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For refcode 1993AJ....106..907H:
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Copyright by American Astronomical Society. Reproduced by permission
1993AJ....106..907H THE DEPENDENCE OF THE COOL MATTER CONTENT ON GALAXY MORPHOLOGY IN GALAXIES OF TYPES E/S0, S0, AND Sa D. E. HOGG AND M. S. ROBERTS National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, Virginia 22903-2475 Electronic mail: dhogg@nrao.edu, mroberts@nrao.edu ALLAN SANDAGE The Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, California 91101 Electronic mail: ars@ociw.edu Received 1993 March 29; revised 1993 May 24 ABSTRACT Using the material assembled in earlier papers, we examine the manner in which the interstellar matter content varies along the Hubble sequence from S0 galaxies to Sa galaxies selected from the RSA2 compilation. For this we make use of a new and more detailed classification which is described here as applied to these early disk/spiral galaxies. The prominence of the disk in S0's and the visibility of features (H II regions) in the Sa's serve as the basis for the subtypes. Three S0 categories: subtle, intermediate, and pronounced, and four Sa descriptors: very early, early, intermediate, and late are assigned to the galaxies. It is found that the total amount of hydrogen (HI + H_2_) is a function of subtype, being low in the S0's and rising smoothly from the early Sa's to the later Sa's. The average surface density of hydrogen exceeds 3M_sun_ pc^-2^ only in the latest subtypes of the Sa's. We conclude that the prominence of the disk of a galaxy closely follows the amount of cool gas which the disk contains.
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