Title  Millimeter survey of stellar disk emission from late-type giants and supergiants
Pi     R. A. Osten
Time   3.5 hrs


   1. Name of program and authors
"Millimeter survey of stellar disk emission from late-type 
giants and supergiants"
R. A. Osten 

   2. One short paragraph with science goal(s)

The VLA resolved the supergiant Betelgeuse (Alpha Ori) at 7mm, providing
crucial measurements for refining atmospheric models and investigating
mass loss mechanisms in late-type stars.  
Sensitive measurements of the mm fluxes from such
stars, combined with superb spatial resolution, will reveal intensity
asymmetries and make vast improvements in the current spherically
symmetric atmospheric models.  This project is a survey of M supergiants 
and K giants, which show predominantly wind emission.  Each object will
be observed twice, separated by at least one month, to check for 
any mm variability (several objects
show evidence of variability at cm wavelengths).  This will provide
some constraints on stellar pulsations and dust shell emission.



   3. Number of sources (e.g., 1 deep field of 4'x4', 50 YSO's,
                              300 T Tauri stars with disks, ...; do NOT
                              list individual sources or your "pet object",
                              except in special cases like LMC, Cen A, HDFS)
  20
   4. Coordinates:
      4.1. Rough RA and DEC (e.g., 30 sources in Taurus, 30 in Oph, 20 in Cha, 
                             30 in Lupus)
    
  scattered in RA and DEC
      4.2. Moving target: yes/no  (e.g. comet, planet, ...)
    no
      4.3. Time critical: yes/no  (e.g. SN, GRB, ...)
    no
   5. Spatial scales:
      5.1. Angular resolution (arcsec):

      5.2. Range of spatial scales/FOV (arcsec):           
           (optional: indicate whether single-field, small mosaic, 
            wide-field mosaic...)

      5.3. Single dish total power data: no

      5.4. ACA: no

      5.5. Subarrays: no


   6. Frequencies:

      6.1. Receiver band: Band 3, 6, 7, or 9
 band 3 and 6
      6.2. Lines and Frequencies (GHz):

      6.3. Spectral resolution (km/s):

      6.4. Bandwidth or spectral coverage (km/s or GHz):
few GHz at each end of the band

   7. Continuum flux density:

      7.1. Typical value (Jy):
       tens of mJy     
      7.2. Required continuum rms (Jy or K):
       20 micro Jy
      7.3. Dynamic range within image:                  
           (from 7.1 and 7.2, but also indicate whether e.g. weak objects 
            next to bright objects)
       >10 

   8. Line intensity:

      8.1. Typical value (K or Jy):
           (take average value of set of objects)
           (optional: provide range of values for set of objects)

      8.2. Required rms per channel (K or Jy):

      8.3. Spectral dynamic range:              


   9. Polarization:  yes/no  (optional)
          no 

      9.1. Required Stokes
      9.2. Total polarized flux density (Jy)
      9.3. Required polarization rms and/or dynamic range
      9.4. Polarization fidelity


   10. Integration time for each observing mode/receiver setting (hr):
     5 minutes per target will give 1 sigma sensitivities of 20 microJy
   11. Total integration time for program (hr):
     20 targets, each observed twice for 5 minutes: 3.5 hours (plus calibration)
   12. Comments on observing strategy (e.g. line surveys, Target of
       Opportunity, Sun, ...): (optional)


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

Review Leonardo Testi: merge with 3.2.3

Comment Ewine: keep as separate for the moment; representative small
program
--------------------------------------------------
Review v2.0:
 
   1. Name of program and authors
"Millimeter survey of stellar disk emission from late-type 
giants and supergiants"
R. A. Osten 

DRSP2.0 Review Leonardo Testi: