Published July 15, 1975
| Published
Journal Article
Open
Molecular clouds in the Galaxy
- Creators
-
Scoville, N. Z.
- Solomon, P. M.
Chicago
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Abstract
The J = 1 → 0 emission of CO has been surveyed in the galactic plane between ℓ = -10° and +90° with a U beam sampling every degree. Molecular clouds emitting in the CO line are plentiful over the inner region of the Galaxy. Their greatest number occurs in the galactic nucleus and at a radius of 5.5 kpc—a distribution similar to radio H II regions and galactic γ-ray emission but very different from that previously derived for atomic hydrogen. The total mass in molecular clouds is found to be 1-3 x 10^9 and each typically has 10^5 M_⊙, an H_2 density of 700 cm^(-3), and a temperature near 7 K. These results suggest that most of the interstellar medium in the interior of the Galaxy is molecular H_2.
Additional Information
© 1975. The American Astronomical Society. Received 1975 February 19; revised 1975 April 8. This research is sponsored in part by the National Science Foundation grants GP-30400-X5 (N.S.) and GP-40768X (P.S.) and by the Office of Naval Research under contract N0014-67-A-0094-0019 (N.S.).Attached Files
Published - 1975ApJ___199L_105S.pdf
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Additional details
- Eprint ID
- 94429
- Resolver ID
- CaltechAUTHORS:20190403-153008367
- NSF
- GP-30400-X5
- Office of Naval Research (ONR)
- N0014-67-A-0094-0019
- Created
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2019-04-11Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field