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|Title:||The XMM deep survey in the CDF-S. IX. An X-ray outflow in a luminous obscured quasar at z ≈ 1.6||Authors:||Vignali, C.
Carrera, F. J.
Brandt, W. N.
Bauer, F. E.
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||583||First Page:||A141||Abstract:||In active galactic nuclei (AGN)-galaxy co-evolution models, AGN winds and outflows are often invoked to explain why super-massive black holes and galaxies stop growing efficiently at a certain phase of their lives. They are commonly referred to as the leading actors of feedback processes. Evidence of ultra-fast (v ≳ 0.05c) outflows in the innermost regions of AGN has been collected in the past decade by sensitive X-ray observations for sizable samples of AGN, mostly at low redshift. Here we present ultra-deep XMM-Newton and Chandra spectral data of an obscured (N<SUB>H</SUB>≈ 2 × 10<SUP>23</SUP> cm<SUP>-2</SUP>), intrinsically luminous (L<SUB>2-10 keV</SUB>≈ 4 × 10<SUP>44</SUP> erg s<SUP>-1</SUP>) quasar (named PID352) at z ≈ 1.6 (derived from the X-ray spectral analysis) in the Chandra Deep Field-South. The source is characterized by an iron emission and absorption line complex at observed energies of E ≈ 2-3 keV. While the emission line is interpreted as being due to neutral iron (consistent with the presence of cold absorption), the absorption feature is due to highly ionized iron transitions (FeXXV, FeXXVI) with an outflowing velocity of , as derived from photoionization models. The mass outflow rate - ~2 M<SUB>☉</SUB> yr<SUP>-1</SUP> - is similar to the source accretion rate, and the derived mechanical energy rate is ~9.5 × 10<SUP>44</SUP> erg s<SUP>-1</SUP>, corresponding to 9% of the source bolometric luminosity. PID352 represents one of the few cases where indications of X-ray outflowing gas have been observed at high redshift thus far. This wind is powerful enough to provide feedback on the host galaxy.||Acknowledgments:||The authors thank the referee for detailed and thoughtful comments and suggestions. Financial contribution from “PRIN–INAF 2011” and “PRIN–INAF 2012” is acknowledged. K.I. acknowledges support by the Spanish MINECO under grant AYA2013-47447-C3-2-P and MDM-2014-0369 of ICCUB (Unidad de Excelencia “María de Maeztu”). G.L. and M.B. acknowledge support from the FP7 Career Integration Grant “eEASy” (“SMBH evolution through cosmic time: from current surveys to eROSITA-Euclid AGN Synergies”, CIG 321913). F.J.C. acknowledges Financial support from the Spanish Ministerio de Economía y Competitividad under project AYA2012-31447. W.N.B. thanks support from Chandra X-ray Center grant G04-15130A and NASA ADP grant NNX10AC99G. F.E.B. acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, “EMBIGGEN” Anillo ACT1101) and the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. C.V. thanks P. Ciliegi, D. Dallacasa and E. Middelberg for information on radio data, and M. Cappi, G. Chartas, A. Feltre, P. Grandi, E. Lusso, G. Ponti, L. Pozzetti, E. Rovilos, P. Severgnini, F. Vito, and G. Zamorani for useful discussions.||URI:||http://hdl.handle.net/20.500.12386/23686||URL:||https://www.aanda.org/articles/aa/abs/2015/11/aa25852-15/aa25852-15.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201525852||Bibcode ADS:||2015A&A...583A.141V||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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