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GALEX observations of low surface brightness galaxies: UV color and star formation efficiency

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dc.contributor.authorBoissier, S.
dc.contributor.authorGil De Paz, Armando
dc.contributor.authorBoselli, A.
dc.contributor.authorBuat, V.
dc.contributor.authorMadore, B.
dc.contributor.authorChemin, L.
dc.contributor.authorBalkowski, C.
dc.contributor.authorAmram, P.
dc.contributor.authorCarignan, C.
dc.contributor.authorvan Driel, W.
dc.date.accessioned2023-06-20T11:07:48Z
dc.date.available2023-06-20T11:07:48Z
dc.date.issued2008-07-01
dc.description© 2008. The American Astronomical Society. All rights reserved. We thank the referee, Stacy McGaugh, for his very constructive comments, as well as David Thilker and Ted Wyder for discussions. This research is first based on the GALEX GI program GALEXGII04-0000-0067, as well as public archival data, available at the MAST archive. This research has made use of the NASA/ IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr). This research has made use of the GOLD Mine Database.
dc.description.abstractWe present GALEX UV observations of a sample of low surface brightness (LSB) galaxies for which H I data are available, allowing us to estimate their star formation efficiency. We find that the UV light extends to larger radii than the optical light (some galaxies, but not all, look similar to the recently discovered XUV-disk galaxies). Using a standard calibration to convert the UV light into star formation rates, we obtain lower star formation efficiencies in LSB galaxies than in high surface brightness galaxies by about one order of magnitude. We show, however, that standard calibrations may not apply to these galaxies, as the FUV–NUV color obtained from the two GALEX bands (FUV and NUV; λ_eff = 1516 and 2267 Å, respectively) is redder than expected for star-forming galaxies. This color can be interpreted as a result of internal extinction, modified initial mass function, or star formation histories characterized by bursts followed by quiescent phases. Our analysis favors this latter hypothesis.
dc.description.departmentDepto. de Física de la Tierra y Astrofísica
dc.description.facultyFac. de Ciencias Físicas
dc.description.refereedTRUE
dc.description.sponsorshipNational Aeronautics and Space Administration (NASA)
dc.description.statuspub
dc.eprint.idhttps://eprints.ucm.es/id/eprint/35635
dc.identifier.doi10.1086/588580
dc.identifier.issn0004-637X
dc.identifier.officialurlhttp://dx.doi.org/10.1086/588580
dc.identifier.relatedurlhttp://iopscience.iop.org/
dc.identifier.urihttps://hdl.handle.net/20.500.14352/51744
dc.issue.number1
dc.journal.titleAstrophysical journal
dc.language.isoeng
dc.page.final257
dc.page.initial244
dc.publisherAmerican Astronomical Society
dc.rights.accessRightsopen access
dc.subject.cdu52
dc.subject.keywordTully-fisher relation
dc.subject.keywordChemo-spectrophotometric evolution
dc.subject.keywordSpectral energy-distribution
dc.subject.keywordResolution rotation curves
dc.subject.keywordLow-mass stars
dc.subject.keywordDisk galaxies
dc.subject.keywordForming galaxies
dc.subject.keywordVirgo cluster
dc.subject.keywordFormation thresholds
dc.subject.keywordFormation history
dc.subject.ucmAstrofísica
dc.subject.ucmAstronomía (Física)
dc.titleGALEX observations of low surface brightness galaxies: UV color and star formation efficiency
dc.typejournal article
dc.volume.number681
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