Detection of CO emission from massive molecular clouds in the inner disk of M31

Details Detection of CO emission from massive molecular clouds in the inner disk of M31 Detection of CO emission from massive molecular clouds in the inner disk of M31

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...410l..15a&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 410, no. 1, p. L15-L18.

Astronomy and Astrophysics

Astrophysics

50

Andromeda Galaxy, Carbon Monoxide, Emission Spectra, H Ii Regions, Molecular Clouds, Interstellar Gas, Interstellar Matter, Line Spectra, Relic Radiation

Scientific paper

Faint emission in the CO(1-0) and CO(2-1) spectral lines at mm wavelengths has been discovered from dark dust clouds in the inner disk of M31. These dust clouds are located in regions of the galaxy where there is little evidence of star-forming activity. The CO emission from these clouds is resolved, and comes from roughly the same area covered by the dust clouds. The line profile widths and cloud sizes imply cloud masses typical for giant molecular clouds (GMCs) in the Galaxy, but the observed surface brightnesses are only a few tenths of a K, and the typical CO(1-0) luminosities are a factor of about 10 smaller than those of Galactic GMCs of the same size and velocity line width. The CO(2-1)/CO(1-0) line ratios are very low, suggesting subthermal excitation, and precluding use of this ratio alone to determine the kinetic temperature. However, there are indications that the kinetic temperatures are significantly lower than the values of 10-30 K typical for Galactic GMCs, and may be close to the 2.7 K cosmic background.

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