ALMA Science Workshop May 14, 2004. Arizona Radio Observatory. Present and Future. Thomas W. Folkers. ARO’s Observing Philosophy. On site support personnel. ( Operators ) Emphasize remote observing. Service observing. Staff Astronomers for observer support.
Present and Future
Thomas W. Folkers
600 – 800 GHz with PI Inst.
* Versus old VAX/CAMAC based System
12CO(2-1) map of the Gem OB1 region obtained using OTF mapping at the HHSMT. The image shows the line integrated intensity, in antenna temperature units, smoothed to the beam size of the telescope at this frequency (i.e., 32"). The contours range from 10 to 140 K km/s in steps of 5 K km/s. The antenna beam is shown in the small box in the upper right-hand corner. Approximately 87,000 spectra have gone into this 0.75 º x 1 º map. An RMS of 0.25 K per binned point was reached for the whole map in 22 hours of observation with a single pixel receiver.
NOTE: Before smoothing, the original number of individual spectra contained in this map is 6 times as many. (522,000)
Bolometer sensitivity: For weather ~ 2mm PWV, 400”x300” map with default pars 150 mJy rms in 35 mins ON-OFF Sequence 600mJy/√secs
225 GHz Tipper Opacity. PWV(mm) = tau225 * 19
IF Processor Card
CS J=8->7 391 GHz
Highest Transition of CS giving over 50 % atmospheric transmission.New Atmospheric Window385-420 GHz