Por favor, use este identificador para citar o enlazar este ítem:
http://inaoe.repositorioinstitucional.mx/jspui/handle/1009/2240| Clustering, Bias and the Accretion Mode of X-ray selected AGN | |
| Manolis Plionis | |
| Acceso Abierto | |
| Atribución-NoComercial-SinDerivadas | |
| Galaxies: active : clustering X-rays: galaxies | |
| 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. | |
| Monthly Notices of the Royal Astronomical Society | |
| 11-01-2013 | |
| Artículo | |
| Inglés | |
| Estudiantes Investigadores Público en general | |
| 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 | |
| ASTRONOMÍA Y ASTROFÍSICA | |
| Versión aceptada | |
| acceptedVersion - Versión aceptada | |
| Aparece en las colecciones: | Artículos de Astrofísica |
Cargar archivos:
| Fichero | Tamaño | Formato | |
|---|---|---|---|
| 22. Clustering, bias and the accretion mode of X-ray-selected AGN.pdf | 475.24 kB | Adobe PDF | Visualizar/Abrir |