Abstract
We present the results of clustering analyses of Lyman break galaxies (LBGs)
at $z 3$, $4$, 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. The mean halo masses, calculated as $M_h =
10^11.7 - 10^12.8 h^-1 M_ødot$, increase with stellar-mass limit of
LBGs. The threshold halo mass to have a central galaxy, $M_min$,
follows the same increasing trend with the low-$z$ results, whereas the
threshold halo mass to have a satellite galaxy, $M_1$, shows higher values at
$z = 3 - 5$ than $z = 0.5 - 1.5$ over the entire stellar mass range. Along with
considering the low satellite fractions in high-$z$, these results suggest that
satellite galaxies form inefficiently within dark haloes at $z=3-5$ even for
less massive satellites with $M_\star < 10^10 M_ødot$. 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 show, for the first time observationally, the
increasing trend of $M_h^pivot$, which is the halo mass with a
peak SHMR, with cosmic time at $z > 3$, and with keeping the constant
star-formation efficiency indicates that mass growth rates of stellar
components and dark haloes are comparable at $3 < z < 5$.
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