  We provide a method for estimating the projected density distribution
$\bar{n}_2w_p(r_p)$ of photometric objects around spectroscopic objects in a
redshift survey. This quantity describes the distribution of Photometric
sources with certain physical properties (e.g. luminosity, mass, color etc)
Around Cosmic webs (PAC) traced by the spectroscopic objects. The method can
make full use of current and future deep and wide photometric surveys to
explore the formation of galaxies up to medium redshift ($z_s < 2$), with the
aid of cosmological redshift surveys that sample only a fairly limited species
of objects (e.g. Emission Line Galaxies). As an example, we apply the PAC
method to the CMASS spectroscopic and HSC-SSP PDR2 photometric samples to
explore the distribution of galaxies for a wide range of stellar mass from
$10^{9.0}{\rm M_\odot}$ to $10^{12.0}{\rm M_\odot}$ around massive ones at
$z_s\approx 0.6$. Using the abundance matching method, we model
$\bar{n}_2w_p(r_p)$ in N-body simulation using MCMC sampling, and accurately
measure the stellar-halo mass relation (SHMR) and stellar mass function (SMF)
for the whole mass range. We can also measure the conditional stellar mass
function (CSMF) of satellites for central galaxies of different mass. The PAC
method has many potential applications for studying the evolution of galaxies.
