Title Albedos, sizes and surface properties of transneptunian objects Pi E. Lellouch Time 140 hrs Title: Albedos, sizes and surface properties of transneptunian objects Authors: E. Lellouch Abstract: The distribution of size in the Kuiper Belt is an indicator of formation and collisional evolution processes. Knowledge of the albedo of the objects is needed to correctly interpret their spectra, and to search for possible correlations in the albedo-size-color space that would trace their dynamical and collisional history. This can be obtained by measuring the continuum thermal flux of these objects. For the largest of these objects, mm lightcurves (i.e. the variation of the thermal flux with the object rotational phase) can be obtained, providing additional information on the object surface properties, particularly the thermal inertia. contin line poln name RA&DEC m T SD CA sub resn size freq line dfreq BW fd rms fd rms fd rms time ------- ----------- - - -- -- --- ---- ---- ---- ---------- -------- ------- ------------ ----------- --------- ------- many ~ecliptic Y Y N N N .05 ~.05 345 N/A N/A 16 GHz 1 mJy .1 K N/A N/A 140x1 h total 140 h Notes: The resolution here is not what is required during observation, but rather the size of the body, which is what is needed for the brightness temp rms calculation. These are point source detections - i.e., we don't *want* the body resolved (any resolution *worse* than this is OK). Each detection (to .1 K rms) takes about an hour. There might be 100 or so bodies, then some monitoring for the larger ones. **************************************************************************** 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.