rms (Jy or K): 8.3. Dynamic range within image: 8.4. Calibration requirements: absolute ( 10% ) repeatability ( 10% ) relative ( 10% ) 9. Line intensity 9.1. Typical value (K or Jy): depends upon line from 0.02 to 3 K km/s (2 km/s line widths) in compact configuration 9.2. Required rms per channel (K or Jy): depends upon line, S/N > 5 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute (10%) repeatability (10%) relative (10%) 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): several frequency setup, with different integration times 12. Total integration time for program (hr): 200 h 13. Comments on observing strategy : Target of Opportunity Line mapping requires ALMA to be in compact configuration. Nucleus investigation requires more extended configurations. So the observing strategy will depend upon Alma configuration at time of comet perihelion. Line monitoring : can be done in single-dish mode -------------------------------------------------- Review v2.0: Review of 4.3.1-4.3.9 These projects have all been updated to v2.0 and a new, timely project on D/H has been added. One issue that all projects share is their use of the ACA in crosscorrelation with the ALMA-12m antennas. Are the common baselines really essential, or would *simultaneous* (but standalone) ACA observations also work? This might be much easier on the system (slewing times; correlator; ...). Fully standalone (and therefore separate in time) ACA observations for comets obviously make little sense (...although, one could think of cases where some large-scale monitoring could be useful). Comment: the integration times do not seem to be worked out in much detail, although the total times listed seem of the correct magnitude. This may be the best that is currently feasible. (cf. v1.1 where more detailed estimates are given). ===================================================================================== DRSP 4.3.5 Title is Hale-Bopp still alive? Pi D. Bockelee-Morvan Time 12 hrs 1. Name of program and authors Is Hale-Bopp still alive? Authors: D. Bockelee-Morvan, N. Biver, J. Crovisier, J. Boissier 2. One short paragraph with science goal(s) CO outgassing is controlling cometary gaseous activity at large heliocentric distances. The CO J(2-1) line was detected in comet C/1995 O1 (Hale-Bopp) up to 14 AU from the Sun using the SEST telescope. At the beginning of 2011, Hale-Bopp will be at 31 AU from the Sun and Earth. With deep integration with ALMA, we may be able to recover the CO 230 GHz line. The line area over 0.6 km/s is expected to be 0.0006 K km/s (T main beam), for a CO production rate of QCO=1.1E27 mol/s. This production rate is expected if QCO decreases as the square of heliocentric distance (as observed between 1 and 14 AU). But modelling of sublimation processes often predicts a much smaller decrease as due to sublimation from deep layers inside the nucleus. 3. Number of sources 1 4. Coordinates: 4.1. Rough RA and DEC RA = 0 DEC = -85 4.2. Moving target: yes 4.3. Time critical: no, but we cannot wait years ... 4.4. Scheduling constraints: 5. Spatial scales: 5.1. Angular resolution (arcsec): Compact configuration (1-2 arcsec) or single-dish 5.2. Range of spatial scales/FOV (arcsec): 5.3. Required pointing accuracy: (arcsec) 0.5" 6. Observational setup 6.1. Single dish total power data: beneficial Observing modes for single dish total power: frequency switch 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: 6 7.2. Lines and Frequencies (GHz): CO (2-1) 7.3. Spectral resolution (km/s): < 0.05 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 20 km/s 8. Continuum flux density: 9. Line intensity 9.1. Typical value (K or Jy): 0.0006 K km/s in single-dish mode 9.2. Required rms per channel (K or Jy): 0.0001 K km/s over 0.6 km/s in single-dish mode 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute (10%) repeatability (10%) relative (10%) 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): 12 h 12. Total integration time for program (hr): 13. Comments on observing strategy : -------------------------------------------------- Review v2.0: Review of 4.3.1-4.3.9 These projects have all been updated to v2.0 and a new, timely project on D/H has been added. One issue that all projects share is their use of the ACA in crosscorrelation with the ALMA-12m antennas. Are the common baselines really essential, or would *simultaneous* (but standalone) ACA observations also work? This might be much easier on the system (slewing times; correlator; ...). Fully standalone (and therefore separate in time) ACA observations for comets obviously make little sense (...although, one could think of cases where some large-scale monitoring could be useful). Comment: the integration times do not seem to be worked out in much detail, although the total times listed seem of the correct magnitude. This may be the best that is currently feasible. (cf. v1.1 where more detailed estimates are given). ===================================================================================== DRSP 4.3.6 Title Chiron distant activity Pi D. Bockelee-Morvan Time 5 hr 1. Name of program and authors Chiron distant activity Authors: D. Bockelee-Morvan, N. Biver, J. Crovisier, J. Boissier 2. One short paragraph with science goal(s) (2060) Chiron is a Centaur which orbits around the Sun between 8.5 and 18.9 AU and presents cometary-like activity, with a well developed dust coma and frequent outbursts. CO outgassing is likely at the origin of this activity, while CN is the only gaseous species detected in the coma. We propose to search for the CO J(2-1) and HCN J(1-0) lines with unprecedented sensitivity with ALMA. 3. Number of sources 1 4. Coordinates: 4.1. Rough RA and DEC 4.2. Moving target: yes 4.3. Time critical: no 4.4. Scheduling constraints: 5. Spatial scales: 5.1. Angular resolution (arcsec): Compact configuration (1-2 arcsec) or single-dish 5.2. Range of spatial scales/FOV (arcsec): 5.3. Required pointing accuracy: (arcsec) 0.5" 6. Observational setup 6.1. Single dish total power data: beneficial Observing modes for single dish total power: frequency switch 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: 3, 6 7.2. Lines and Frequencies (GHz): CO (2-1) 7.3. Spectral resolution (km/s): < 0.05 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 20 km/s 8. Continuum flux density: 9. Line intensity 9.1. Typical value (K or Jy): ? 9.2. Required rms per channel (K or Jy): 0.0015 K km/s over 0.1 km/s in single-dish mode at 230 GHz 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute (10%) repeatability (10%) relative (10%) 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): 12. Total integration time for program (hr): 5 hr 13. Comments on observing strategy : -------------------------------------------------- Review v2.0: Review of 4.3.1-4.3.9 These projects have all been updated to v2.0 and a new, timely project on D/H has been added. One issue that all projects share is their use of the ACA in crosscorrelation with the ALMA-12m antennas. Are the common baselines really essential, or would *simultaneous* (but standalone) ACA observations also work? This might be much easier on the system (slewing times; correlator; ...). Fully standalone (and therefore separate in time) ACA observations for comets obviously make little sense (...although, one could think of cases where some large-scale monitoring could be useful). Comment: the integration times do not seem to be worked out in much detail, although the total times listed seem of the correct magnitude. This may be the best that is currently feasible. (cf. v1.1 where more detailed estimates are given). ===================================================================================== DRSP 4.3.7 Title CO nucleus outgassing of 29P/Schwassmann-Wachmann 1 Pi D. Bockelee-Morvan Time 1. Name of program and authors CO nucleus outgassing of 29P/Schwassmann-Wachmann 1 Authors: D. Bockelee-Morvan, N. Biver, J. Crovisier, J. Boissier 2. One short paragraph with science goal(s) Comet 29P/Schwassmann-Wachmann 1 is an unusual comet which orbits on an almost circular orbit at ~6 AU from the Sun. It shows a well developed dusty coma and recurrent outbursts. CO is the only detected parent molecule (through millimeter observations), and likely one of the main drivers of this activity. Maps of the CO J(2-1) line profiles show that its brightness distribution is more extended than expected. This can be due to gas temperature variations in the coma. Diffuse production in the coma by icy grains is also not excluded. Interferometric maps will unravel CO outgassing from the nucleus and the kinematics of the inner coma. 3. Number of sources 1 4. Coordinates: 4.1. Rough RA and DEC DEC about 0 4.2. Moving target: yes 4.3. Time critical: no 4.4. Scheduling constraints: 5. Spatial scales: 5.1. Angular resolution (arcsec): Compact configuration (1 arcsec at 230 GHz to 3 arsec at 115 GHz) 5.2. Range of spatial scales/FOV (arcsec): 5.3. Required pointing accuracy: (arcsec) 0.5" 6. Observational setup 6.1. Single dish total power data: beneficial Observing modes for single dish total power: frequency switch 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: beneficial 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: 3, 6 7.2. Lines and Frequencies (GHz): CO (2-1) 230 GHz CO (1-0) 115 GHz 7.3. Spectral resolution (km/s): < 0.05 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): 20 km/s 8. Continuum flux density: 9. Line intensity 9.1. Typical value (K or Jy): 1 K km/s with 1" resolution over 1 km/s for CO2-1 0.5 K km/s with 3" resolution over 1 km/s for CO(1-0) 9.2. Required rms per channel (K or Jy): 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute (10%) repeatability (10%) relative (10%) 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): 230 GHz: 7h 115 GHz: 7h 12. Total integration time for program (hr): 14 hr 13. Comments on observing strategy : -------------------------------------------------- Review v2.0: Review of 4.3.1-4.3.9 These projects have all been updated to v2.0 and a new, timely project on D/H has been added. One issue that all projects share is their use of the ACA in crosscorrelation with the ALMA-12m antennas. Are the common baselines really essential, or would *simultaneous* (but standalone) ACA observations also work? This might be much easier on the system (slewing times; correlator; ...). Fully standalone (and therefore separate in time) ACA observations for comets obviously make little sense (...although, one could think of cases where some large-scale monitoring could be useful). Comment: the integration times do not seem to be worked out in much detail, although the total times listed seem of the correct magnitude. This may be the best that is currently feasible. (cf. v1.1 where more detailed estimates are given). ===================================================================================== DRSP 4.3.8 Title CO nucleus outgassing of 29P/Schwassmann-Wachmann 1 Pi D. Bockelee-Morvan Time 40 hrs Title: CO nucleus outgassing of 29P/Schwassmann-Wachmann 1 Authors: D. Bockelee-Morvan, N. Biver, J. Crovisier, F. Henry Abstract: Comet 29P/Schwassmann-Wachmann 1 is an unusual comet which orbits on an almost circular orbit at ~6 AU from the Sun. It shows a well developed dusty coma and recurrent outbursts. CO is the only detected parent molecule (through millimeter observations), and likely one of the main drivers of this activity. Maps of the CO J(2-1) line profiles show that part of the CO is not directly released by the nucleus, but presents a much more extended distribution due to diffuse production in the coma by possibly icy grains or a parent species, like CO2. By filtering the diffuse CO coma, interferometric maps will unravel CO outgassing from the nucleus and the kinematics of the inner coma. contin line poln name RA&DEC m T SD CA sub resn size freq line dfreq BW fd rms fd rms fd rms time -------- ----------- - - -- -- --- ---- ---- ---- ------ -------- ------- ------------ ----------- --------- ------- 29P/S-W1 ecliptic Y N Y Y N .5 ?? 230 CO 10 kHz 20 km/s N/A 1 K .2 K N/A 40 h total 40 h ****************************************************************************** Review Mark Gurwell: OK. Note Bockelee-Morvan: This observation is not time critical. ===================================================================================== DRSP 4.3.9 Title D/H in cometary water Pi D. Bockelée-Morvan Time 10 hrs per year 1. Name of program and authors D/H in cometary water D. Bockelée-Morvan 2. One short paragraph with science goal(s) The D/H ratio in cometary water is a key parameter to constrain the origin of cometary ices. It complements values measured in other Solar System bodies, proto-planetary disks and star-forming regions for a better understanding of Solar System and planetary formation. It has only been measured in 3 comets coming from the Oort cloud with similar values (~3 E-4). The goal is to obtain measurements in a larger sample of comets, including short-period comets coming from the Kuiper Belt. 3. Number of sources Several. Typically one favourable long-period each year, one short-period every two years. Two interesting short-period comets in 2010 (103P/Hartley 2) and 2011 (45P/Honda-Mrkos-Padjusakova). 4. Coordinates: 4.1. Rough RA and DEC 4.2. Moving target: yes 4.3. Time critical: yes 4.4. Scheduling constraints: (optional) 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.75" (compact configuration) 5.2. Range of spatial scales/FOV (arcsec): 5.3. Required pointing accuracy: (arcsec) 0.5" (ephemeris accuracy will be about 1-2") 6. Observational setup 6.1. Single dish total power data: Possibly sloghtly better sensitivity with 54 antennas in total power Observing modes for single dish total power: frequency switch 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: beneficial only for strong sources (active comets with QH2O > 5 E29 s-1) 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: 8 7.2. Lines and Frequencies (GHz): HDO 465 GHz Methanol lines in the same frequency set-up for reference 7.3. Spectral resolution (km/s): < 0.1 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): Adapted to cover strong methanol lines in signal or image bands. 8. Continuum flux density: 9. Line intensity: 9.1. Typical value (K or Jy): From 0.1 K km/s (short-period comet with QH2O=E28 s-1 at Earth distance of 1 AU) to 4 K km/s (long-period comet with QH2O=5E29 s-1 at Earth distance of 1 AU). Typical long-period comet: 0.9 K km/s. Line width is about 1.5 km/s. Angular resolution of 0.75" is assumed. 9.2. Required rms per channel (K or Jy): the value for detection with S/N > 5 ALMA sensitivity estimator gives 0.1 K km/s in 1h for 0.75" angular resolution. 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute (5%) repeatability (10%) relative (5%) 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): 1 to 10 hours depending on the comet 12. Total integration time for program (hr): Say at most 10 h per year 13. Comments on observing strategy : (optional) Target of Opportunity -------------------------------------------------- Review v2.0: Review of 4.3.1-4.3.9 These projects have all been updated to v2.0 and a new, timely project on D/H has been added. One issue that all projects share is their use of the ACA in crosscorrelation with the ALMA-12m antennas. Are the common baselines really essential, or would *simultaneous* (but standalone) ACA observations also work? This might be much easier on the system (slewing times; correlator; ...). Fully standalone (and therefore separate in time) ACA observations for comets obviously make little sense (...although, one could think of cases where some large-scale monitoring could be useful). Comment: the integration times do not seem to be worked out in much detail, although the total times listed seem of the correct magnitude. This may be the best that is currently feasible. (cf. v1.1 where more detailed estimates are given). ===================================================================================== DRSP 4.4.1 Title Direct detection of Jupiters around nearby solar-like stars Pi K. M. Menten Time 500 hrs 1. Name: Direct detection of Jupiters around nearby solar-like stars Author: K. M. Menten (kmenten@mpifr-bonn.mpg.de) 2. Science goal: Detect Jupiter at the distance of alpha Centauri (D = 1.34 pc) and around start out to 5 pc. Jupiter at alpha Cen's distance would have a 345 GHz flux density of 6 microJy, while alpha Cen A (G2 V) itself is expected to have a flux density of 19 mJy at this frequency. A Jupiter-like planet moving on the same orbit around alpha Cen A as the real Jupiter around the Sun would, at maximum elongation, appear at a projected distance of 3.9" from alpha Cen A. Using ALMA, this planet could be detected at the 4 sigma level in ~250 hours. The dynamic range of ~10000 (i.e. maximum signal over rms noise) necessary for this observation should be easily reachable, given that self-calibration can be employed using alpha Cen A as a reference. Self calibration will be possible as long as the reference star is detected on each baseline at a few, say 3, sigma within a coherence time, t_coh. If we assume t_coh = 20 sec, we find an SNR of 3 for a single baseline, making self-calibation on alpha Cen A easily feasible. Significantly longer coherence times might be expected, allowing self-calibration for stars at greater distances. Once coherence is achieved with self calibration, long integrations are possible; e.g. 3500 hours of observing time would be required for a 5 sigma$ detection of "Jupiter" at D = 5 pc. Other possible target stars observable with ALMA within or around that distance include tau Cet, Sirius, Procyon, Altair, and sigma Pav. 3. Number of sources: 6 4. Coordinates: 4.1. Solar-like stars within 5 pc: tau Cet (G8 VI, D = 3.6 pc) 01 44 04.08 -15 56 14.9 Sirius (A1 V, D = 2.7 pc) 06 45 08.92 -16 42 58.0 Procyon (F5 V, D = 3.5 pc) 07 39 18.12 +05 13 30.0 alpha Cen (G2 V, D=1.34 pc) 14 39 36.20 -60 50 08.2 Altair (A7 V, D = 5.1 pc) 19 50 47.00 +08 52 06.0 sigma Pav (G6 V, D = 5.7 pc) 20 49 18.17 -68 46 35.5 (All coordinates are J2000) 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.1" 5.2. Range of spatial scales/FOV: point source(s) spread over a few arcseconds. 5.3 required pointing accuracy: 6 Observational Setup 6.1 Single dish total power data: no 6.2 stand-alone ACA: no 6.3 Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 7 7.2. Line: none 7.3. Spectral resolution (km/s): N/A 7.4. Spectral coverage (km/s or GHz): N/A 8. Continuum flux density: 8.1. Typical value: a few microJy (planets) 5 - 20 mJy (host stars) 8.2. Required continuum rms: 0.1 microJy 8.3. Dynamic range in image: 10000 8.4. Calibration requirements: absolute 10% repeatability 10% relative 10% 9. Line intensity: 9.1. Typical value: none 9.2. Required rms per channel: N/A 9.3. Spectral dynamic range: N/A 10. Polarization: no 11. Integration time per setting: 250 - 3500 h 12. Total integration time for program: ~10000 hr => reduce to 500 hr 13. Comments on observing strategy ************************************************************************** Review Leonardo Testi: The proposal is challenging but sound. It may be unfeasible to do ALL this programme in the three years covered by the DRSP. One could reasonably consider to do 2 of the closest targets in the 3yrs timeframe, corresponding to approx 1000hrs. Or even limit at the proof of concept on alpha Centauri with 250hrs. Reply Butler: I think this program might be done in the later days of ALMA but i think it has no place in the DRSP. As far as i know, there has never been a claimed detection of an EGP around any of these stars. eps eri is the closest that i know of, and that one is hotly disputed. to propose to use 10000 hours is, well, i think an extreme overcommitment of time. i had suggested that you scrap this entry altogether previously, and i still think this is what should be done. given 2500 hours for all of the proposals in this entire theme, i would not suggest even using 500 for this type of proposal. Comment Mark Gurwell: We (should? could?) include comments that observations of Jupiter and Saturn in our solar system show incredibly deep and broad absorption due to PH3 at 267 GHz (see for example section 4.1.5). In a selected case of a few very nearby objects (1.3 to maybe 3 pc), focused observations of a few hundred to few thousand hours could in fact detect such absorption from a Jupiter or maybe even a Saturn (its not the mass that matters as much as the stellar-planet distance)...with enough integration the line shape could be roughly determined and give some information on the temperature structure of the atmosphere. Comment Ewine: There will undoubtedly be proposal pressure to observe exo-planets with ALMA and it is likely at least some of them will be approved by the TAC. Therefore, 500 hrs has been reserved for this theme (one several M_J exo-planet) and the total time for this theme has been increased. -------------------------------------------------- Review v2.0: Review of 4.4.1-4.4.3 No updated required w.r.t. DRSP 1.1. Integration times still formally hold for 64 antennas, so either increase the total times by 30% or reduce the sensitivity by 14%. Other, unknown factors in the sensitivity and performance will be larger than this correction. R.: This program is not jeopardized by the reduction of the number of antennae. Target list can be adjusted. The key point of this astrometric programm is the performance of ALMA in the extended configuration to benefit of the highest angular resolution of the instrument. ===================================================================================== DRSP 4.4.2 Title Dynamical parameters of extrasolar planets by ALMA astrometry Pi J-F Lestrade Time 100 hrs 1. Name: Dynamical parameters of extrasolar planets by ALMA astrometry Authors: J-F Lestrade, K.M. Menten (Jean-François.LESTRADE@obspm.fr) 2. Science goal: ALMA Astrometry with a theoretical precision of 0.1 milliarcsecond can yield important dynamical parameters of extrasolar planets - masses, inclinations and nodes of orbits - that radial velocity measurements cannot provide. ALMA has the capability to detect directly the thermal emission of the photospheres of 446 nearby stars in the Gleise and Jarheiss (1991) catalogue with reasonable integration times. Wobbles of these stars could be searched to discover new planets with masses as low as 0.1 Jupiter and orbital periods of ~ 10 years. Differently, ALMA could complement the determination of the system orbital parameters for the 46 stars that have known planets from radial velicity surveys and are also detectable by ALMA. We anticipate that the first series of observations will have to demonstrate that the phase-referencing technique combined with the fast switching mode of observation can provide the required high sensitivity (submJy) and proper calibration of the rapid phase fluctuations of the atmosphere. This astrometric programm requires that the most extended configuration of baselines be used and, possibly, militate for a larger array than currently designed. 3. Number of sources: 446 4. Coordinates: 4.1. All over the ALMA sky 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: < 0.020" 5.2. Range of spatial scales/FOV: 0.005'' - 0.001'' 5.3 Positional accuracy 6. Observational Setup 6.1. Single dish total power data: no 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: 345 GHz 7.2. Line: N/A 7.3. Spectral resolution (km/s): N/A 7.4. Spectral coverage (km/s or GHz): N/A 8. Continuum flux density: 8.1. Typical value: 0.2 mJy 8.2. Required continuum rms (Jy or K): 0.01 mJy 8.3. Dynamic range within image: low 8.3. Required continuum rms: 0.01 mJy 8.4. Calibration requirements: absolute N/A repeatability N/A relative N/A 9. Line intensity: 9.1. Typical value : N/A 9.2. Required rms per channel: N/A 9.3. Spectral dynamic range: N/A 10. Polarization: no 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time per setting: 5 hrs 12. Total integration time for program: 100 hr 13. Comments on observing strategy : The tricky part of this project will be instead PHASE CALIBRATION, both instrumental and atmospheric. We expect that phase referencing relative to an angularly nearby calibrator will do it as succesfully demonstrated at lower frequencies. Position accuracy required for the calibrators is 10 milliarcsecond or better. *************************************************************************** Review Leonardo Testi: These two are essentially the same project and should be combined. The requirements set by the two authors are, however very different both in terms of the number of sources and the integration time per source and the expected return. It is hard for me to judge who is right: 4.4.2 asserts that you need to reach 0.01 mJy/beam sensitivity and that you can only access ~450 sources; 4.4.3 requires 0.1 mJy/beam and claim that one can observe up to ~1500 stars. Note that the time estimate in 4.3.2 is wrong: 5h are needed to reach the S/N per star and per single observation (one needs many to detect the wobble), the total time of 100h is for 1 observation of 20 objects ?? A key point which is missing is the required positional accuracy and its relation with the observing parameters (flux of targets, signal to noise required etc)... especially in 4.4.3 which quotes flux densities down to 0.1mJy and requires rms~0.1mJy. It is clearly a project that will be tried with ALMA. My feeling is that we should have one such proposals in the DRSP with something like 100-150 hours, which will correspond to observations of a sample of a few tens of the best candidates. Reply Butler: Merging 4.4.2 and 4.4.3 makes perfect sense to me. I point to my recent memo (with al and bob brown) for justification of the numbers I used at: http://www.alma.nrao.edu/memos/html-memos/abstracts/abs475.html . There is also a section in that memo on direct detection. One difference between the two "proposals" is that 4.4.2 suggests to also observe in detail the stars which already have confirmed planets (from radial velocity studies). i didn't include that part in 4.4.3. Beyond that difference, yes, i think they've overestimated the number of stars we can do this on. But in the end, the two "proposals" ask for roughly the same amount of time, so i think it makes sense to just set aside 100-150 hours for this kind of work, and not worry to much about the details. Comment Ewine: keep two separate programs; 250 hrs in total for this important science seems very reasonable. -------------------------------------------------- Review v2.0: Review of 4.4.1-4.4.3 No updated required w.r.t. DRSP 1.1. Integration times still formally hold for 64 antennas, so either increase the total times by 30% or reduce the sensitivity by 14%. Other, unknown factors in the sensitivity and performance will be larger than this correction. R.: This program is not jeopardized by the reduction of the number of antennae. Target list can be adjusted. The key point of this astrometric programm is the performance of ALMA in the extended configuration to benefit of the highest angular resolution of the instrument. ===================================================================================== DRSP 4.4.3 Title Search for extrasolar planets via astrometry of nearby stars Pi B. Butler Time 144 hrs 1. Title: Search for extrasolar planets via astrometry of nearby stars Authors: B. Butler program 4.4.3 2. Science goal: The orbit of any planet around its central star causes that star to undergo a reflexive circular motion around the star-planet barycenter. By taking advantage of the incredibly high resolution of ALMA in its widest configuration, we may be able to detect this motion. Taking the stellar catalogs of Gliese & Jahreiss (1988) and Hipparcos (Perryman et al. 1997), and computing how many of these might have detectable wobble gives: companion mass # G&J # Hipp 5*jovian 200 800 jovian 120 180 neptunian 30 0 Details are in Butler & Wootten (2000). Realistically, we might expect to monitor some few hundred of these, perhaps up to 1000, notably the solar-type ones in the G&J catalog (of which there are 130 total). Each observation takes about 1 minute, so with overhead this might be 1 day total for each set of observations (for 1000 stars), which would be spread over several days to get the required sky coverage. We will require at least 3 different epochs, and likely more - a reasonable estimate might be one set of observations per 6 months, meaning 6 total sets of observations in 3 years. 3. number of sources: 100 - 1000 4. Coordinates: 4.1. all over the ALMA sky 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 0.01" 5.2. Range of spatial scales/FOV: small 5.3 Positional accuracy: 0.1 milli-arcsecond 6. Observational Setup 6.1. Single dish total power data: no 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: 345 GHz 7.2. Line: N/A 7.3. Spectral resolution (km/s): N/A 7.4. Spectral coverage (km/s or GHz): N/A 8. Continuum flux density: 8.1. Typical value: 0.1 - 10 mJy 8.2. Required continuum rms (Jy or K): 0.1 mJy 8.3. Dynamic range within image: low 8.3. Required continuum rms: 0.01 mJy 8.4. Calibration requirements: absolute N/A repeatability N/A relative N/A 9. Line intensity: 9.1. Typical value : N/A 9.2. Required rms per channel: N/A 9.3. Spectral dynamic range: N/A 10. Polarization: no 10.1. Required Stokes parameters: N/A 10.2. Total polarized flux density (Jy): N/A 10.3. Required polarization rms and/or dynamic range: N/A 10.4. Polarization fidelity: N/A 10.5. Required calibration accuracy: N/A 11. Integration time per setting: 24 hrs 12. Total integration time for program: 144 hr 13. Comments on observing strategy : These are moving, albeit relatively slowly, but it will have to be accounted for properly since this is astrometry. The timing is not critical, except to separate the sessions by some period of roughly 6 months. ----------------------------------------- Review Leonardo Testi: See program 4.4.2 -------------------------------------------------- Review v2.0: Review of 4.4.1-4.4.3 No updated required w.r.t. DRSP 1.1. Integration times still formally hold for 64 antennas, so either increase the total times by 30% or reduce the sensitivity by 14%. Other, unknown factors in the sensitivity and performance will be larger than this correction. R.: This program is not jeopardized by the reduction of the number of antennae. Target list can be adjusted. The key point of this astrometric programm is the performance of ALMA in the extended configuration to benefit of the highest angular resolution of the instrument. ===================================================================================== DRSP 5.1.1 Title The general relativistic shadow of Sgr A* Pi C. Carilli Time 16 hrs 5.1.1: Name -- The general relativistic shadow of Sgr A* Authors: C. Carilli 2. Science goal: We propose VLBI imaging at 220 GHz of Sgr A* using the 'Pacific array' (see note below). These observations will allow for reasonable imaging at 20 uas resolution, well matched to the scale of the expected general relativistic shadow of the SMBH in Sgr A* (Falcke et al.2000 528, L13). These observations will provide the final evidence for the existence of a SMBH at the Galactic center, provide a fundamental test of strong field GR, and are the most direct method for separating a Kerr (ie. spinning) from a Schwarzschild black hole. At a minimum, the sensitivity per baseline is adequate to perform model fitting on relatively short timescales (minutes), while the array itself has enough antennas to provide both closure amplitude and phases, and hence should be adequate for hybrid imaging of the GR shadow of Sgr A*. The existence of reasonable mm-VLBI calibrators (eg NRAO 530) in the vicinity of Sgr A* will allow for phase-referenced fringe fitting, although the source itself is strong enough, and the UV coverage dense enough, to allow for hybrid mapping as well. The source Sgr A* has been detected at 220 GHz on the PdBI -- Pico Veleta baseline (resolution = 300 uas) with a flux density of 2.0 Jy, and an upper limit to the size of order 100 uas (Krichbaum et al. 1998 335, L106). The proposed observations will have more than an order of magnitude better resolution, more than two orders of magnitude better sensitivity, and, again, enough antennas to perform proper imaging of Sgr A*. 3. Number of sources: 1 4. Coordinates: 4.1. 1742-2859 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 20uas 5.2. Range of spatial scales/FOV: 20 uas -- 100 uas 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 6 -- 220 GHz in Configuration D or E, phased array 6.2. Lines and Frequencies 6.3. Spectral Resolution (km/s) 6.4. Bandwidth or spectral coverage: 1 GHz x 2pol (set by VLBI recorder) 7. Continuum flux density: 7.1. Typical value: 7.2. Continuum peak value: <= 2 Jy 7.3. Required continuum rms: ALMA - HHT baseline, 10 min rms = 0.7 mJy ALMA - LMT baseline, 10 min rms = 0.2 mJy 7.4. Dynamic range in image: 1e3 8. Line intensity: 8.1. Typical value: 8.2. Required rms per channel: 8.3. Spectral dynamic range: 9. Polarization: yes 10. Integration time per setting: 4 tracks of 4hrs each 11. Total integration time for program: 16 hr Notes: The pacific array at 220 GHz consists of: ALMA, HHT, LMT, CARMA, and any of CSO/JCMT/SMA. We estimate mutual visibility of Sgr A* of about 4hrs. Note that an Atlantic array might also be considered, including PdBI, IRAM 30m. **************************************************************************** Review Jean Turner: Fascinating project to detect the "shadow" of Sgr A*, which is predicted to be at 10 Rsch. If the hole is spinning (Kerr) the shadow will be flattened and offset. Unclear from the proposal what will be seen, or what is "shadowed" in the radio but whatever is there in SgrA* is well worth the effort. This is a modest amount of time for a great project. I have to take Chris's numbers on faith since they involve other telescopes and VLBI. They seem very reasonable given the ALMA sensitivities. -------------------------------------------------- Review v2.0: 1.6.3 The general releativisitic shadow of Sgr A* (Carilli) Not revised since DRSP 1.1. Nothing needs to be added to the review back then, no severe impact through reduction to 50 antennas, no need for ACA. ===================================================================================== DRSP 5.1.2 Title mm VLBI observations of core-jets Pi C. Carilli Time 50 hrs 5.1.2: Name -- mm VLBI observations of core-jets Authors: C. Carilli 2. Science goal: We propose VLBI imaging using the Pacific array (see 1.6.3) at 220 GHz of a representative sample of radio jets in low redshift radio galaxies. These data will probe to scales of 20uas, corresponding to 50 Schwarzschild radii at the distance of M87 (17 Mpc). Observations of M87 suggest that these scales correspond to the fundamental regime where initial jet collimation occurs (Junor et al. 1999 Nature 401, 891). Hence these observations will provide a key test of jet formation models in radio galaxies. 3. Number of sources: 10 4. Coordinates: 4.1. Choose equatorial sources: Declination = 0 +/- 10deg 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 20uas 5.2. Range of spatial scales/FOV: 20 uas -- 200 uas 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 6 -- 220 GHz in Configuration D or E, phased-array 6.2. Lines and Frequencies 6.3. Spectral Resolution (km/s) 6.4. Bandwidth or spectral coverage: 1 GHz x 2pol (set by VLBI recorder) 7. Continuum flux density: 7.1. Typical value: 7.2. Continuum peak value: typically of order 1 Jy 7.3. Required continuum rms: ALMA - HHT baseline, 10 min rms = 0.7 mJy ALMA - LMT baseline, 10 min rms = 0.2 mJy 7.4. Dynamic range in image: 1e3 8. Line intensity: 8.1. Typical value: 8.2. Required rms per channel: 8.3. Spectral dynamic range: 9. Polarization: yes 10. Integration time per setting: 10 sources at 5 hrs per source 11. Total integration time for program: 50 hr *********************************************************************** Review Jean Turner: mm-VLBI can probe to 50 Rsch at M87, an important region for probing jet physics. Proposed sample is 10 sources, 50 hours, this is reasonable although getting 50 hrs to do VLBI is often tricky, but this is an obvious project & obvious sources (like M87). I have to take Chris's numbers on faith since they involve other telescopes and VLBI. -------------------------------------------------- Review v2.0: 1.6.4 mm VLBI observations of core-jets (Carilli) Not revised since DRSP 1.1. Nothing needs to be added to the review back then, no severe impact through reduction to 50 antennas, no need for ACA. ===================================================================================== DRSP 5.1.3 Title mm VLBI imaging of IDVs Pi C. Carilli Time 50 hrs 5.1.3: Name -- mm VLBI imaging of IDVs Authors: C. Carilli 2. Science goal: We propose VLBI imaging using the Pacific array (see 1.6.3) at 220 GHz of a representative sample of IDVs (Intra-Day Variability). These data will probe to scales of 20uas, and test models for coherent emission mechanisms to explain the very high brightness temperatures inferred from the ISS (Maquart et al. 2000 ApJ 528, 623), thereby constraining physical conditions in the jet, and perhaps study aspects of the accretion disk via the induced Compton scattering mechanism(?). 3. Number of sources: 5 4. Coordinates: 4.1. Any 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 20uas 5.2. Range of spatial scales/FOV: 20 uas -- 200 uas 5.3. Single dish: no 5.4. ACA: no 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 6 -- 220 GHz in Configuration D or E, phased-array 6.2. Lines and Frequencies 6.3. Spectral Resolution (km/s) 6.4. Bandwidth or spectral coverage: 1 GHz x 2pol (set by VLBI recorder) 7. Continuum flux density: 7.1. Typical value: 7.2. Continuum peak value: <= 2 Jy 7.3. Required continuum rms: ALMA - HHT baseline, 10 min rms = 0.7 mJy ALMA - LMT baseline, 10 min rms = 0.2 mJy 7.4. Dynamic range in image: 1e3 8. Line intensity: 8.1. Typical value: 8.2. Required rms per channel: 8.3. Spectral dynamic range: 9. Polarization: yes 10. Integration time per setting: 5 sources at 5 hrs per source 11. Total integration time for program: 50 hr note: this is not a monitoring project (at least initially), nor is it triggered since getting the source during an IDV event is not critical for the high frequency VLBI imaging. ****************************************************************** Review Jean Turner: Technical: I have to take Chris's numbers on faith since they involve other telescopes and VLBI. They seem very reasonable given the ALMA sensitivities. -------------------------------------------------- Review v2.0: 1.6.6. mm VLBI imaging of IDVs (Carilli) Not revised since DRSP 1.1. Nothing needs to be added to the review back then, no severe impact through reduction to 50 antennas, no need for ACA. I'm not an expert in this, but I think there is still a debate going on if this effect is source intrinsic or not. If not, the scientific interest in this topic may disappear or get much weaker. =====================================================================================