Molecular Clouds in the Galactic Nucleus
- Creators
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Scoville, N. Z.
- Solomon, P. M.
- Jefferts, K. B.
Abstract
Observations of the 2.6-mm CO line have been obtained along the galactic equator covering longitudes |ℓ| ≤ 3° and velocities |V| ≤ 300 km s^(-1). The strongest emission is concentrated toward the center (|ℓ| < 1°.5) and at low velocities (<125 km s^-1)) The similarities in distribution and brightness temperature between the CO and 100-µ emissions suggest that the grains and the gas are colocated and nearly in thermal equilibrium. Kinematic models for the gas in the nucleus are briefly discussed. The mass of this gas (mostly H_2) is estimated as 10^7 - 10^8 M_⊙ within 600 pc of the center. This large mass of interstellar molecules indicates that the galactic nucleus may not be deficient in Population I material.
Additional Information
© 1974. The American Astronomical Society. Received 1973 October 9; revised 1973 November 12. The Millimeter-Wave Observatory is operated by the Electrical Engineering Research Laboratory, The University of Texas at Austin, with support from the National Aeronautics and Space Administration, The National Science Foundation, and McDonald Observatory. This research was supported in part by the University of Minnesota Graduate School and by NSF grant GP-27983.Attached Files
Published - 1974ApJ___187L__63S.pdf
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Additional details
- Eprint ID
- 94300
- Resolver ID
- CaltechAUTHORS:20190329-150047014
- NASA
- GP-27983
- NSF
- McDonald Observatory
- University of Minnesota
- Created
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2019-03-29Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field