The relationship of SMBHs and host galaxies at $z<4$ in the deep optical variability-selected AGN sample in the COSMOS field Atsushi Hoshi, Toru Yamada, Mitsuru Kokubo, Yoshiki Matsuoka, Tohru Nagao arXiv:2404.13561v1 Announce Type: new Abstract: We present the study on the relationship between SMBHs and their host galaxies using our variability-selected AGN sample ($i_mathrm{AB} leq 25.9, z leq 4.5$) 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 $1.5sim1%$) 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 ($M_mathrm{BH} 4$. 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.arXiv:2404.13561v1 Announce Type: new
Abstract: We present the study on the relationship between SMBHs and their host galaxies using our variability-selected AGN sample ($i_mathrm{AB} leq 25.9, z leq 4.5$) 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 $1.5sim1%$) 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 ($M_mathrm{BH} 4$. 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.

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