Interaction, star formation, and H I deficiency in E + S pairs

Details Interaction, star formation, and H I deficiency in E + S pairs Interaction, star formation, and H I deficiency in E + S pairs

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...430..179z&link_type=abstract

The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 430, no. 1, p. 179-185

Astronomy and Astrophysics

Astrophysics

12

Elliptical Galaxies, Far Infrared Radiation, Interacting Galaxies, Spiral Galaxies, Star Formation, Starburst Galaxies, Emission Spectra, Interstellar Matter

Scientific paper

We use a sample of mixed morphology (ellictical + spiral) pairs of galaxies to make a new study of star formation enhancement in spiral galaxies. The approach makes use of the fact that only the spiral component in each pair is likely to be a significant source of (FIR) or H I emission. We find at least a twofold enhanced FIR emission from about one-half of the late-type components in close pairs. There is evidence that a typical burst duration may be as short as 2-3 x 108 yr. The total H I masses of the spiral components are near normal. Little or no H I depletion in star formation-enhanced galaxies implies one or more of the following: (1) a bimodal IMF for the interaction-induced starburst activity; (2) a duration for the active phase of enhanced star formation of no more than 1-2 x 109 yr; or (3) a continuous source of gas replenishment. We find some evidence for an H I deficit in the currently most active star forming spiral. This argues for an transient phase change in up to 50% of the neutral gas during a burst event. We conclude that the Interstellar Matter (ISM) in our sample of pairs is clearly not predominantly molecular gas.

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