http://arxiv.org/abs/1902.04087
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 $D_n4000$ 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 $\sim ! 10 \,\, M_\odot \,\, \mathrm{yr}^{-1}$ 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 $10^{10} \,\, M_\odot \lesssim M_{DM} \lesssim 10^{12} \,\, M_\odot$ and evolve parallel to the stellar mass-halo mass relation based on N-body simulations. Thus, the stellar mass-halo mass relation of massive galaxies apparently results primarily from dry minor merging.
H. Zahid, M. Geller, I. Damjanov, et. al.
Wed, 13 Feb 19
52/62
Comments: 22 pages, 18 figures. Submitted to ApJ. Comments welcome
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