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The Star Formation Relation in Nearby Galaxies

Published online by Cambridge University Press:  21 March 2013

Andreas Schruba
Andreas Schruba*
Affiliation:
Cahill Center for Astronomy and Astrophysics, California Institute of Technology, MC 249-17, 1200 E California Blvd, Pasadena, CA 91125, USA email: schruba@astro.caltech.edu
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Abstract

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I review observational studies of the large-scale star formation process in nearby galaxies. A wealth of new multi-wavelength data provide an unprecedented view on the interplay of the interstellar medium and (young) stellar populations on a few hundred parsec scale in 100+ galaxies of all types. These observations enable us to relate detailed studies of star formation in the Milky Way to the zoo of galaxies in the distant universe. Within the disks of spiral galaxies, recent star formation strongly scales with the local amount of molecular gas (as traced by CO) with a molecular gas depletion time of ∼2 Gyr. This is consistent with the picture that stars form in giant molecular clouds that have about universal properties. Galaxy centers and star-bursting galaxies deviate from this normal trend as they show enhanced star formation per unit gas mass suggesting systematic changes in the molecular gas properties and especially the dense gas fraction. In the outer disks of spirals and in dwarf galaxies, the decreasing availability of atomic gas inevitably limits the amount of star formation, though with large local variations. The critical step for the gas-stars cycle seems therefore to be the formation of a molecular gas phase, a process that shows complex dependencies on various environmental properties and is being investigated by intensive simulational work.

Keywords

galaxies: evolution — galaxies: ISM — ISM: molecules — radio lines: ISM — radio lines: galaxies
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S292: Molecular Gas, Dust, and Star Formation in Galaxies , August 2012 , pp. 311 - 318
Copyright
Copyright © International Astronomical Union 2013

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