X-ray emission of <i>z</i> > 2.5 active galactic nuclei can be obscured by their host galaxies

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dc.contributor.authorCircosta, C.
dc.contributor.authorVignali, C.
dc.contributor.authorGilli, R.
dc.contributor.authorFeltre, A.
dc.contributor.authorVito, F.
dc.contributor.authorCalura, F.
dc.contributor.authorMainieri, V
dc.contributor.authorMassardi, M.
dc.contributor.authorNorman, C.
dc.date.accessioned2025-01-23T21:16:56Z
dc.date.available2025-01-23T21:16:56Z
dc.date.issued2019
dc.description.abstractWe present a multiwavelength study of seven active galactic nuclei (AGN) at spectroscopic redshift >2.5 in the 7 Ms Chandra Deep Field South that were selected for their good far-infrared (FIR) and submillimeter (submm) detections. Our aim is to investigate the possibility that the obscuration observed in the X-rays can be produced by the interstellar medium (ISM) of the host galaxy. Based on the 7 Ms Chandra spectra, we measured obscuring column densities N-H,N- X in excess of 7 x 10(22) cm(-2) and intrinsic X-ray luminosities L-X > 10(44) erg s(-1) for our targets, as well as equivalent widths for the Fe K alpha emission line EWrest greater than or similar to 0.5-1 keV. We built the UV-to-FIR spectral energy distributions (SEDs) by using broadband photometry from the CANDELS and Herschel catalogs. By means of an SED decomposition technique, we derived stellar masses (M-* similar to 10(11) M-circle dot), IR luminosities (L-IR > 10(12) L-circle dot), star formation rates (SFR similar to 190-1680 M-circle dot yr(-1)) and AGN bolometric luminosities (L-bol similar to 10(46) erg s(-1)) for our sample. We used an empirically calibrated relation between gas masses and FIR/submm luminosities and derived M-gas similar to 0.8-5.4 x 10(10) M-circle dot. High-resolution (0.3-0.7 '') ALMA data (when available, CANDELS data otherwise) were used to estimate the galaxy size and hence the volume enclosing most of the ISM under simple geometrical assumptions. These measurements were then combined to derive the column density associated with the ISM of the host, which is on the order of N-H,N- ISM similar to 10(23-24) cm(-2). The comparison between the ISM column densities and those measured from the X-ray spectral analysis shows that they are similar. This suggests that at least at high redshift, significant absorption on kiloparsec scales by the dense ISM in the host likely adds to or substitutes that produced by circumnuclear gas on parsec scales (i.e., the torus of unified models). The lack of unobscured AGN among our ISM-rich targets supports this scenario.
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361/201834426
dc.identifier.issn1432-0746
dc.identifier.urihttps://doi.org/10.1051/0004-6361/201834426
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/101138
dc.identifier.wosidWOS:000462556100001
dc.language.isoen
dc.revistaAstronomy & astrophysics
dc.rightsacceso restringido
dc.subjectgalaxies: active
dc.subjectgalaxies: evolution
dc.subjectgalaxies: star formation
dc.subjectquasars: general
dc.subjectsurveys
dc.subjectX-rays: galaxies
dc.titleX-ray emission of <i>z</i> > 2.5 active galactic nuclei can be obscured by their host galaxies
dc.typeartículo
dc.volumen623
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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