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 value