Tombesi, FrancescoFrancescoTombesiMushotzky, R. F.R. F.MushotzkyReynolds, C. S.C. S.ReynoldsKallman, T.T.KallmanReeves, J. N.J. N.ReevesBRAITO, ValentinaValentinaBRAITOUeda, Y.Y.UedaLeutenegger, M. A.M. A.LeuteneggerWilliams, B. J.B. J.WilliamsStawarz, Ł.Ł.StawarzCAPPI, MASSIMOMASSIMOCAPPI2021-01-272021-01-2720170004-637Xhttp://hdl.handle.net/20.500.12386/30027We present a spectral analysis of a 200 ks observation of the broad-line radio galaxy 3C 120, performed with the high-energy transmission grating spectrometer on board the Chandra X-ray Observatory. We find (I) a neutral absorption component intrinsic to the source with a column density of {log}{N}<SUB>{{H</SUB>}}=20.67+/- 0.05 cm<SUP>-2</SUP> (II) no evidence for a warm absorber (WA) with an upper limit on the column density of just {log}{N}<SUB>{{H</SUB>}}< 19.7 cm<SUP>-2</SUP>, assuming the typical ionization parameter logξ ≃ 2.5 erg s<SUP>-1</SUP> cm the WA may instead be replaced by (III) a hot emitting gas with a temperature kT ≃ 0.7 keV observed as soft X-ray emission from ionized Fe L-shell lines, which may originate from a kiloparsec-scale shocked bubble inflated by the active galactic nucleus (AGN) wind or jet with a shock velocity of about 1000 km s<SUP>-1</SUP> determined by the emission line width; (IV) a neutral Fe Kα line and accompanying emission lines indicative of a Compton-thick cold reflector with a low reflection fraction R ≃ 0.2, suggesting a large opening angle of the torus; (v) a highly ionized Fe xxv emission feature indicative of photoionized gas with an ionization parameter logξ ={3.75}<SUB>-0.38</SUB><SUP>+0.27</SUP> erg s<SUP>-1</SUP> cm and a column density of {log}{N}<SUB>{{H</SUB>}}> 22 cm<SUP>-2</SUP> localized within ∼2 pc from the X-ray source; and (VI) possible signatures of a highly ionized disk wind. Together with previous evidence for intense molecular line emission, these results indicate that 3C 120 is likely a late-state merger undergoing strong AGN feedback.STAMPAenArticle10.3847/1538-4357/aa63422-s2.0-85016768751000398672800002https://iopscience.iop.org/article/10.3847/1538-4357/aa63422017ApJ...838...16TFIS/04 - FISICA NUCLEARE E SUBNUCLEARE