Start with the extensive list prepared by the Japanese and sent by
Hasegawa-san to ASAC a few weeks. Input from other ASAC members was on
protostellar envelopes, debris disks and nearby galaxies.

Select 3-4 examples to highlight:

Example 1: Extended protostellar envelopes --- How accurate can ALMA images
reproduce its radial profile? Can we distinguish between collapse model X and
Y (e.g. Shu-type collapse vs. other collapse model)?

Example 2: Multiple dense cores in a GMC at a distance of LMC --- How
accurate can an ALMA image reproduce the extended diffuse component and the
mass function of the cores embedded therein?

Example 3: Face-on disk galaxies at small to intermediate distances --- How
accurate can ALMA images reproduce the extended disk component and the
brightness of the arms and the interarm regions?

Example 4: Debris disk, e.g. Epsilon Eridani-type objects: How well
can ALMA image the structure in such disks?
 

The main question is how to translate these science examples into test models
for the ACA. There are several useful examples in the literature such as the
HL Tau environment (Welch et al. 2000, ApJ 540, 363) and the
BIMA-SONG/OVRO/Nobeyama data on nearby galaxies, but those probably have to be
translated into examples with higher dynamic range. Several people (Lee Mundy,
Michiel Hogerheijde, ...) have offered to help. ASAC suggestions
are welcome.