The existence of a large population of Compton thick (CT; N-H > 10(24) cm(-2) ) active galactic nuclei (AGN) is a key ingredient of most cosmic X-ray background synthesis models. However, direct identification of these sources, especially at high redshift, is difficult due to flux suppression and complex spectral shape produced by CT obscuration. We explored the Chandra Cosmological Evolution Survey (COSMOS) Legacy point source catalogue, comprising 1855 sources to select, via X-ray spectroscopy, a large sample of CT candidates at high redshift. Adopting a physical model to reproduce the toroidal absorber and a Monte-Carlo sampling method, we selected 67 individual sources with >5 per cent probability of being CT, in the redshift range 0.04 less than or similar to z less than or similar to 3.5. The sum of the probabilities above N-H > 10(24) cm(-2) gives a total of 41.9 effective CT, corrected for classification bias. We derive number counts in the 2-10 keV band in three redshift bins. The observed log N-log S is consistent with an increase of the intrinsic CT fraction (f(CT)) from similar to 0.30 to similar to 0.55 from low to high redshift. When resealed to a common luminosity (log(L-X/ erg s(-1)) = 44.5), we find an increase from f(CT) = 0.191(-0.06)(+0.07) to 0.30(-0.08)(+0.10) and f(CT )= 0.49(-0.11)(+0.12) from low to high z. This evolution can be parametrized as f(CT) = 0.11(-0.04)(+0.05)(1 + z)(1.11 +/- 0.13). T hanks to Hubble Space Mlescope-Advanced Camera for Surveys deep imaging, we find that the fraction of CT AGN in mergers/interacting systems increases with luminosity and redshift and is significantly higher than for non-CT AGN hosts.

Lanzuisi G., C.F. (2018). The Chandra COSMOS Legacy Survey: Compton thick AGN at high redshift. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 480(2), 2578-2592 [10.1093/mnras/sty2025].

The Chandra COSMOS Legacy Survey: Compton thick AGN at high redshift

Lanzuisi G.
Writing – Original Draft Preparation
;
Marchesi S.;Brusa M.
Membro del Collaboration Group
;
Vignali C.
Membro del Collaboration Group
;
2018

Abstract

The existence of a large population of Compton thick (CT; N-H > 10(24) cm(-2) ) active galactic nuclei (AGN) is a key ingredient of most cosmic X-ray background synthesis models. However, direct identification of these sources, especially at high redshift, is difficult due to flux suppression and complex spectral shape produced by CT obscuration. We explored the Chandra Cosmological Evolution Survey (COSMOS) Legacy point source catalogue, comprising 1855 sources to select, via X-ray spectroscopy, a large sample of CT candidates at high redshift. Adopting a physical model to reproduce the toroidal absorber and a Monte-Carlo sampling method, we selected 67 individual sources with >5 per cent probability of being CT, in the redshift range 0.04 less than or similar to z less than or similar to 3.5. The sum of the probabilities above N-H > 10(24) cm(-2) gives a total of 41.9 effective CT, corrected for classification bias. We derive number counts in the 2-10 keV band in three redshift bins. The observed log N-log S is consistent with an increase of the intrinsic CT fraction (f(CT)) from similar to 0.30 to similar to 0.55 from low to high redshift. When resealed to a common luminosity (log(L-X/ erg s(-1)) = 44.5), we find an increase from f(CT) = 0.191(-0.06)(+0.07) to 0.30(-0.08)(+0.10) and f(CT )= 0.49(-0.11)(+0.12) from low to high z. This evolution can be parametrized as f(CT) = 0.11(-0.04)(+0.05)(1 + z)(1.11 +/- 0.13). T hanks to Hubble Space Mlescope-Advanced Camera for Surveys deep imaging, we find that the fraction of CT AGN in mergers/interacting systems increases with luminosity and redshift and is significantly higher than for non-CT AGN hosts.
2018
Lanzuisi G., C.F. (2018). The Chandra COSMOS Legacy Survey: Compton thick AGN at high redshift. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 480(2), 2578-2592 [10.1093/mnras/sty2025].
Lanzuisi G., Civano F., Marchesi S., Comastri A., Brusa M., Gilli R., Vignali C., Zamorani G., Brightman M., Griffiths R. E., Koekemoer A. M....espandi
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