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Linking galaxies to dark matter halos at z ~ 1 : dependence of galaxy clustering on stellar mass and specific star formation rate.

Kim, Jae-Woo and Im, Myungshin and Lee, Seong-Kook and Edge, Alastair C. and Wake, David A. and Merson, Alexander I. and Jeon, Yiseul (2015) 'Linking galaxies to dark matter halos at z ~ 1 : dependence of galaxy clustering on stellar mass and specific star formation rate.', The Astrophysical Journal, 806 (2). p. 189.


We study the dependence of angular two-point correlation functions on stellar mass (M*) and specific star formation rate (sSFR) of ${M}_{*}\gt {10}^{10}{M}_{\odot }$ galaxies at $z\sim 1$. The data from the UK Infrared Telescope Infrared Deep Sky Survey Deep eXtragalactic Survey and Canada–France–Hawaii Telescope Legacy Survey cover 8.2 deg2 sample scales larger than 100 ${h}^{-1}\;\mathrm{Mpc}$ at $z\sim 1$, allowing us to investigate the correlation between clustering, M*, and star formation through halo modeling. Based on halo occupation distributions (HODs) of M* threshold samples, we derive HODs for M* binned galaxies, and then calculate the ${M}_{*}/{M}_{\mathrm{halo}}$ ratio. The ratio for central galaxies shows a peak at ${M}_{\mathrm{halo}}\sim {10}^{12}{h}^{-1}{M}_{\odot }$, and satellites predominantly contribute to the total stellar mass in cluster environments with ${M}_{*}/{M}_{\mathrm{halo}}$ values of 0.01–0.02. Using star-forming galaxies split by sSFR, we find that main sequence galaxies ($\mathrm{log}\;\mathrm{sSFR}/{\mathrm{yr}}^{-1}\sim -9$) are mainly central galaxies in $\sim {10}^{12.5}{h}^{-1}{M}_{\odot }$ halos with the lowest clustering amplitude, while lower sSFR galaxies consist of a mixture of both central and satellite galaxies where those with the lowest M* are predominantly satellites influenced by their environment. Considering the lowest ${M}_{\mathrm{halo}}$ samples in each M* bin, massive central galaxies reside in more massive halos with lower sSFRs than low mass ones, indicating star-forming central galaxies evolve from a low M*–high sSFR to a high M*–low sSFR regime. We also find that the most rapidly star-forming galaxies ($\mathrm{log}\;\mathrm{sSFR}/{\mathrm{yr}}^{-1}\gt -8.5$) are in more massive halos than main sequence ones, possibly implying galaxy mergers in dense environments are driving the active star formation. These results support the conclusion that the majority of star-forming galaxies follow secular evolution through the sustained but decreasing formation of stars.

Item Type:Article
Keywords:Galaxies: evolution, Galaxies: halos, Large-scale structure of universe.
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Publisher statement:© 2015. The American Astronomical Society. All rights reserved.
Date accepted:05 May 2015
Date deposited:12 November 2015
Date of first online publication:June 2015
Date first made open access:No date available

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