Astronomy and Astrophysics – Astronomy
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21420403g&link_type=abstract
American Astronomical Society, AAS Meeting #214, #204.03; Bulletin of the American Astronomical Society, Vol. 41, p.712
Astronomy and Astrophysics
Astronomy
Scientific paper
Spectral line surveys are a fundamental technique to gain information about an astronomical source. For interstellar molecular clouds that are at temperatures between 10 K and a few hundred K, the bulk of the emission is at relatively low frequencies, corresponding to centimeter to submillimeter wavelengths. The enormous variety of over 140 known astronomical molecules emit a complex set of spectral lines which reflect the chemical composition, the physical conditions (temperature, density), the velocity field, and the variation of all these parameters throughout the source. Collecting the basic data from a spectral line survey is enhanced by several key technical factors, including (1) low noise temperature; (2) broad instantaneous and bandwidth; (3) ability to carry out spectral analysis over as large a possible frequency range with required velocity resolution appropriate for the source being observed. In this talk I will review some of the spectral surveys of molecular and circumstellar clouds that have been undertaken, focusing on those which have been carried out recently. I will discuss the techniques used for analyzing the surveys to obtain information about key parameters of the source. I will also describe some of the surveys anticipated to be carried out with new ground-based facilities as well as the Herschel Space Observatory. I will briefly describe some of the challenges associated with interpreting these potentially powerful data sets.
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