Dense molecular gas in galaxies - HCN, HCO(+), and CS in M 82 and NGC 253

Details Dense molecular gas in galaxies - HCN, HCO(+), and CS in M 82 and NGC 253 Dense molecular gas in galaxies - HCN, HCO(+), and CS in M 82 and NGC 253

Aug 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...220...57n&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 220, no. 1-2, Aug. 1989, p. 57-64. Research supported by the University of Tok

Astronomy and Astrophysics

Astrophysics

53

Andromeda Galaxy, Interstellar Gas, Molecular Gases, Brightness Temperature, Formyl Ions, Hydrocyanic Acid, Molecular Spectra, Radio Spectra

Scientific paper

The HCN (J = 1 to 0), HCO(+) (J = 1 to 0), and CS (J = 2 to 1) lines have been observed in five positions along the major axis toward the nuclei of M 82 and NGC 253. The present line strengths suggest that a large fraction of the molecular gas in M 82 and NGC 253 resides in small dense clumps with a low volume filling factor. The results are consistent with quiescent Milky Way molecular clouds. It is found that the HCO(+)/HCN abundance ratio in M 82 is enhanced with respect to that in NGC 253, and that the distribution of HCN and HCO(+) is depressed or flat toward the center or M 82 and appears centrally peaked in NGC 253. The HCN spectra toward the central position of M82 are shown to exhibit an absorption feature at 230 km/s which probably arises from the cold and dense gas in the disk of the galaxy.

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