{"id":792530,"date":"2021-11-04T21:35:37","date_gmt":"2021-11-05T04:35:37","guid":{"rendered":"https:\/\/www.microsoft.com\/en-us\/research\/?post_type=msr-research-item&#038;p=792530"},"modified":"2021-11-04T21:46:16","modified_gmt":"2021-11-05T04:46:16","slug":"the-coevolution-of-massive-quiescent-galaxies-and-their-dark-matter-halos-over-the-last-6-billion-years","status":"publish","type":"msr-research-item","link":"https:\/\/www.microsoft.com\/en-us\/research\/publication\/the-coevolution-of-massive-quiescent-galaxies-and-their-dark-matter-halos-over-the-last-6-billion-years\/","title":{"rendered":"The Coevolution of Massive Quiescent Galaxies and Their Dark Matter Halos over the Last 6 Billion Years"},"content":{"rendered":"<p>We investigate the growth of massive quiescent galaxies at <i>z<\/i>\u00a0<\u00a00.6 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 <i>D<\/i><sub><i>n<\/i><\/sub>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 <img decoding=\"async\" src=\"https:\/\/cfn-live-content-bucket-iop-org.s3.amazonaws.com\/journals\/0004-637X\/878\/2\/158\/1\/apjab21b9ieqn1.gif?AWSAccessKeyId=AKIAYDKQL6LTV7YY2HIK&Expires=1636691078&Signature=0NOhCrdFGtg19fme1qLhQG33LU4%3D\" alt=\"$\\sim 10\\,{M}_{\\odot }\\,{\\mathrm{yr}}^{-1}$\" \/>, and dark matter growth rates from our empirical model are remarkably consistent with <i>N<\/i>-body simulations. Massive quiescent galaxies grow by minor mergers with dark matter halos of mass <img decoding=\"async\" src=\"https:\/\/cfn-live-content-bucket-iop-org.s3.amazonaws.com\/journals\/0004-637X\/878\/2\/158\/1\/apjab21b9ieqn2.gif?AWSAccessKeyId=AKIAYDKQL6LTV7YY2HIK&Expires=1636691078&Signature=Un8pKFendVwLXEWl9OWfakZQ9c0%3D\" alt=\"${10}^{10}\\,{M}_{\\odot }\\lesssim {M}_{\\mathrm{DM}}\\lesssim {10}^{12}\\,{M}_{\\odot }$\" \/> and evolve parallel to the stellar mass\u2013halo mass (SMHM) relation based on <i>N<\/i>-body simulations. Thus, the SMHM relation of massive galaxies apparently results primarily from dry minor merging.<\/p>\n","protected":false},"excerpt":{"rendered":"<p>We investigate the growth of massive quiescent galaxies at z\u00a0<\/p>\n","protected":false},"featured_media":0,"template":"","meta":{"msr-url-field":"","msr-podcast-episode":"","msrModifiedDate":"","msrModifiedDateEnabled":false,"ep_exclude_from_search":false,"_classifai_error":"","msr-author-ordering":null,"msr_publishername":"","msr_publisher_other":"","msr_booktitle":"","msr_chapter":"","msr_edition":"","msr_editors":"","msr_how_published":"","msr_isbn":"","msr_issue":"","msr_journal":"The Astrophysical 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