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The Ratio of H2 to HI Gas in Infrared Luminous Galaxies

Published online by Cambridge University Press:  14 August 2015

I. F. Mirabel  and
D. B. Sanders
I. F. Mirabel
Affiliation:
Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125
D. B. Sanders
Affiliation:
Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125

Abstract

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The majority of infrared active galaxies (ffir/fb ≥ 2) have molecular to atomic mass fractions in the range of 0.5 to 2.0. Among the galaxies with the higher infrared excesses there are spectacular cases of HI deficient systems, where less than 15% of the total mass of interstellar gas is in atomic form. The optical morphology of luminous infrared galaxies suggest that the overall mass fractions of molecular to atomic gas, and the infrared luminosities per nucleon of interstellar gas are enhanced during galaxy-galaxy interactions.

Type
Joint Commission Meeting
Information
Highlights of Astronomy , Volume 8: Highlights of Astronomy. As presented at the XXth General Assembly of the IAU, 1988 , 1989 , pp. 603 - 604
Copyright
Copyright © Kluwer 1989

References

Mirabel, I. F., and Sanders, D. B. 1988, Ap. J., 335, in press.Google Scholar
Soifer, B. T., Sanders, D. B., Madore, B. F., Neugebauer, G., Persson, C. J., Persson, S. E., and Rice, W. L. 1987, Ap. J., 320, 238.Google Scholar