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Revisiting the relationship between 6 μm and 2-10 keV continuum luminosities of AGN

AutorMateos, Silvia ; Carrera, Francisco J. ; Alonso-Herrero, A. ; Rovilos, E.; Hernán-Caballero, Antonio ; Barcons, Xavier ; Blain, A.; Caccianiga, A.; Della Ceca, R.; Severgnini, P.
Palabras claveX-rays: galaxies
Infrared: galaxies
Quasars: supermassive black holes
Galaxies: active
Fecha de publicación2015
EditorOxford University Press
CitaciónMonthly Notices of the Royal Astronomical Society 449(2): 1422-1440 (2015)
ResumenWe have determined the relation between the AGN luminosities at rest-frame 6 μm associated with the dusty torus emission and at 2–10 keV energies using a complete, X-ray-flux-limited sample of 232 AGN drawn from the Bright Ultra-hard XMM-Newton Survey. The objects have intrinsic X-ray luminosities between 1042 and 1046 erg s−1 and redshifts from 0.05 to 2.8. The rest-frame 6 μm luminosities were computed using data from the Wide-field Infrared Survey Explorer and are based on a spectral energy distribution decomposition into AGN and galaxy emission. The best-fitting relationship for the full sample is consistent with being linear, L6 μm ∝ L0.99±0.032−10keVL2−10keV0.99±0.03, with intrinsic scatter, Δ log L6 μm ∼ 0.35 dex. The L6μm/L2−10keVL6μm/L2−10keV luminosity ratio is largely independent of the line-of-sight X-ray absorption. Assuming a constant X-ray bolometric correction, the fraction of AGN bolometric luminosity reprocessed in the mid-IR decreases weakly, if at all, with the AGN luminosity, a finding at odds with simple receding torus models. Type 2 AGN have redder mid-IR continua at rest-frame wavelengths <12 μm and are overall ∼1.3–2 times fainter at 6 μm than type 1 AGN at a given X-ray luminosity. Regardless of whether type 1 and type 2 AGN have the same or different nuclear dusty toroidal structures, our results imply that the AGN emission at rest-frame 6 μm is not isotropic due to self-absorption in the dusty torus, as predicted by AGN torus models. Thus, AGN surveys at rest-frame ∼6 μm are subject to modest dust obscuration biases.
Versión del editorhttps://doi.org/10.1093/mnras/stv299
Identificadoresdoi: 10.1093/mnras/stv299
issn: 0035-8711
e-issn: 1365-2966
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