The relationship of SMBHs and host galaxies at $z<4$ in the deep optical variability-selected AGN sample in the COSMOS field

Abstract

We present the study on the relationship between SMBHs and their host galaxies using our variability-selected AGN sample ($i_{\mathrm{AB}}\le 25.9,z\le 4.5$) constructed from the HSC-SSP Ultra-deep survey in the COSMOS field. We estimated the BH mass ($M_{\mathrm{BH}}=10^{5.5-10}{M}_{\odot }$) based on the single-epoch virial method and the total stellar mass ($M_{\mathrm{star}}=10^{10-12}{M}_{\odot }$) by separating the AGN component with SED fitting. We found that the redshift evolution of the BH-stellar mass ratio ($M_{\mathrm{BH}}/M_{\mathrm{star}}$) depends on the $M_{\mathrm{BH}}$ which is caused by the no significant correlation between $M_{\mathrm{BH}}$ and $M_{\mathrm{star}}$. Variable AGNs with massive SMBHs ($M_{\mathrm{BH}}>10^9{M}_{\odot }$) at $1.5<z<3$ show considerably higher BH-stellar mass ratios ($>\sim 1\%$) than the BH-bulge ratios ($M_{\mathrm{BH}}/M_{\mathrm{bulge}}$) observed in the local universe for the same BH range. This implies that there is a typical growth path of massive SMBHs which is faster than the formation of the bulge component as final products seen in the present day. For the low-mass SMBHs ($M_{\mathrm{BH}}<10^8{M}_{\odot }$) at $0.5<z<3$, on the other hand, variable AGNs show the similar BH-stellar mass ratios with the local objects ($\sim 0.1\%$) but smaller than those observed at $z>4$. We interpret that host galaxies harboring less massive SMBHs at intermediate redshift have already acquired sufficient stellar mass, although high-z galaxies are still in the early stage of galaxy formation relative to those at the intermediate/local universe.

Accepted for publication in ApJ, 14 pages, 5 figures

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