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dc.creatorSomerville, Rachel S.en_US
dc.creatorBarden, Marcoen_US
dc.creatorRix, Hans-Walteren_US
dc.creatorBell, Eric F.en_US
dc.creatorBeckwith, Steven V. W.en_US
dc.creatorBorch, Andreaen_US
dc.creatorCaldwell, John A. R.en_US
dc.creatorHaussler, Borisen_US
dc.creatorHeymans, Catherineen_US
dc.creatorJahnke, Knuden_US
dc.creatorJogee, Shardhaen_US
dc.creatorMcIntosh, Daniel H.en_US
dc.creatorMeisenheimer, Klausen_US
dc.creatorPeng, Chen Y.en_US
dc.creatorSanchez, Sebastian F.en_US
dc.creatorWisotzki, Lutzen_US
dc.creatorWolf, Christianen_US
dc.date.accessioned2016-04-28T19:39:11Z
dc.date.available2016-04-28T19:39:11Z
dc.date.issued2008-01en
dc.identifierdoi:10.15781/T2TZ4P
dc.identifier.citationSomerville, Rachel S., Marco Barden, Hans-Walter Rix, Eric F. Bell, Steven VW Beckwith, Andrea Borch, John AR Caldwell et al. "An Explanation for the Observed Weak Size Evolution of Disk Galaxies." The Astrophysical Journal, Vol. 672, No. 2 (Jan., 2008): 776.en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/35029
dc.description.abstractSurveys of distant galaxies with the Hubble Space Telescope and from the ground have shown that there is only mild evolution in the relationship between radial size and stellar mass for galactic disks from z similar to 1 to the present day. Using a sample of nearby disk-dominated galaxies from the Sloan Digital Sky Survey (SDSS) and high-redshift data from the GEMS (Galaxy Evolution from Morphology and SEDs) survey, we investigate whether this result is consistent with theoretical expectations within the hierarchical paradigm of structure formation. The relationship between virial radius and mass for dark matter halos in the Lambda CDM model evolves by about a factor of 2 over this interval. However, N-body simulations have shown that halos of a given mass have less centrally concentrated mass profiles at high redshift. When we compute the expected disk size-stellar mass distribution, accounting for this evolution in the internal structure of dark matter halos and the adiabatic contraction of the dark matter by the self-gravity of the collapsing baryons, we find that the predicted evolution in the mean size at fixed stellar mass since z similar to 1 is about 15%-20%, in good agreement with the observational constraints from GEMS. At redshift z similar to 2, the model predicts that disks at fixed stellar mass were on average only 60% as large as they are today. Similarly, we predict that the rotation velocity at a given stellar mass (essentially the zero point of the Tully-Fisher relation) is only about 10% larger at z similar to 1 (20% at z similar to 2) than at the present day.en_US
dc.description.sponsorshipNASA NAS5-26555, GO-9500, NAG5-13102en_US
dc.description.sponsorshipHST AR-10290en_US
dc.description.sponsorshipEuropean Communityメs Human Potential Program HPRN-CT-2002-00305 Euro3D RTNen_US
dc.description.sponsorshipGerman DFG SCHI 536/3-1en_US
dc.description.sponsorshipAlfred P. Sloan Foundationen_US
dc.description.sponsorshipNSFen_US
dc.description.sponsorshipDOEen_US
dc.description.sponsorshipJapaneseMonbukagakushoen_US
dc.description.sponsorshipThe Max Planck Societyen_US
dc.description.sponsorshipJapan Participation Groupen_US
dc.description.sponsorshipJohns Hopkins Universityen_US
dc.description.sponsorshipLos Alamos National Laboratoryen_US
dc.description.sponsorshipNewMexico State Universityen_US
dc.description.sponsorshipUniversity of Pittsburghen_US
dc.description.sponsorshipPrinceton Universityen_US
dc.description.sponsorshipThe United States Naval Observatoryen_US
dc.description.sponsorshipThe University of Washingtonen_US
dc.language.isoEnglishen_US
dc.relation.ispartofen_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.subjectcosmology : observationsen_US
dc.subjectgalaxies : evolutionen_US
dc.subjectgalaxies :en_US
dc.subjecthigh-redshiften_US
dc.subjectgalaxies : spiralen_US
dc.subjectsurveysen_US
dc.subjecttully-fisher relationen_US
dc.subjectdark-matter halosen_US
dc.subjectangular-momentumen_US
dc.subjectstellar-systemsen_US
dc.subjectdensity profileen_US
dc.subjectbaryonic infallen_US
dc.subjectgalactic halosen_US
dc.subjecthigh-redshiften_US
dc.subjectblack-holesen_US
dc.subjectdeep fielden_US
dc.subjectastronomy & astrophysicsen_US
dc.titleAn Explanation For The Observed Weak Size Evolution Of Disk Galaxiesen_US
dc.typeArticleen_US
dc.description.departmentAstronomyen_US
dc.identifier.Filename2008_01_evolutiondiskgalaxies.pdfen_US
dc.rights.restrictionOpenen_US
dc.identifier.doi10.1086/523661en_US
dc.contributor.utaustinauthorCaldwell, John A. R.en_US
dc.relation.ispartofserialAstrophysical Journalen_US


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