^12CO (J=1--0) and ^13CO (J=1--0) Mapping of the Starburst Galaxy M82

Details ^12CO (J=1--0) and ^13CO (J=1--0) Mapping of the Starburst Galaxy M82 ^12CO (J=1--0) and ^13CO (J=1--0) Mapping of the Starburst Galaxy M82

Jun 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998pasj...50..309k&link_type=abstract

Publications of the Astronomical Society of Japan, v.50, p.309-315.

Astronomy and Astrophysics

Astronomy

8

Galaxies: Active, Galaxies: Evolution, Galaxies: Individual (M82), Stars: Formation

Scientific paper

We have mapped the central 1 kpc region of the nearby starburst galaxy M82 in both the (12) CO (J=1--0) and (13) CO (J=1--0) emission lines under the same angular resolution ( ~ 7('') times 6('') ). The intensity ratio (R) of (12) CO (J=1--0) to (13) CO (J=1--0) emission shows the significant spatial variation: R =~ 35--40 (the NE lobe), R =~ 20--25 (the SW lobe), and R >70 (the 2.2 mu m secondary peak). These values are significantly higher than those of giant molecular clouds in our Galaxy and molecular gas in other normal spiral galaxies. We also find that a very high ratio (R > 90) is achieved around the brightest radio continuum source, 41.9+58, which is considered to be a supernova remnant (or remnants). Based on the LTE model, we show that the molecular gas in M82 tends to be optically thin, even for the (12) CO emission; its optical depth is a few or less. The smaller optical depths may naturally explain the higher R values observed in M82. We discuss the possibility that a superwind causes the formation of such clouds.

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