1. Searching for Proto- Super Star Clusters in the Antennae
C. Wilson

   2. One short paragraph with science goal(s)

The goal is to identify young massive star clusters that are still 
deeply embedded in molecular gas or proto-clusters i.e. dense compact
cores that are massive enough to form a young massive star clusters. We
need sensitivity sufficient to detect an object with 10^5 Msun of gas
and dust confined to a region of space roughly 1 pc across. In the
Antennae at 20 Mpc, this translates to 0.01" resolution and a detectable
dust flux of 60 micro Jy.

   3. Number of sources: 1 source, four fields

   4. Coordinates:

      4.1. Rough RA and DEC:  12 hour -15 degrees

      4.2. Moving target: no

      4.3. Time critical: no

   5. Spatial scales:

      5.1. Angular resolution (arcsec): 0.012

      5.2. Range of spatial scales/FOV (arcsec): 15" x several fields

      5.3. Single dish total power data: no

      5.4. ACA: no

      5.5. Subarrays: no


   6. Frequencies:

      6.1. Receiver band: Band 7

      6.2. Lines and Frequencies (GHz): 350 GHz

   7. Continuum flux density:

      7.1. Typical value (Jy): 60-600 micro Jy
           (take average value of set of objects)
           (optional: indicate range of fluxes within set of objects)

      7.2. Required continuum rms (Jy or K): 12 micro Jy

      7.3. Dynamic range within image: 50; objects may be clustered with
		several within a few arcseconds.

   9. Polarization:  no 

   10. Integration time for each observing mode/receiver setting (hr):
		5 hours per field; assume 4 fields to cover all 
		gas-rich regions

   11. Total integration time for program (hr): 20 hours

   12. Comments on observing strategy (e.g. line surveys, Target of
       Opportunity, Sun, ...): (optional)

The limiting factor in this experiment is the angular resolution,
which pushes the limit of what ALMA can do.


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Review Chris Carilli: OK.