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Title:
The Star Formation Demographics of Galaxies in the Local Volume
Authors:
Lee, Janice C.; Kennicutt, Robert C.; Funes, S. J., José G.; Sakai, Shoko; Akiyama, Sanae
Affiliation:
AA(Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101; .; Hubble Fellow.), AB(Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK.; Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721.), AC(Specola Vaticana, V-00120 Vatican.), AD(Division of Astronomy and Astrophysics, University of California, Los Angeles, CA 90095.), AE(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721.)
Publication:
The Astrophysical Journal, Volume 671, Issue 2, pp. L113-L116. (ApJL Homepage)
Publication Date:
12/2007
Origin:
UCP
ApJ Keywords:
Galaxies: Dwarf, Galaxies: Evolution, Galaxies: Fundamental Parameters, Galaxies: ISM, Galaxies: Stellar Content, Stars: Formation
DOI:
10.1086/526341
Bibliographic Code:
2007ApJ...671L.113L

Abstract

We examine the connections between the current global star formation activity, luminosity, dynamical mass, and morphology of galaxies in the Local Volume, using Hα data from the 11 Mpc Hα and Ultraviolet Galaxy Survey (11HUGS). Taking the equivalent width (EW) of the Hα emission line as a tracer of the specific star formation rate, we analyze the distribution of galaxies in the MB-EW and rotational velocity (Vmax)-EW planes. Star-forming galaxies show two characteristic transitions in these planes. A narrowing of the galaxy locus occurs at MB~-15 and Vmax~50 km s-1, where the scatter in the logarithmic EWs drops by a factor of 2 as the luminosities/masses increase, and galaxy morphologies shift from predominately irregular to late-type spiral. Another transition occurs at MB~-19 and Vmax~120 km s-1, above which the sequence turns off toward lower EWs and becomes mostly populated by intermediate- and early-type bulge-prominent spirals. Between these two transitions, the mean logarithmic EW appears to remain constant at 30 Å. We comment on how these features reflect established empirical relationships, and provide clues for identifying the large-scale physical processes that both drive and regulate star formation, with emphasis on the low-mass galaxies which dominate our approximately volume-limited sample.
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