Cold Chemistry In TMC-CP: Temperature Deduced From HC9N Line Intensities

Details Cold Chemistry In TMC-CP: Temperature Deduced From HC9N Line Intensities Cold Chemistry In TMC-CP: Temperature Deduced From HC9N Line Intensities

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21348516m&link_type=abstract

American Astronomical Society, AAS Meeting #213, #485.16; Bulletin of the American Astronomical Society, Vol. 41, p.458

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We present a model for the temperature of the Taurus Molecular Cloud (TMC) Cyanopolyene Peak (CP). This model is based on a fit to molecular line observations with the Robert C. Byrd Green Bank Telescope. We find this region to be very cold, with temperature of approximately 3 Kelvin.
The TMC-CP region is of great interest because of its known high abundance of large organic molecules. Large molecular structures have been observed within TMC-1 by various authors (Pratrap et al 1997, Dickens et al 2001, and Turner et al 2005). The detection of large molecules, such as HC5N, HC7N, and HC9N, suggests that smaller amino acids could also form in the interstellar medium. Amino acids are essential to life found on earth, and it is highly possible that early biological molecules had their origins within the molecular clouds of the interstellar medium.
We observed a sequence of HC9N and HC7N line transitions, in the frequency range 11 to 15 GHz, to estimate the temperature of the molecular line emission region. We present radio images of the structure of TMC from our search for the molecules HC11N and HC13N. Finally, we present upper limits on the abundance of selected molecules, based on averaging observations of many spectral lines in the manner described by Langston and Turner (2007).
The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.

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