Sub-mm Results in 98/99 at the Sub Millimeter Telescope Observatory

Details Sub-mm Results in 98/99 at the Sub Millimeter Telescope Observatory Sub-mm Results in 98/99 at the Sub Millimeter Telescope Observatory

Oct 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999alma.confe..74w&link_type=abstract

Science with the Atacama Large Millimeter Array (ALMA), Associated Universities, Inc., held October 6-8, 1999 at Carnegie Instit

Other

Modelling, Molecular Clouds, Star Formation, Smto, Hht, Telescope, Foci, Receivers

Scientific paper

Radio astronomers have studied only small regions of the sky in the necessary detail, with accurate pointing, calibration and high signal-to-noise ratio needed for the accurate modelling of molecular clouds. For ALMA, such studies with single telescopes are needed before high resolution imaging can be undertaken. In addition, cloud imaging in the sub-mm wavelength range allows us to select warm regions with high H2 densities. Such regions are more likely to collapse to form stars or contain newly-formed stars. We have used the Heinrich Hertz 10-m telescope (HHT) to take these data. The HHT is located on Mt. Graham at an elevation of 3.2 km. The RMS pointing error is 2.5'', the beam size at 806 GHz is 13", and the telescope beam efficiency at 806 GHz is ~38%. We expect to improve these telescope parameters in the coming year. The receivers at the HHT are located in two naysmth foci to the left and right of the telescope axis. The left focus contains the facility SIS heterodyne receivers, while the right side is reserved for bolometers and P.I. instruments. Changing foci is accomplished in less than a minute by flipping a flat mirror under remote control. This flexibility makes the HHT an ideal 'test bed' for new, experimental receiver systems. All of the results in this report were taken with heterodyne receivers. The spectra were analyzed using either filter banks or Acoustic Optical Spectrometers. The results were taken with either position switching or beam switching with a beam throw of 4'. The efficiency of data taking and reliability of the results were improved using the spectral line On-The-Fly (OTF) mapping technique. After its implementation in December 1998, OTF mapping was used for several projects at frequencies up to 806 GHz (CO 7-6) using the CfA Hot Electron Bolometer Receiver. We show maps of the ongoing scientific programs dealing with star formation, outflow dynamics, the interaction of HII regions with molecular clouds and the chemistry, ionization and structure of the interstellar medium. Our images of galactic sources include CO J=7-6 data for Orion KL, Cepheus B and Sharpless 106. Maps of extragalacitc sources such as M82, IC 342 and Maffei 2 were taken by other groups and will be presented in another forum.

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