The Galaxy--Halo Connection in High-Redshift Universe: Details and Evolution of Stellar-to-Halo Mass Ratios of Lyman Break Galaxies on CFHTLS Deep Fields

Abstract

We present the results of clustering analyses of Lyman break galaxies (LBGs) at $z\sim 3$, $4$, and $5$ using the final data release of the Canada--France--Hawaii Telescope Legacy Survey (CFHTLS). Deep- and wide-field images of the CFHTLS Deep Survey enable us to obtain sufficiently accurate two-point angular correlation functions to apply a halo occupation distribution analysis. Mean halo masses, calculated as $⟨M_h⟩=10^{11.7}-10^{12.8}{h}^{-1}{M}_{\odot }$, increase with stellar-mass limit of LBGs. The threshold halo mass to have a central galaxy follows the same increasing trend with the low-$z$ results, whereas the threshold halo mass to have a satellite galaxy shows higher values at $z=3-5$ than $z=0.5-1.5$ over the entire stellar mass range. Satellite fractions of dropout galaxies, even at less massive haloes, are found to drop sharply from $z=2$ down to less than $0.04$ at $z=3-5$. These results suggest that satellite galaxies form inefficiently within dark haloes at $z=3-5$ even for less massive satellites with $M_{\star }<10^{10}{M}_{\odot }$. We compute stellar-to-halo mass ratios (SHMRs) assuming a main sequence of galaxies, which is found to provide consistent SHMRs with those derived from a spectral energy distribution fitting method. The observed SHMRs are in good agreement with the model predictions based on the abundance-matching method within $1\sigma$ confidence intervals. We derive observationally, for the first time, $M_{\mathrm{h}}^{\mathrm{pivot}}$, which is the halo mass at a peak in the star-formation efficiency, at $3<z<5$, and it shows a little increasing trend with cosmic time at $z>3$. In addition, $M_{\mathrm{h}}^{\mathrm{pivot}}$ and its normalization are found to be almost unchanged during $0<z<5$. Our study shows an observational evidence that galaxy formation is ubiquitously most efficient near a halo mass of $M_{\mathrm{h}}\sim 10^{12}{M}_{\odot }$ over cosmic time.

arXiv comment15 pages, 11 figures, submitted to ApJ

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