The coevolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshift

Abstract

It is well known that supermassive black holes (SMBHs) and their host galaxies co-evolve. A manifestation of this co-evolution is the correlation that has been found between the SMBH mass, M${}_{BH}$, and the galaxy bulge or stellar mass, M${}_{\ast }$. The cosmic evolution of this relation, though, is still a matter of debate. In this work, we examine the M${}_{BH}-$M${}_{\ast }$ relation, using 687 X-ray luminous (median $\log [{\mathrm{L}}_{\mathrm{X},2-10keV}(\mathrm{erg}{\mathrm{s}}^{-1})]=44.3$), broad line AGN, at $0.2<\mathrm{z}<4.0$ (median $\mathrm{z}\approx 1.4$) that lie in the XMM-{\it{XXL}} field. Their M${}_{BH}$ and M${}_{\ast }$ range from $7.5<\log [{\mathrm{M}}_{\mathrm{BH}}({\mathrm{M}}_{\odot })]<9.5$ and $10<\log [{\mathrm{M}}_{\ast }({\mathrm{M}}_{\odot })]<12$, respectively. Most of the AGN live in star-forming galaxies and their Eddington ratios range from 0.01 to 1, with a median value of 0.06. Our results show that M${}_{BH}$ and M${}_{\ast }$ are correlated ($\mathrm{r}=0.47\pm 0.21$, averaged over different redshift intervals). Our analysis also shows that the mean ratio of the M${}_{BH}$ and M${}_{\ast }$ does not evolve with redshift, at least up to $\mathrm{z}=2$ and has a value of $\log ($M${}_{BH}/$M${}_{\ast })=-2.44$. The majority of the AGN ($75\%$) are in a SMBH mass growth dominant phase. In these systems, the M${}_{BH}-$M${}_{\ast }$ correlation is weaker and their M${}_{\ast }$ tends to be lower (for the same M${}_{BH}$) compared to systems that are in a galaxy mass growth phase. Our findings suggest that the growth of black hole mass occurs first, while the early stellar mass assembly may not be so efficient.

Accepted for publication in A&A. 8 pages, 7 figures

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