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.