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The roles that mass and environment play in the galaxy quenching are stillunder debate. Leveraging the Photometric objects Around Cosmic webs (PAC)method, we analyze the excess surface distribution$\bar{n}_2w_{\rm{p}}(r_{\rm{p}})$ of photometric galaxies in different color(rest-frame $u-r$) within the stellar mass range of$10^{9.0}M_{\odot}\sim10^{11.0}M_{\odot}$ around spectroscopic massive centralgalaxies ($10^{10.9}\sim10^{11.7}M_{\odot}$) at the redshift interval$0<z_s<0.7$, utilizing data from the Hyper SuprimeCam Subaru Strategic Programand the spectroscopic samples of Slogan Digital Sky Survey (i.e. Main, LOWZ andCMASS samples). We find that both mass and environment quenching contribute tothe evolution of companion galaxies. To isolate the environment effect, wequantify the quenched fraction excess (QFE) of companion galaxies encirclingmassive central galaxies within$0.01h^{-1}{\rm{Mpc}}<r_{\rm{p}}<20h^{-1}\rm{Mpc}$, representing the surplusquenched fraction relative to the average. We find that the high density haloenvironment affects the star formation quenching up to about three times of thevirial radius, and this effect becomes stronger at lower redshift. We also findthat even after being scaled by the virial radius, the environment quenchingefficiency is higher for more massive halos or for companion galaxies of higherstellar mass, though the trends are quite weak. We present a fitting formulathat comprehensively captures the QFE across central and companion stellar massbins, halo-centric distance bins, and redshift bins, offering a valuable toolfor constraining galaxy formation models. Furthermore, we have made aquantitative comparison with Illustris-TNG that underscores some importantdifferences, particularly in the excessive quenching of low-mass companiongalaxies ($<10^{9.5}M_{\odot}$) by TNG.

PAC.V. The Roles of Mass and Environment in the Quenching of Galaxies