Black Hole and Galaxy Coevolution in Moderately Luminous Active Galactic Nuclei at z~1.4 in SXDF

TL;DR

This study examines the relationship between black hole mass and host galaxy properties in moderately luminous AGNs at z~1.4, revealing that these galaxies are in a phase of active SMBH growth and have established local black hole-bulge relations.

Contribution

It provides new insights into black hole and galaxy coevolution at z~1.4 using spectral energy distribution modeling of X-ray selected AGNs.

Findings

Black hole to stellar mass ratio similar to local universe

Most host galaxies are main-sequence star-forming galaxies

AGNs are in a SMBH-growth dominant phase

Abstract

We investigate the relation of black hole mass versus host stellar mass and that of mass accretion rate versus star formation rate (SFR) in moderately luminous ($\log L_{\rm bol} \sim 44.5-46.5\ {\rm erg\ s^{-1}}$), X-ray selected broad-line active galactic nuclei (AGNs) at $z=1.18-1.68$ in the Subaru/XMM-Newton Deep Field. The far-infrared to far-ultraviolet spectral energy distributions of 85 AGNs are reproduced with the latest version of Code Investigating GALaxy Emission ({\tt CIGALE}), where the AGN clumpy torus model {\tt SKIRTOR} is implemented. Most of their hosts are confirmed to be main-sequence star-forming galaxies. We find that the mean ratio of the black hole mass ($M_{\rm BH}$) to the total stellar mass ($M_{\rm stellar}$) is $\log M_{\rm BH}/M_{\rm stellar} = -2.2$, which is similar to the local black hole-to-bulge mass ratio. This suggests that if the host galaxies of these moderately luminous AGNs at $z\sim1.4$ are dominated by bulges, they already established the local black hole mass-bulge mass relation; if they are disk dominant, their black holes are overmassive relative to the bulges. AGN bolometric luminosities and SFR show a good correlation with ratios higher than that expected from the local black hole-to-bulge mass relation, suggesting that these AGNs are in a SMBH-growth dominant phase.