Warm molecular gas in the nucleus of IC 342 - The CO (J = 3-2) distribution

Details Warm molecular gas in the nucleus of IC 342 - The CO (J = 3-2) distribution Warm molecular gas in the nucleus of IC 342 - The CO (J = 3-2) distribution

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...388..328i&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 388, April 1, 1992, p. 328-337. Research supported by NSERC.

Astronomy and Astrophysics

Astrophysics

17

Carbon Monoxide, Galactic Nuclei, Gas Temperature, Interstellar Extinction, Milky Way Galaxy, Molecular Gases, Gas Density, H Ii Regions, Velocity Distribution

Scientific paper

The nuclear molecular bar of the nearby face-on galaxy, IC 342, in the (C-12)O(J = 3-2) was extensively mapped. The emission is centrally peaked with a weaker maximum to the north, and there is evidence for both circular and noncircular motions in this region. A comparison of the CO(J = 3-2)/CO(J = 2-1) and CO(J = 2-1)/CO(J = 1-0) line ratios from both the JCMT and IRAM telescopes, together with a large velocity gradient model, shows that the emission is generally due to warm gas of mean density, 2000/cu cm, and moderate optical thickness. CO abundances are lower than in Galactic dark clouds, especially in the central, active, star-forming regions, possibly due to UV photodissociation. A north-south ridge of higher excitation is observed to the east of the nucleus and may be associated with shocks. A total H2 mass of 10 exp 7 - 10 exp 8 solar masses in the bar is estimated; the molecular mass is likely a substantial fraction of the dynamical mass within the 170 pc.

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