Title  The Connection Between Cloud Structure and the IMF
Pi     C. Chandler
Time   400 hrs
1. Name: The Connection Between Cloud Structure and the IMF
         =================================================
   Authors: C. Chandler, A. Wootten, J. Mangum 

2. Science goal: The origin of the IMF and its relationship to the 
   initial conditions within star forming molecular clouds is one of the
   major unsolved problems in star formation, and one which has  
   implications for almost every scientific field in which ALMA will be 
   important.  We propose to conduct a large-scale survey of the  
   Ophiuchus, Lupus, Perseus, and Orion molecular cloud complexes in  
   order to determine this relationship.  The main survey will be carried 
   out at 1 mm, and companion survey at 3 mm is needed to enable us to 
   distinguish unambiguously between dust and free-free emission.

3. Number of sources: 4 

4. Coordinates: 
4.1. Ophiuchus (RA=16:30, DEC=-24); Perseus (RA=03, DEC=+30);
     Lupus (RA=16, DEC=-35); Orion (RA=05:30, DEC=-05) 
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: 1 degree 
5.3. Single dish: yes 
5.4. ACA: yes 
5.5. Subarrays: no

6. Frequencies: 
6.1. Receiver band: Band 6 230 GHz Band 3 100 GHz
6.2. Line:   
6.3. Spectral resolution (km/s):  
6.4. Spectral coverage (km/s or GHz): 

7. Continuum flux density: 
7.1. Typical value: 1 mJy
7.2. Continuum peak value: 1 Jy 
7.3. Required continuum rms: 0.3 mJy 
7.4. Dynamic range in image: 1000

8. Line intensity:
8.1. Typical value: 
8.2. Required rms per channel:  
8.3. Spectral dynamic range: 20 

9. Polarization: no 
10. Integration time per setting: 4 x 6 s x 57600 fields at 300 GHz
                                  4 x 1 s x 14400 fields at 100 GHz
                                  (NOTE: use OTF mosaicing)
11. Total integration time for program:  400 hr

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

Review John Richer: see program 2.1.1.
--------------------------------------------------
Review v2.0:
 
init_6 = 2.1.6

1. Name: The Connection Between Cloud Structure and the IMF
         =================================================
   Authors: C. Chandler, A. Wootten, J. Mangum 

Unchanged w.r.t. DRSP 1.1. This is a very large program. How does it
compare in terms of sensitivity to what is being done with Spitzer and
what is being planned with SCUBA2 on JMCT? Angular resolution will be
much higher with ALMA, but do you need to do the _entire_ clouds, or
just a number of representative regions to "translate" number counts
and mass distributions from one scale to another?