The Chandra COSMOS Legacy Survey: Clustering of X-ray selected AGN at 2.9<z<5.5 using photometric redshift Probability Distribution Functions

Abstract

We present the measurement of the projected and redshift space 2-point correlation function (2pcf) of the new catalog of Chandra COSMOS-Legacy AGN at 2.9$\le$z$\le$5.5 ($⟨L_{bol}⟩\sim$10${}^{46}$ erg/s) using the generalized clustering estimator based on phot-z probability distribution functions (Pdfs) in addition to any available spec-z. We model the projected 2pcf estimated using ${\pi }_{max}$ = 200 h${}^{-1}$ Mpc with the 2-halo term and we derive a bias at z$\sim$3.4 equal to b = 6.6${}_{-0.55}^{+0.60}$, which corresponds to a typical mass of the hosting halos of log M${}_h$ = 12.83${}_{-0.11}^{+0.12}$ h${}^{-1}$ M${}_{\odot }$. A similar bias is derived using the redshift-space 2pcf, modelled including the typical phot-z error ${\sigma }_z$ = 0.052 of our sample at z$\ge$2.9. Once we integrate the projected 2pcf up to ${\pi }_{max}$ = 200 h${}^{-1}$ Mpc, the bias of XMM and \textit{Chandra} COSMOS at z=2.8 used in Allevato et al. (2014) is consistent with our results at higher redshift. The results suggest only a slight increase of the bias factor of COSMOS AGN at z$\gtrsim$3 with the typical hosting halo mass of moderate luminosity AGN almost constant with redshift and equal to logM${}_h$ = 12.92${}_{-0.18}^{+0.13}$ at z=2.8 and log M${}_h$ = 12.83${}_{-0.11}^{+0.12}$ at z$\sim$3.4, respectively. The observed redshift evolution of the bias of COSMOS AGN implies that moderate luminosity AGN still inhabit group-sized halos at z$\gtrsim$3, but slightly less massive than observed in different independent studies using X-ray AGN at z$\le 2$.

Accepted for publication in The Astrophysical Journal

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• The clustering and bias of radio-selected AGN and star-forming galaxies in the COSMOS field
• Type 2 AGN host galaxies in the Chandra-COSMOS Legacy Survey: No Evidence of AGN-driven Quenching
• Spatial clustering and halo occupation distribution modeling of local AGN via cross-correlation measurements with 2MASS galaxies
• Imprints of the super-Eddington accretion on the quasar clustering