Connecting Transitions In Galaxy Properties To Refueling

dc.contributor.utaustinauthorJogee, Shardhaen_US
dc.creatorKannappan, Sheila J.en_US
dc.creatorStark, David V.en_US
dc.creatorEckert, Kathleen D.en_US
dc.creatorMoffett, Amanda J.en_US
dc.creatorWei, Lisa H.en_US
dc.creatorPisano, D. J.en_US
dc.creatorBaker, Andrew J.en_US
dc.creatorVogel, Stuart N.en_US
dc.creatorFabricant, Daniel G.en_US
dc.creatorLaine, Seppoen_US
dc.creatorNorris, Mark A.en_US
dc.creatorJogee, Shardhaen_US
dc.creatorLepore, Natashaen_US
dc.creatorHough, Loren E.en_US
dc.creatorWeinberg-Wolf, Jenniferen_US
dc.date.accessioned2016-04-28T19:41:53Z
dc.date.available2016-04-28T19:41:53Z
dc.date.issued2013-11en
dc.description.abstractWe relate transitions in galaxy structure and gas content to refueling, here defined to include both the external gas accretion and the internal gas processing needed to renew reservoirs for star formation. We analyze two z = 0 data sets: a high-quality similar to 200 galaxy sample (the Nearby Field Galaxy Survey, data release herein) and a volume-limited similar to 3000 galaxy sample with reprocessed archival data. Both reach down to baryonic masses similar to 10(9) M and span void-to-cluster environments. Two mass-dependent transitions are evident: (1) below the "gas-richness threshold" scale (V similar to 125 km s(-1)), gas-dominated quasi-bulgeless Sd-Im galaxies become numerically dominant; while (2) above the "bimodality" scale (V similar to 200 km s(-1)), gas-starved E/S0s become the norm. Notwithstanding these transitions, galaxy mass (or V as its proxy) is a poor predictor of gas-to-stellar mass ratio M-gas/M-*. Instead, M-gas/M-* correlates well with the ratio of a galaxy's stellar mass formed in the last Gyr to its preexisting stellar mass, such that the two ratios have numerically similar values. This striking correspondence between past-averaged star formation and current gas richness implies routine refueling of star-forming galaxies on Gyr timescales. We argue that this refueling underlies the tight M-gas/M-* versus color correlations often used to measure "photometric gas fractions." Furthermore, the threshold and bimodality scale transitions reflect mass-dependent demographic shifts between three refueling regimes-accretion-dominated, processing-dominated, and quenched. In this picture, gas-dominated dwarfs are explained not by inefficient star formation but by overwhelming gas accretion, which fuels stellar mass doubling in less than or similar to 1 Gyr. Moreover, moderately gas-rich bulged disks such as the Milky Way are transitional, becoming abundant only in the narrow range between the threshold and bimodality scales.en_US
dc.description.departmentAstronomyen_US
dc.description.sponsorshipNSF CAREER grant AST-0955368en_US
dc.description.sponsorshipGAANN Fellowshipsen_US
dc.description.sponsorshipNorth Carolina Space Grant Fellowshipsen_US
dc.description.sponsorshipNRAO Charlottesville visitor programen_US
dc.description.sponsorshipNASA Harriet Jenkins Fellowshipen_US
dc.description.sponsorshipUniversity of North Carolina Royster Society of Fellowsen_US
dc.description.sponsorshipNorth Carolina Space Grant Programen_US
dc.description.sponsorshipNSF under the CARMA cooperative agreementen_US
dc.description.sponsorshipSMA Postdoctoral Fellowshipen_US
dc.description.sponsorshipNorman Hackerman Advanced Research Program (NHARP) ARP-03658-0234-2009en_US
dc.description.sponsorshipNSF AST-0607748en_US
dc.description.sponsorshipHubble Space Telescope grant from STScI GO-11082en_US
dc.description.sponsorshipNASA NAS5-26555en_US
dc.description.sponsorshipNational Science Foundationen_US
dc.description.sponsorshipJPL/Caltechen_US
dc.description.sponsorshipAlfred P. Sloan Foundationen_US
dc.description.sponsorshipU.S. Department of Energy Office of Scienceen_US
dc.description.sponsorshipUniversity of Arizonaen_US
dc.description.sponsorshipBrookhaven National Laboratory, University of Cambridgeen_US
dc.description.sponsorshipCarnegie Mellon Universityen_US
dc.description.sponsorshipUniversity of Floridaen_US
dc.description.sponsorshipHarvard Universityen_US
dc.description.sponsorshipInstituto de Astrofisica de Canariasen_US
dc.description.sponsorshipJohns Hopkins Universityen_US
dc.description.sponsorshipLawrence Berkeley National Laboratoryen_US
dc.description.sponsorshipMax Planck Institute for Astrophysicsen_US
dc.description.sponsorshipNew Mexico State Universityen_US
dc.description.sponsorshipNew York Universityen_US
dc.description.sponsorshipOhio State Universityen_US
dc.description.sponsorshipPennsylvania State Universityen_US
dc.description.sponsorshipUniversity of Portsmouthen_US
dc.description.sponsorshipPrinceton Universityen_US
dc.description.sponsorshipUniversity of Tokyoen_US
dc.description.sponsorshipUniversity of Utahen_US
dc.description.sponsorshipVanderbilt Universityen_US
dc.description.sponsorshipUniversity of Virginiaen_US
dc.description.sponsorshipUniversity of Washingtonen_US
dc.description.sponsorshipYale Universityen_US
dc.description.sponsorship10A-070en_US
dc.identifierdoi:10.15781/T2JZ46
dc.identifier.Filename2013_11_connectingtransitions.pdfen_US
dc.identifier.citationKannappan, Sheila J., David V. Stark, Kathleen D. Eckert, Amanda J. Moffett, Lisa H. Wei, D. J. Pisano, Andrew J. Baker et al. "Connecting transitions in galaxy properties to refueling." The Astrophysical Journal, Vol. 777, No. 1 (Nov., 2013): 42.en_US
dc.identifier.doi10.1088/0004-637x/777/1/42en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/35124
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.relation.ispartofserialAstrophysical Journalen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.rights.restrictionOpenen_US
dc.subjectgalaxies: evolutionen_US
dc.subjecttully-fisher relationen_US
dc.subjectdigital sky surveyen_US
dc.subjectstar-formation ratesen_US
dc.subjectcolden_US
dc.subjectdark-matteren_US
dc.subjectfast alpha surveyen_US
dc.subject40-percent alfalfa surveyen_US
dc.subjectsupermassiveen_US
dc.subjectblack-holesen_US
dc.subjectstellar mass functionsen_US
dc.subjectnearby field galaxiesen_US
dc.subjectblue compacten_US
dc.subjectgalaxiesen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleConnecting Transitions In Galaxy Properties To Refuelingen_US
dc.typeArticleen_US

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