Title  Sizes and albedoes of NEAs
Pi     B. Butler
Time   20 hrs

Title: Sizes and albedoes of NEAs
Authors: B. Butler

Abstract: Thermal emission observations of NEAs, when combined
   with optical/NIR observations, will provide accurate measures 
   of their sizes and albedoes.  This is very similar to the
   situation with MBAs, where early sizes and albedoes determined
   from optical observations were found to be seriously in error
   in many instances when confronted with the more accurate 
   determination from observations of the emission (the crossover
   wavelength for emission vs. reflection is of order 10 microns).
   There are generally ~10 NEA opportunities per year.

                                                                          contin         line        poln
name   RA&DEC   m T SD CA sub resn size  freq   line   dfreq      BW    fd       rms    fd    rms   fd    rms   time
----  --------  - - -- -- --- ---- ----- ----  ------ --------  -----  --------------  -----------  ---------  ------
NEA   ecliptic  Y Y N  N   N   any small  345    N/A    N/A     8 GHz  ~200 K    1 K       N/A      3 K  .1 K  30x1 h
total                                                                                                          20 h

Note: These will be mostly TOO observations, occurring at
   truly unpredictable times.

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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.