Title Continuum survey from 80 to 900 GHz  
Pi    S.Guilloteau 
Time   260 hrs
  1. Title: Continuum survey from 80 to 900 GHz
  Authors: S.Guilloteau, A.Dutrey, M.Saito

  2.Science Goals:
  Determine the dust evolution and coagulation processes.
  To disentangle grain properties from the disk properties, it
  is needed to map disks at several submm/mm wavelengths with
  sufficient angular resolution (0.1"-0.2"). In particular, obtaining
  the evolution of the dust emissivity as function of radius is a key
  parameter to constrain the dust coagulation process. To do so,
  it is required to resolve the optically thick at least at 2
  frequencies, and
  to obtain sufficient brightness sensitivity at all frequencies up to some
  outer radius in order to derive the SED (and thus Beta) in a few radial
  bins.  Optically thick radius for dust is about 20 - 50 AU at 1 mm. To get
  a few radial bins, we should detect the dust at least up to 300 AU, and
  observe with a resolution 0.1" (15 AU at 150 pc). At this
  resolution, there
  are 120 beams at a radius of 300 AU (for a face on disk).

  Goals: dust characterization (abs.coefficient, spectral index)
  dust disk properties (outer radius, surface density, temperature)

  3.Number of sources: ~ 70

  4.Coordinates:
   4.1
      5 sources in Hyd      (RA= , DEC=-60)
     15 sources in Taurus   (RA=04, DEC=+25)
     20 sources in ChaI     (RA=11, DEC=-70)
     20 sources in Oph      (RA=16:30, DEC=-24)
     10 sources in ONC      (RA=05,  DEC=-05)
    4.2 Moving target: no
    4.3 Time critical: no

  5.  Spatial scales:
    5.1. Angular resolution: 0.1 arcsec
    5.2. Range of spatial scales/FOV: up to 5 arcsec
    5.3. Single dish: no
    5.4. ACA: no
    5.5. Subarrays: no

  6. Frequencies:
    6.1. Receiver band: Band 3, Band 6, Band 7, Band 10
    6.2. Lines: no or CO if done in parallel with  DRSP 2.4.1.

  7. Continuum flux density:
    7.1. Typical value: 50-200 mJy
    7.2. Continuum typical brightness at 300 AU
      A. 110 GHz   30 mK
      B. 230 GHz   60 mK
      C. 350 GHz   90 mK
      D. 670 GHz   180 mK
    7.3. Required continuum rms:
      Signal to noise of 10 on the brightness at 300 AU,
      where we have about 120 beams, so the required rms per beam is
      A. 110 GHz   33 mK
      B. 230 GHz   60 mK
      C. 350 GHz   0.1 K
      D. 670 GHz   0.2 K
    7.4. Dynamic range in image: high in general (> 1000)

  9. Polarization: Yes

  10. Integration time per setting:
      A. rms in 1 hr: 60 mK   3.30 hrs per source
      B. rms in 1 hr: 30 mK   0.25 hrs per source
      C. rms in 1 hr: 40 mK   0.16 hrs per source
      D. rms in 1 hr: 35 mK   0.03 hrs per source
  Total 3.7 hours per source

  11. Total integration time for program:  260hr
       70(src)x(3.7 hrs)= 260 hrs

*************************************************************************

Review Phil Myers: Good basic data program.  Good for disk structure,
may also be useful for dust evolution and coagulation.
--------------------------------------------------
Review v2.0:
 
  1. Title: Continuum survey from 80 to 900 GHz
  Authors: S.Guilloteau, A.Dutrey, M.Saito


Reviewer:  John Bally

Unclear why 70 sources need to be observed.  A well-chosen sub-set of
the nearest disks should be selected for this program.  Disk
orientation should also be specified.  Nearly face-on disks will
provide the clearest perspective, but also have the lowest optical
depths.  Nearly edge-on disks will tend to have higher optical depths,
but structure information will be sacrificed.