Detailed Structure of Giant Molecular Cloud Peripheries

Details Detailed Structure of Giant Molecular Cloud Peripheries Detailed Structure of Giant Molecular Cloud Peripheries

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998stin...9984012s&link_type=abstract

Nobeyama Radio Observatory Report, p. 5

Other

Surveys, Molecular Clouds, Gas Density, Interstellar Gas, Spatial Resolution, Image Resolution, Boundaries, Brightness, Clumps, Estimating, Excitation, High Resolution, Low Temperature, Luminosity, Molecular Gases, Monatomic Gases, Populations, Substructures

Scientific paper

We present the first extensive and high-resolution images of a giant molecular cloud periphery. We detected CO emission almost everywhere within the outermost boundary of L1641. There exist two distinct populations of molecular gas: "clumps" and "extended component." The clumps dominate the CO luminosity from the central ridge region where they are severely overlapped, while they are isolated in the periphery of the cloud. The extended component is widely distributed, especially in the eastern side of the cloud, and seems to be connected to the atomic gas layer in the Galactic plane, It lacks notable substructures at our spatial resolution and exhibits a surface filling factor very close to unity. Molecular gas density estimated from excitation analysis of C-12O J = 2 - 1 and J = 1 - 0 emissions is approx. greater than 3 x 103/cc in the clumps and approx. 2 x 102/cc in the extended component. The peripheral region of the cloud is fainter in CO brightness not because the surface filling factor of emitting gas is smaller, but because the emission is dominated by the tenuous extended component with low brightness temperature. Our follow-up large-scale C-12O J = 2 - 1 survey of nearby clouds confirms the existence of extended low-density envelopes in other molecular clouds.

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