The molecular gas toward Cassiopeia A

Details The molecular gas toward Cassiopeia A The molecular gas toward Cassiopeia A

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...280..221w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 280, no. 1, p. 221-230

Astronomy and Astrophysics

Astrophysics

17

Absorption Spectra, Carbon Monoxide, Cassiopeia A, Emission Spectra, Interstellar Matter, Line Spectra, Molecular Clouds, Molecular Gases, Abundance, Ammonia, Hydrogen, Hydroxides, Interstellar Magnetic Fields, Molecules

Scientific paper

Fully sampled 20 sec resolution maps of Cassiopeia A in the J = 1 - 0 line of (13)CO, and additional observations of the J = 1 - 0 and J = 2 - 1 lines of (12)CO and (13)CO are presented. From the peak (12)CO line intensity, the kinetic temperature of the molecular gas reaches 20K. The warmest clouds are in the SE part of the region mapped. From the (13)CO data, there are at least eleven molecular clouds. Ten clouds are in the Perseus spiral arm, approximately 3 kpc from the sun; one is in the solar neighborhood. For the Perseus arm clouds, a Large Velocity Gradient analysis of J = 2 - 1 and J = 1 - 0 lines of (13)CO gives H2 densities less than or equal to 4000/cu cm. For these clouds, masses from CO data are significantly smaller than obtained from the virial theorem if only gravity is important; the clouds toward the SE of Cas A are closest to being bound. A comparison with OH, H2CO and NH3 absorption line maps shows a reasonable agreement of the positions of maxima; most interestingly a few OH clouds have only weak CO conterparts. From these data, relative abundances are obtained. The atomic and CO content of the Perseus and Orion arm clouds is compared.

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