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The Molecular Gas Component of Galaxy Disks

Published online by Cambridge University Press:  01 June 2008

Leo Blitz
Leo Blitz*
Affiliation:
University of California, Berkeley Radio Astronomy Lab., 601 Campbell HallBerkeley, CA 94720-3411, USA email: [email protected]
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Abstract

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The molecular gas in galaxy disks shows much more galaxy to galaxy variation than does the atomic gas. Detailed studies show that this variation can be attributed to differences in hydrostatic pressure in the disks due largely to variations in the stellar surface density and the total gas surface density. One prediction of pressure modulated H2 formation is that the location where HI and H2 have equal surface densities occurs at a constant value of the stellar surface density in the disk. Observations confirm this constancy to 40%.

Keywords

star formationgalaxiesgalaxy disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S254: The Galaxy Disk in Cosmological Context , June 2008 , pp. 307 - 312
Copyright
Copyright © International Astronomical Union 2009

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