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dc.contributor.authorFinn, Rose A.
dc.contributor.authorDesai, Vandana
dc.contributor.authorRudnick, Gregory
dc.contributor.authorBalogh, Michael
dc.contributor.authorHaynes, Martha P.
dc.contributor.authorJablonka, Pascale
dc.contributor.authorKoopmann, Rebecca A.
dc.contributor.authorMoustakas, John
dc.contributor.authorPeng, Chien Y.
dc.contributor.authorPoggianti, Bianca
dc.contributor.authorRines, Kenneth
dc.contributor.authorZaritsky, Dennis
dc.date.accessioned2018-12-05T21:08:18Z
dc.date.available2018-12-05T21:08:18Z
dc.date.issued2018-08-01
dc.identifier.citationRose A. Finn et al 2018 ApJ 862 149en_US
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/aac32a
dc.identifier.urihttp://hdl.handle.net/10150/631113
dc.description.abstractThe goal of the Local Cluster Survey is to look for evidence of environmentally driven quenching among star-forming galaxies in nearby galaxy groups and clusters. Quenching is linked with environment and stellar mass, and much of the current observational evidence comes from the integrated properties of galaxies. However, the relative size of the stellar and star-forming disk is sensitive to environmental processing and can help identify the mechanisms that lead to a large fraction of quenched galaxies in dense environments. Toward this end, we measure the size of the star-forming disks for 224 galaxies in nine groups and clusters (0.02 < z < 0.04; SFR > 0.1 M-circle dot yr(-1)) using 24 mu m imaging from the Spitzer Space Telescope. We normalize the 24 mu m effective radius (R-24) by the size of the stellar disk (R-d). We find that star-forming galaxies with higher bulge-to-total ratios (BIT) and galaxies in more dense environments have more centrally concentrated star formation. Comparison with H mass fractions and NUV - r colors indicates that a galaxy's transition from gas-rich and blue to depleted and red is accompanied by an increase in the central concentration of star formation. We build a simple model to constrain the timescale over which the star-forming disks shrink in the cluster environment. Our results are consistent with a long-timescale (>2 Gyr) mechanism that produces outside-in quenching, such as the removal of the extended gas halo or weak stripping of the cold disk gas.en_US
dc.description.sponsorshipNSF [AST-0847430, AST-1107390]; NASA [NNX17AF25G]; Brinson Foundation; NASA; Undergraduate ALFALFA Team through NSF [AST-1211005, AST-0724918, AST-0725267, AST-0725380]en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.relation.urlhttp://stacks.iop.org/0004-637X/862/i=2/a=149?key=crossref.023f04f5a1590d4df8611f10a5f8d4c9en_US
dc.rights© 2018. The American Astronomical Society. All rights reserved.en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectgalaxies: clusters: generalen_US
dc.subjectgalaxies: evolutionen_US
dc.subjectgalaxies: groups: generalen_US
dc.subjectgalaxies: star formationen_US
dc.titleThe Local Cluster Survey. I. Evidence of Outside-in Quenching in Dense Environmentsen_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Steward Observen_US
dc.identifier.journalASTROPHYSICAL JOURNALen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleThe Astrophysical Journal
dc.source.volume862
dc.source.issue2
dc.source.beginpage149
refterms.dateFOA2018-12-05T21:08:18Z


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