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The Coevolution of Massive Quiescent Galaxies and Their Dark Matter Halos over the Last 6 Billion Years
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Zahid, H. Jabran | - |
dc.contributor.author | Geller, Margaret J. | - |
dc.contributor.author | Damjanov, Ivana | - |
dc.contributor.author | Sohn, Jubee | - |
dc.date.accessioned | 2024-05-03T02:26:51Z | - |
dc.date.available | 2024-05-03T02:26:51Z | - |
dc.date.created | 2024-05-03 | - |
dc.date.created | 2024-05-03 | - |
dc.date.issued | 2019-06 | - |
dc.identifier.citation | ASTROPHYSICAL JOURNAL, Vol.878 No.2 | - |
dc.identifier.issn | 0004-637X | - |
dc.identifier.uri | https://hdl.handle.net/10371/200747 | - |
dc.description.abstract | We investigate the growth of massive quiescent galaxies at z < 0.6 based on the Sloan Digital Sky Survey and the Smithsonian Hectospec Lensing Survey, two magnitude-limited spectroscopic surveys of high data quality and completeness. Our three-parameter model links quiescent galaxies across cosmic time by self-consistently evolving stellar mass, stellar population age-sensitive D(n)4000 index, half-light radius, and stellar velocity dispersion. Stellar velocity dispersion is a robust proxy of dark matter halo mass; we use it to connect galaxies and dark matter halos and thus empirically constrain their coevolution. The typical rate of stellar mass growth is -similar to 10 M-circle dot yr(-1), and dark matter growth rates from our empirical model are remarkably consistent with N-body simulations. Massive quiescent galaxies grow by minor mergers with dark matter halos of mass 10(10)M(circle dot) less than or similar to M-DM less than or similar to 10(12) M-circle dot and evolve parallel to the stellar mass-halo mass (SMHM) relation based on N-body simulations. Thus, the SMHM relation of massive galaxies apparently results primarily from dry minor merging. | - |
dc.language | 영어 | - |
dc.publisher | IOP PUBLISHING LTD | - |
dc.title | The Coevolution of Massive Quiescent Galaxies and Their Dark Matter Halos over the Last 6 Billion Years | - |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/ab21b9 | - |
dc.citation.journaltitle | ASTROPHYSICAL JOURNAL | - |
dc.identifier.wosid | 000472939700006 | - |
dc.identifier.scopusid | 2-s2.0-85069532961 | - |
dc.citation.number | 2 | - |
dc.citation.volume | 878 | - |
dc.description.isOpenAccess | Y | - |
dc.contributor.affiliatedAuthor | Sohn, Jubee | - |
dc.type.docType | Article | - |
dc.description.journalClass | 1 | - |
dc.subject.keywordPlus | DIGITAL SKY SURVEY | - |
dc.subject.keywordPlus | STELLAR POPULATION SYNTHESIS | - |
dc.subject.keywordPlus | VELOCITY-DISPERSION EVOLUTION | - |
dc.subject.keywordPlus | LARGE-SCALE STRUCTURE | - |
dc.subject.keywordPlus | STAR-FORMATION | - |
dc.subject.keywordPlus | FUNDAMENTAL PLANE | - |
dc.subject.keywordPlus | REDSHIFT SURVEY | - |
dc.subject.keywordPlus | SIZE EVOLUTION | - |
dc.subject.keywordPlus | STRUCTURAL-PROPERTIES | - |
dc.subject.keywordPlus | PHYSICAL-PROPERTIES | - |
dc.subject.keywordAuthor | dark matter | - |
dc.subject.keywordAuthor | galaxies: evolution | - |
dc.subject.keywordAuthor | galaxies: formation | - |
dc.subject.keywordAuthor | galaxies: kinematics and dynamics | - |
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