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Molecular clouds in the Galaxy

Scoville, N. Z. and Solomon, P. M. (1975) Molecular clouds in the Galaxy. Astrophysical Journal, 199 . L105-L109. ISSN 0004-637X.

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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.

Item Type:Article
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Scoville, N. Z.0000-0002-0438-3323
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.).
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Office of Naval Research (ONR)N0014-67-A-0094-0019
Subject Keywords:galactic structure -- Galaxy, The -- molecules, interstellar
Record Number:CaltechAUTHORS:20190403-153008367
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:94429
Deposited By: George Porter
Deposited On:11 Apr 2019 19:51
Last Modified:03 Oct 2019 21:03

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