Title  Mapping the surfaces of the Moon, Mercury and Mars
Pi     B. Butler
Time   66 hrs

Title: Mapping the surfaces of the Moon, Mercury and Mars
Authors: B. Butler

Abstract: ALMA will be able to map with unprecedented accuracy
   and fidelity the millimeter wavelength emission from the solid
   surfaces of the terrestrial planets (with the exception of 
   Venus).  Such maps will provide us with information on the 
   thermal and electrical properties of the surface and near-surface,
   as well as the surface texture - see e.g. Rudy et al. 1987;
   Mitchell & de Pater 1994.  For Mercury, the question of the
   presence of a molten liquid core may be answered if the accuracy
   is good enough.  In addition, the temperature can be determined
   in the polar cold traps, which might be locations of water ice 
   stability (this will require high resolution).  For Mars, results 
   will be compared to those returned from spacecraft in orbit at 
   the time.  This might also be true for the Moon.  Maps should be 
   made at all wavelengths, many of which will have to be mosaics 
   because of the large size of the bodies (notably the Moon).

                                                                             contin        line        poln
name      RA&DEC    m T SD CA sub resn size freq   line   dfreq      BW    fd     rms    fd    rms   fd    rms  time
------- ----------- - - -- -- --- ---- ---- ----  ------ --------  -----  ------------  -----------  ---------  ----
Moon     ecliptic   Y Y Y  Y   N   2   1800   90    N/A    N/A     8 GHz  200 K   2 K      N/A       5 K  .1 K  6 h
Moon     ecliptic   Y Y Y  Y   N   2   1800  230    N/A    N/A     8 GHz  200 K   2 K      N/A       5 K  .1 K  6 h
Mars     ecliptic   Y Y Y  Y   N   .1   10    90    N/A    N/A     8 GHz  200 K   2 K      N/A       5 K  .1 K  6 h
Mars     ecliptic   Y Y Y  Y   N   .1   10   230    N/A    N/A     8 GHz  200 K   2 K      N/A       5 K  .1 K  6 h
Mars     ecliptic   Y Y Y  Y   N   .1   10   345    N/A    N/A     8 GHz  200 K   2 K      N/A       5 K  .1 K  6 h
Mars     ecliptic   Y Y Y  Y   N   .1   10   650    N/A    N/A     8 GHz  200 K   2 K      N/A       5 K  .1 K  6 h
Mercury  ecliptic   Y Y Y  Y   N   .1   10    90    N/A    N/A     8 GHz  450 K   2 K      N/A       10 K .1 K  6 h
Mercury  ecliptic   Y Y Y  Y   N   .1   10   230    N/A    N/A     8 GHz  450 K   2 K      N/A       10 K .1 K  6 h
Mercury  ecliptic   Y Y Y  Y   N   .1   10   345    N/A    N/A     8 GHz  450 K   2 K      N/A       10 K .1 K  6 h
Mercury  ecliptic   Y Y Y  Y   N   .1   10   650    N/A    N/A     8 GHz  450 K   2 K      N/A       10 K .1 K  6 h
Mercury  ecliptic   Y Y Y  Y   N   .05  10   345    N/A    N/A     8 GHz  450 K   2 K      N/A       10 K .1 K  6 h
total                                                                                                           66 h

Notes: The mosaics of the Moon will contain some million or
   so pointings and must be done in OTF interferometer mode.
   The noise in 10 msec is plenty good enough though, even to
   get the 0.1 K in polarized brightness.  Mercury should be
   observed at conjunction, which occurs frequently enough
   that it shouldn't be a problem.

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See program 4.1.1 for general comments Butler and Gurwell

Review Mark Gurwell: OK.
--------------------------------------------------
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.