Universal bolometric corrections for active galactic nuclei over seven luminosity decades

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dc.contributor.authorDuras, F.
dc.contributor.authorBongiorno, A.
dc.contributor.authorRicci, F.
dc.contributor.authorPiconcelli, E.
dc.contributor.authorShankar, F.
dc.contributor.authorLusso, E.
dc.contributor.authorBianchi, S.
dc.contributor.authorFiore, F.
dc.contributor.authorMaiolino, R.
dc.contributor.authorMarconi, A.
dc.contributor.authorOnori, F.
dc.contributor.authorSani, E.
dc.contributor.authorSchneider, R.
dc.contributor.authorVignali, C.
dc.contributor.authorLa Franca, F.
dc.date.accessioned2025-01-23T19:51:58Z
dc.date.available2025-01-23T19:51:58Z
dc.date.issued2020
dc.description.abstractContext. The AGN bolometric correction is a key element for understanding black hole (BH) demographics and computing accurate BH accretion histories from AGN luminosities. However, current estimates still differ from each other by up to a factor of two to three, and rely on extrapolations at the lowest and highest luminosities.
dc.description.abstractAims. Here we revisit this fundamental question by presenting general hard X-ray (K-X) and optical (K-O) bolometric corrections, computed by combining several AGN samples spanning the widest (about 7 dex) luminosity range ever used for this type of studies.
dc.description.abstractMethods. We analysed a total of similar to 1000 type 1 and type 2 AGN for which we performed a dedicated SED-fitting.
dc.description.abstractResults. We provide a bolometric correction separately for type 1 and type 2 AGN; the two bolometric corrections agree in the overlapping luminosity range. Based on this we computed for the first time a universal bolometric correction for the whole AGN sample (both type 1 and type 2). We found that K-X is fairly constant at log(L-BOL/L-circle dot) < 11, while it increases up to about one order of magnitude at log(L-BOL/L-circle dot) similar to 14.5. A similar increasing trend has been observed when its dependence on either the Eddington ratio or the BH mass is considered, while no dependence on redshift up to z & x2004;similar to & x2004;3.5 has been found. In contrast, the optical bolometric correction appears to be fairly constant (i.e. K-O & x2004;similar to & x2004;5) regardless of the independent variable. We also verified that our bolometric corrections correctly predict the AGN bolometric luminosity functions. According to this analysis, our bolometric corrections can be applied to the whole AGN population in a wide range of luminosity and redshift.
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361/201936817
dc.identifier.eissn1432-0746
dc.identifier.issn0004-6361
dc.identifier.urihttps://doi.org/10.1051/0004-6361/201936817
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/100610
dc.identifier.wosidWOS:000530110700005
dc.language.isoen
dc.revistaAstronomy & astrophysics
dc.rightsacceso restringido
dc.subjectblack hole physics
dc.subjectgalaxies
dc.subjectactive
dc.subjectquasars
dc.subjectsupermassive black holes
dc.subjectgalaxies
dc.subjectevolution
dc.subjectgalaxies
dc.subjectfundamental parameters
dc.subjectX-rays
dc.subjectgalaxies
dc.titleUniversal bolometric corrections for active galactic nuclei over seven luminosity decades
dc.typeartículo
dc.volumen636
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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