Title Radar observations of NEAs Pi B. Butler Time 12 hrs Title: Radar observations of NEAs Authors: B. Butler Abstract: Radar observations are a powerful way to measure surface and near-surface properties of solid bodies. In addition, orbit and spin state are accurately measured this way - see, e.g., de Pater et al. 1994. 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 .05 small 90 radar ~1 Hz 10 kHz N/A 1000 Jy 10 mJy 100 Jy 10 mJy 4x3 h total 12 h Note: These will be purely TOO observations, occurring at unpredictable times. This presumes the existence of a radar transmitting 100 kW through a 50-m aperture at 90 GHz, and that the NEA comes by at the right time (when the array is in spread out configuration). ********************************************************************* See program 4.1.1 for general comments Butler and Gurwell Review Mark Gurwell: Really cool...we should try to keep the radar reception BW needed as a correlator specification! Reply Butler: I need to track this down -------------------------------------------------- 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.