The XMM-Newton Wide Field Survey in the COSMOS Field: Clustering Dependence of X-ray Selected AGN on Host Galaxy Properties. (arXiv:1906.07911v1 [astro-ph.GA])

The XMM-Newton Wide Field Survey in the COSMOS Field: Clustering Dependence of X-ray Selected AGN on Host Galaxy Properties. (arXiv:1906.07911v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Viitanen_A/0/1/0/all/0/1">A. Viitanen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allevato_V/0/1/0/all/0/1">V. Allevato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Finoguenov_A/0/1/0/all/0/1">A. Finoguenov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bongiorno_A/0/1/0/all/0/1">A. Bongiorno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cappelluti_N/0/1/0/all/0/1">N. Cappelluti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gilli_R/0/1/0/all/0/1">R. Gilli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miyaji_T/0/1/0/all/0/1">T. Miyaji</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Salvato_M/0/1/0/all/0/1">M. Salvato</a>

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 $M_*$ and specific black hole
accretion rate $L_X/M_*$, 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 $L_X/M_*$, 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) $L_X/M_*$ subsample. We also find no difference in the hosting
halos in terms of $M_*$ 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) $M_*$
subsample. By comparing the $M_*-M_mathrm{halo}$ 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 $M_*$ AGN subsample is similar to that of non-active galaxies.
However, AGNs in our low $M_*$ 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 $M_*$ may be due a larger
fraction of AGNs as satellites in massive halos.

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 $M_*$ and specific black hole
accretion rate $L_X/M_*$, 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 $L_X/M_*$, 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) $L_X/M_*$ subsample. We also find no difference in the hosting
halos in terms of $M_*$ 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) $M_*$
subsample. By comparing the $M_*-M_mathrm{halo}$ 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 $M_*$ AGN subsample is similar to that of non-active galaxies.
However, AGNs in our low $M_*$ 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 $M_*$ may be due a larger
fraction of AGNs as satellites in massive halos.

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