The XMM-Newton Wide Field Survey in the COSMOS Field: Clustering Dependence of X-ray Selected AGN on Host Galaxy Properties

Abstract

We study the spatial clustering through the projected two-point correlation function of $632$ $(1130)$ XMM-COSMOS Active Galactic Nuclei (AGNs) with known spectroscopic (spectroscopic or photometric) redshifts in the range $z=[0.1-2.5]$ in order to measure the AGN bias and estimate the typical mass of the hosting dark matter (DM) halo as a function of AGN host galaxy properties. We create AGN subsamples in terms of stellar mass $M_{\ast }$ and specific black hole accretion rate $L_X/M_{\ast }$, to probe how AGN environment depends on these quantities. For the full spectroscopic AGN sample, we measure a typical DM halo mass of $\log (M_{\mathrm{halo}}/h^{-1}{\mathrm{M}}_{\odot })=12.79_{-0.43}^{+0.26}$, similar to galaxy group environments and in line with previous studies for moderate-luminosity X-ray selected AGN. We find no significant dependence on $L_X/M_{\ast }$, with $\log (M_{\mathrm{halo}}/h^{-1}{\mathrm{M}}_{\odot })=13.06_{-0.38}^{+0.23}$ ($12.97_{-1.26}^{+0.39}$) for the low (high) $L_X/M_{\ast }$ subsample. We also find no difference in the hosting halos in terms of $M_{\ast }$ with $\log (M_{\mathrm{halo}}/h^{-1}{\mathrm{M}}_{\odot })=12.93_{-0.62}^{+0.31}$ ($12.90_{-0.62}^{+0.30}$) for the low (high) $M_{\ast }$ subsample. By comparing the $M_{\ast }-M_{\mathrm{halo}}$ relation derived for XMM-COSMOS AGN subsamples with what is expected for normal non-active galaxies by abundance matching and clustering results, we find that the typical DM halo mass of our high $M_{\ast }$ AGN subsample is similar to that of non-active galaxies. However, AGNs in our low $M_{\ast }$ subsample are found in more massive halos than non-active galaxies. By excluding AGNs in galaxy groups from the clustering analysis, we find evidence that the result for low $M_{\ast }$ may be due a larger fraction of AGNs as satellites in massive halos.

arXiv comment11 pages, 8 figures, accepted to A&A

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