Sub-Millimeter Astronomy and Astrophysics

Abstract

As of 1984, the submm band (ν >300 GHz) is relatively unexplored. The word “relatively” should be stressed since, evidently, a great deal of work has been done. However, much of this is of the “discovery” or “first detection” category with emphasis on the priority of a given result, and less thought as to astrophysical consequences. It therefore seems to be a useful exercise to examine what astrophysics one should expect from submm measurements. A great deal of these measurements will be the extension of work going on at longer wavelengths, and we will base much of our discussion on our own recent research and comment on its consequences for observations at frequencies above 300 GHz. (Summaries of frequency scans in the 200–260 GHz region are Erickson et al. 1980 and G. Blake, this volume.) We will emphasize the way in which observations in the various wavelength bands complement one another, and outline the connections by means of a few examples. Finally, we will present a short description of the 10-m submm dish to be built by the MPIfR and to be operated by the University of Arizona and the MPIfR on Mt. Graham, near Tucson, Arizona.