Kavli Affiliate: Chiaki Hikage
| First 5 Authors: Wentao Luo, John D. Silverman, Surhud More, Andy Goulding, Hironao Miyatake
| Summary:
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 48907 AGNs constructed using HSC and WISE
photometry. %The lensing detection around AGNs has a signal to noise ratio of
textbf{29}. As expected, we find that the lensing mass profile of total AGN
sample is consistent with that of massive galaxies ($rm
log(M_{*}/h^{-2}M_odot)sim$ 10.61). Surprisingly, the lensing signal remains
unchanged when the AGN sample is split into four stellar mass bins of host
galaxies. 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 tends to suppress AGN activity, probably due to the lack of
available gas.
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