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The Photometric objects Around Cosmic webs (PAC) approach developed in \cite{2022ApJ...925...31X} has the advantage of making full use of the spectroscopic and deeper photometric surveys. With the merits of PAC, we can accurately measure quasars-galaxy cross-correlations at small scale down to $0.1\,h^{-1}{\rm{Mpc}}$ and at different stellar mass bins. We calculate the excess surface density $\bar{n}_2w_{{\rm{p}}}$ of photometric objects around quasars down to stellar mass $10^{10.80}\,M_{\odot}$ at redshift $0.8<z_s$\footnote{Throughout the paper, we use $z_s$ for spectroscopic redshift, $z$ for the $z$-band magnitude.}$<1.0$, with the data from the Sloan Digital Sky Survey IV (SDSS-IV) extended Baryon Oscillation Spectroscopic Survey (eBOSS) and the Dark Energy Spectroscopic Instrument (DESI) Legacy Imaging Surveys. Using subhalo abundance matching method, we can precisely model the stellar halo mass relation (SHMR) of galaxies and quasar-halo relation. Under the assumption that the probability of a (sub)halo becoming a quasar follows a Gaussian distribution of logarithmic halo mass $\log_{10}(M_{{\rm{h}}}/h^{-1}M_{\odot})$ and with a parameter to describe satellite fraction, we find that $\mu$ and $\sigma_{q}$ are $13.91_{-0.71}^{+0.68}$ and $0.91_{-0.23}^{+0.19}$ respectively at redshift 0.8 - 1.0 and notice a high satellite fraction of quasars around galaxies with $f_{\mathrm{q}}=0.23_{-0.02}^{+0.01}$. These findings enhance our understanding of the environment quasar lives in and the accurate connection between quasars and halos.