| dc.creator | Manolis Plionis | |
| dc.date | 2013-01-11 | |
| dc.date.accessioned | 2023-07-25T16:25:14Z | |
| dc.date.available | 2023-07-25T16:25:14Z | |
| dc.identifier | http://inaoe.repositorioinstitucional.mx/jspui/handle/1009/2240 | |
| dc.identifier.uri | https://repositorioslatinoamericanos.uchile.cl/handle/2250/7807421 | |
| dc.description | We present the spatial clustering properties of 1466 X-ray selected AGN compiled from the Chandra CDF-N, CDF-S, eCDF-S, COSMOS and AEGIS fields in the 0.5−8 keV band. The X-ray sources span the redshift interval 0 < z < 3 and have a median value of ž = 0.976. We employ the projected two-point correlation function to infer the spatial clustering and find a clustering length of r₀ = 7.2 ± 0.6h⁻¹ Mpc and a slope of γ = 1.48 ± 0.12, which corresponds to a bias of b(ž) = 2.26±0.16. Using two different halo bias models, we consistently estimate an average dark-matter host halo mass of Mh ⋍ 1.3(±0.3) × 10¹³ h⁻¹M⨀. The Xray AGN bias and the corresponding dark-matter host halo mass, are significantly higher than the corresponding values of optically selected AGN (at the same redshifts). The redshift evolution of the X-ray selected AGN bias indicates, in agreement with other recent studies, that a unique dark-matter halo mass does not fit well the bias at all the different redshifts probed. Furthermore, we investigate if there is a dependence of the clustering strength on X-ray luminosity. To this end we consider only 650 sources around z ~ 1 and we apply a procedure to disentangle the dependence of clustering on redshift. We find indications for a positive dependence of the clustering length on X-ray luminosity, in the sense that the more luminous sources have a larger clustering length and hence a higher dark-matter halo mass. In detail we find for an average luminosity difference of δ log₁₀ Lx ⋍ 1 a halo mass difference of a factor of ~3. These findings appear to be consistent with a galaxy-formation model where the gas accreted onto the supermassive black hole in intermediate luminosity AGN comes mostly from the hot-halo atmosphere around the host galaxy. | |
| dc.format | application/pdf | |
| dc.language | eng | |
| dc.publisher | Monthly Notices of the Royal Astronomical Society | |
| dc.relation | citation:Koutoulidis, L., et al., (2013), Clustering, Bias and the Accretion Mode of X-ray selected AGN, Monthly Notices of the Royal Astronomical Society, Vol. 428(2):1382-1394 | |
| dc.rights | info:eu-repo/semantics/openAccess | |
| dc.rights | http://creativecommons.org/licenses/by-nc-nd/4.0 | |
| dc.subject | info:eu-repo/classification/Inspec/Galaxies: active : clustering | |
| dc.subject | info:eu-repo/classification/Inspec/X-rays: galaxies | |
| dc.subject | info:eu-repo/classification/cti/1 | |
| dc.subject | info:eu-repo/classification/cti/21 | |
| dc.subject | info:eu-repo/classification/cti/21 | |
| dc.title | Clustering, Bias and the Accretion Mode of X-ray selected AGN | |
| dc.type | info:eu-repo/semantics/article | |
| dc.type | info:eu-repo/semantics/acceptedVersion | |
| dc.audience | students | |
| dc.audience | researchers | |
| dc.audience | generalPublic | |
