Title  Structure and composition of Saturn's rings
Pi     B. Butler
Time   48 hrs

Title: Structure and composition of Saturn's rings
Authors: B. Butler

Abstract: Observations at millimeter wavelengths will constrain
   the size distribution and properties of the rings of Saturn - see,
   e.g., Grossman et al. 1989; van der Tak et al. 1999.  In addition, 
   structures (density waves, e.g.) will be observed, allowing for
   constraints on their formation mechanism.

                                                                           contin         line        poln
name    RA&DEC   m T SD CA sub resn size freq   line   dfreq      BW    fd        rms   fd    rms   fd    rms  time
------ --------  - - -- -- --- ---- ---- ----  ------ --------  -----  --------------  -----------  ---------  -----
Saturn ecliptic  Y Y Y  Y   N   .1   15    90    N/A    N/A     8 GHz  10-100 K .5 K       N/A      1 K  .1 K  4x4 h
Saturn ecliptic  Y Y Y  Y   N   .1   15   345    N/A    N/A     8 GHz  10-100 K .5 K       N/A      1 K  .1 K  4x4 h
Saturn ecliptic  Y Y Y  Y   N   .1   15   650    N/A    N/A     8 GHz  10-100 K .5 K       N/A      1 K  .1 K  4x4 h
total                                                                                                          48 h


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See program 4.1.1 for general comments Butler and Gurwell

Review Mark Gurwell: 
       I am not sure if "size" of 15" is right for the Saturn ring
       DRSP...Saturn's rings generally extend much more than this...
       but otherwise ok

Reply Butler:
I just put in the size of Saturn, and the rings about
double the size.  I don't think it matters too much for the 
purposes of the DRSP, but you are right to point it out and i've
corrected it.  of course it depends on where it is in its orbit
too.

Comment Ewine: updated DRSP is now baseline



--------------------------------------------------
Review v2.0:
 
Review of 4.2.1-4.2.8 (no DRSP 2.0 updates received)

These projects still remain scientifically valid. Do the additional
ALMA bands offer something new (e.g., for projects 4.2.4, 4.2.5)? The
integration times are probably still ok eventhough the number of
antennas has gone from 64 to 50 - or at least close enough.

Several of these projects focus on objects larger than the ALMA
primary beam, and mosaicing is needed. Here the ACA and also the ACA
in crosscorrelation with the ALMA-12m antennas may be beneficial.