CO 7-6 submillimeter emission from the galactic center - Warm molecular gas and the rotation curve in the central 10 parsecs

Details CO 7-6 submillimeter emission from the galactic center - Warm molecular gas and the rotation curve in the central 10 parsecs CO 7-6 submillimeter emission from the galactic center - Warm molecular gas and the rotation curve in the central 10 parsecs

Jul 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...294l..93h&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 294, July 15, 1985, p. L93-L97. Research supported

Other

65

Carbon Monoxide, Galactic Nuclei, Interstellar Gas, Molecular Gases, Angular Velocity, Gas Heating, Luminosity, Mass Distribution, Submillimeter Waves

Scientific paper

Bright CO J = 7-6 submillimeter line emission in the central 10 pc of the Galaxy has been mapped. This is the first detection of the 7-6 line from the Galactic center; it was made with a new submillimeter heterodyne spectrometer mounted on the 3.0-m NASA IRTF telescope at Mauna Kea, Hawaii. The 372-micrometer CO emission comes from a dense, clumpy disk (10,000 solar masses) of temperature about 300 K. The luminosity of all CO rotational lines emitted from this approximately 4-arcmin diameter region is about 20,000 solar luminosities. CO line emission is a major contribution to the cooling of the interstellar gas near Sgr A. The CO data show that the rotational velocities drop by a factor of 1.4 to 2 between 2 and 6 pc from the center. The rotation curve is consistent with a 'Keplerian' fall off around a point mass and implies that most of the mass is in a more compact distribution than an isothermal stellar cluster. Broad line width emission toward the central 30 arcsec of the Galaxy indicates that there is a significant amount of molecular material in the inner, mostly ionized, cavity.

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