Dark matter halos of luminous AGNs from galaxy-galaxy lensing with the
  HSC Subaru Strategic Program
  We assess the dark matter halo masses of luminous AGNs over the redshift
range 0.2 to 1.2 using galaxy-galaxy lensing based on imaging data from the
Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). We measure the weak
lensing signal of a sample of 8882 AGNs constructed using HSC and WISE
photometry. The lensing detection around AGNs has a signal-to-noise ratio of
15. As expected, we find that the lensing mass profile is consistent with that
of massive galaxies ($M_{*}\sim 10.8~M_\odot$). Surprisingly, the lensing
signal remains unchanged when the AGN sample is split into low and high stellar
mass hosts. Specifically, we find that the excess surface density (ESD) of
AGNs, residing in galaxies with high stellar masses, significantly differs from
that of the control sample. We further fit a halo occupation distribution model
to the data to infer the posterior distribution of parameters including the
average halo mass. We find that the characteristic halo mass of the full AGN
population lies near the knee ($\rm log(M_h/h^{-1}M_{\odot})=12.0$) of the
stellar-to-halo mass relation (SHMR). Illustrative of the results given above,
the halo masses of AGNs residing in host galaxies with high stellar masses
(i.e., above the knee of the SHMR) falls below the calibrated SHMR while the
halo mass of the low stellar mass sample is more consistent with the
established SHMR. These results indicate that massive halos with higher
clustering bias tend to suppress AGN activity, probably due to the lack of
available gas.
