{"paper":{"title":"The XMM deep survey in the CDF-S. IX. An X-ray outflow in a luminous obscured quasar at z~1.6","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.GA","authors_text":"1), (10) Department of Astronomy & Astrophysics, 11, (11) Institute for Gravitation, 12), (12) Department of Physics, (13) Instituto de Astrofisica, 14, (14) Millennium Institute of Astrophysics, 15), (15) Space Science Institute, (16) INAF-Osservatorio Astronomico di Roma, (17) Department of Astronomy, 18) ((1) Dipartimento di Fisica e Astronomia, (18) NASA Goddard Space Flight Center, 2), (2) INAF-Osservatorio Astronomico di Bologna, (3) ICREA, (4) Institute for Astronomy & Astrophysics, (5) ESO, 6), (6) Excellence Cluster Universe, (7) Instituto de Fisica de Cantabria, (8) Sterrenkundig Observatorium, 9), (9) Instituto de Radioastronomia y Astrofisica, A. Comastri (2), Bologna, Boulder, Colorado, C. Vignali (1, F.E. Bauer (13, F. Fiore (16), F.J. Carrera (7), F. Tombesi (17, Garching, G. Lanzuisi (2, Greenbelt, ICC, I. Georgantopoulos (4), J. Fritz (8, K. Iwasawa (3), M. Brusa (1, MD, MontePorzio, National Observatory of Athens, N. Cappelluti (2), Pontificia Universidad Catolica de Chile, P. Ranalli (4), Providencia, R. Gilli (2), Roma, Santander, Santiago de Chile, the Cosmos, The Pennsylvania State University, UNAM, Universitat de Barcelona, Universiteit Gent, University of Maryland, USA), V. Mainieri (5, W.N. Brandt (10","submitted_at":"2015-09-17T20:15:23Z","abstract_excerpt":"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 (Nh~2x10^{23} cm^-2), intrinsically"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1509.05413","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}