  In this paper, we report a robust measurement of the morphology, color and
galaxy size dependences of the stellar-halo mass relation (SHMR) at the high
mass end ($10^{11.3}{\rm M_{\odot}}<M_{\star}<10^{11.7}{\rm M_{\odot}}$) at
redshift $z_s\sim0.6$ (Throughout the paper, we use $z_s$ for redshift, $z$ for
the z-band magnitude.). Applying our method, Photometric objects Around Cosmic
webs (PAC), developed in a previous work to CMASS and HSC-SSP observations, we
measure the excess surface density ($\bar{n}_2w_p(r_p)$) of satellites around
massive central galaxies with different morphologies indicated by S\'ersic
index $n$. We find that more compact (larger $n$) central galaxies are
surrounded by more satellites. With the abundance matching method, we estimate
halo mass for the central galaxies, and find that halo mass is increased
monotonically with $n$, solid evidence for a morphology dependence of SHMR.
Specifically, our results show that the most compact galaxies ($n>6$) have the
halo mass around 5.5 times larger than the disk galaxies ($n<2$). Similarly,
using the effective radius $R_e$ and the rest-frame $u-r$ color, we find that
red (large) galaxies reside in halos that are in average $2.6$ ($2.3$) times
more massive than those hosting blue (small) galaxies.
