The Spitzer South Pole Telescope Deep Field Survey: Linking galaxies and halos at z=1.5

Abstract

We present an analysis of the clustering of high-redshift galaxies in the recently completed 94 deg${}^2$ Spitzer-SPT Deep Field survey. Applying flux and color cuts to the mid-infrared photometry efficiently selects galaxies at $z\sim 1.5$ in the stellar mass range $10^{10}-10^{11}{M}_{\odot }$, making this sample the largest used so far to study such a distant population. We measure the angular correlation function in different flux-limited samples at scales $>6^{\prime \prime }$ (corresponding to physical distances $>0.05$ Mpc) and thereby map the one- and two-halo contributions to the clustering. We fit halo occupation distributions and determine how the central galaxy's stellar mass and satellite occupation depend on the halo mass. We measure a prominent peak in the stellar-to-halo mass ratio at a halo mass of $\log (M_{\mathrm{halo}}/M_{\odot })=12.44\pm 0.08$, 4.5 times higher than the $z=0$ value. This supports the idea of an evolving mass threshold above which star formation is quenched. We estimate the large-scale bias in the range $b_g=2-4$ and the satellite fraction to be $f_{\mathrm{sat}}\sim 0.2$, showing a clear evolution compared to $z=0$. We also find that, above a given stellar mass limit, the fraction of galaxies that are in similar mass pairs is higher at $z=1.5$ than at $z=0$. In addition, we measure that this fraction mildly increases with the stellar mass limit at $z=1.5$, which is the opposite of the behavior seen at low-redshift.

32 pages, 22 figures. Published in MNRAS

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Cited by in corpus (4)

• Candidate Clusters of Galaxies at $z>1.3$ Identified in the Spitzer SPT Deep Field Survey
• Angular clustering and host halo properties of [OII] emitters at $z>1$ in the Subaru HSC survey
• The Stellar-to-Halo Mass Ratios of Passive and Star-Forming Galaxies at z~2-3 from the SMUVS survey
• The informativeness of [C II] line-intensity mapping as a probe of the H I content and metallicity of galaxies at the end of reionization