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
  We present the results of clustering analyses of Lyman break galaxies (LBGs)
at $z\sim3$, $4$, 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 $\langle M_{h}
\rangle=10^{11.7}-10^{12.8}h^{-1}M_{\odot}$, 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, $M_{{\rm h}}^{{\rm pivot}}$,
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,
$M_{{\rm h}}^{{\rm pivot}}$ 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 $M_{{\rm
h}}\sim10^{12}M_{\odot}$ over cosmic time.
