X-ray polarization measurement of the gold standard of radio-quiet active galactic nuclei: NGC 1068

被引：3

作者：

Marin, F. ^{[1
]}

Marinucci, A. ^{[2
]}

Laurenti, M. ^{[3
,4
,17
]}

Kim, D.E. ^{[3
,5
,6
]}

Barnouin, T. ^{[1
]}

Di Marco, A. ^{[5
]}

Ursini, F. ^{[7
]}

Bianchi, S. ^{[7
]}

Ravi, S. ^{[8
]}

Marshall, H.L. ^{[8
]}

Matt, G. ^{[7
]}

Chen, C.-T. ^{[9
]}

Gianolli, V.E. ^{[7
,10
]}

Ingram, A. ^{[11
]}

Middei, R. ^{[3
,17
]}

Maksym, W.P. ^{[12
]}

Panagiotou, C. ^{[8
]}

Podgorny, J. ^{[13
]}

Puccetti, S. ^{[4
]}

Ratheesh, A. ^{[5
]}

Tombesi, F. ^{[3
,14
,15
]}

Agudo, I. ^{[16
]}

Antonelli, L.A. ^{[4
,17
]}

Bachetti, M. ^{[18
]}

Baldini, L. ^{[19
,20
]}

Baumgartner, W. ^{[21
]}

Bellazzini, R. ^{[19
]}

Bongiorno, S. ^{[21
]}

Bonino, R. ^{[22
,23
]}

Brez, A. ^{[19
]}

Bucciantini, N. ^{[24
,25
,26
]}

Capitanio, F. ^{[5
]}

Castellano, S. ^{[19
]}

Cavazzuti, E. ^{[2
]}

Ciprini, S. ^{[4
,14
]}

Costa, E. ^{[5
]}

De Rosa, A. ^{[5
]}

Del Monte, E. ^{[5
]}

Di Gesu, L. ^{[2
]}

Di Lalla, N. ^{[27
]}

Donnarumma, I. ^{[2
]}

Doroshenko, V. ^{[28
]}

Dovčiak, M. ^{[13
]}

Ehlert, S. ^{[21
]}

Enoto, T. ^{[29
]}

Evangelista, Y. ^{[5
]}

Fabiani, S. ^{[5
]}

Ferrazzoli, R. ^{[5
]}

Garcia, J. ^{[30
]}

Gunji, S. ^{[31
]}

机构：

[1] Université de Strasbourg, CNRS, Observatoire Astronomique de Strasbourg, UMR 7550, Strasbourg,67000, France

[2] ASI - Agenzia Spaziale Italiana, Via del Politecnico snc, Roma,00133, Italy

[3] Dipartimento di Fisica, Università di Roma Tor Vergata, Via della Ricerca Scientifica 1, Roma,00133, Italy

[4] Space Science Data Center, SSDC, ASI, Via del Politecnico snc, Roma,00133, Italy

[5] INAF, Istituto di Astrofisica e Planetologia Spaziali, Via del Fosso del Cavaliere 100, Roma,00133, Italy

[6] Dipartimento di Fisica, Università degli Studi di Roma La Sapienza, Piazzale Aldo Moro 5, Roma,00185, Italy

[7] Dipartimento di Matematica e Fisica, Università degli Studi Roma Tre, via della Vasca Navale 84, Roma,00146, Italy

[8] MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge,MA,02139, United States

[9] Science and Technology Institute, Universities Space Research Association, Huntsville,AL,35805, United States

[10] Université Grenoble Alpes, CNRS, IPAG, Grenoble,38000, France

[11] School of Mathematics, Statistics, and Physics, Newcastle University, Newcastle upon Tyne,NE1 7RU, United Kingdom

[12] Center for Astrophysics, Harvard & Smithsonian, 60 Garden St., Cambridge,MA,02138, United States

[13] Astronomical Institute of the Czech Academy of Sciences, Boční II 1401/1, Praha 4,14100, Czech Republic

[14] Istituto Nazionale di Fisica Nucleare, Sezione di Roma Tor Vergata, Via della Ricerca Scientifica 1, Roma,00133, Italy

[15] Department of Astronomy, University of Maryland, College Park,MD,20742, United States

[16] Instituto de Astrofísica de Andalucía-CSIC, Glorieta de la Astronomía s/n, Granada,18008, Spain

[17] INAF Osservatorio Astronomico di Roma, Via Frascati 33, Monte Porzio Catone (RM),00078, Italy

[18] INAF Osservatorio Astronomico di Cagliari, Via della Scienza 5, Selargius (CA),09047, Italy

[19] Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, Largo B. Pontecorvo 3, Pisa,56127, Italy

[20] Dipartimento di Fisica, Università di Pisa, Largo B. Pontecorvo 3, Pisa,56127, Italy

[21] NASA Marshall Space Flight Center, Huntsville,AL,35812, United States

[22] Istituto Nazionale di Fisica Nucleare, Sezione di Torino, Via Pietro Giuria 1, Torino,10125, Italy

[23] Dipartimento di Fisica, Università degli Studi di Torino, Via Pietro Giuria 1, Torino,10125, Italy

[24] INAF, Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, Firenze,50125, Italy

[25] Dipartimento di Fisica e Astronomia, Università degli Studi di Firenze, Via Sansone 1, Sesto Fiorentino (FI),50019, Italy

[26] Istituto Nazionale di Fisica Nucleare, Sezione di Firenze, Via Sansone 1, Sesto Fiorentino (FI),50019, Italy

[27] Department of Physics, Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford,CA,94305, United States

[28] Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, Tübingen,72076, Germany

[29] RIKEN Cluster for Pioneering Research, 2-1 Hirosawa, Wako, Saitama,351-0198, Japan

[30] California Institute of Technology, Pasadena,CA,91125, United States

[31] Yamagata University, 1-4-12 Kojirakawamachi, Yamagatashi,990-8560, Japan

[32] University of British Columbia, Vancouver,BC,V6T 1Z4, Canada

[33] International Center for Hadron Astrophysics, Chiba University, Chiba,263-8522, Japan

[34] Institute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston,MA,02215, United States

[35] Department of Astrophysics, St. Petersburg State University, Universitetsky pr. 28, Petrodvoretz, St. Petersburg,198504, Russia

[36] Department of Physics and Astronomy and Space Science Center, University of New Hampshire, Durham,NH,03824, United States

[37] Physics Department, McDonnell Center for the Space Sciences, Washington University in St. Louis, St. Louis,MO,63130, United States

[38] Finnish Centre for Astronomy, ESO, University of Turku, 20014, Finland

[39] Guangxi Key Laboratory for Relativistic Astrophysics, School of Physical Science and Technology, Guangxi University, Nanning,530004, China

[40] Graduate School of Science, Division of Particle and Astrophysical Science, Nagoya University, Furocho, Chikusaku, Aichi, Nagoya,464-8602, Japan

[41] Hiroshima Astrophysical Science Center, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima,739-8526, Japan

[42] University of Maryland, Baltimore County, Baltimore,MD,21250, United States

[43] NASA Goddard Space Flight Center, Greenbelt,MD,20771, United States

[44] Center for Research and Exploration in Space Science and Technology, NASA, GSFC, Greenbelt,MD,20771, United States

[45] Department of Physics, The University of Hong Kong, Pokfulam, Hong Kong

[46] Department of Astronomy and Astrophysics, Pennsylvania State University, University Park,PA,16802, United States

[47] Department of Physics and Astronomy, University of Turku, 20014, Finland

[48] INAF, Osservatorio Astronomico di Brera, Via E. Bianchi 46, (LC), Merate,23807, Italy

[49] Dipartimento di Fisica e Astronomia, Università degli Studi di Padova, Via Marzolo 8, Padova,35131, Italy

[50] Anton Pannekoek Institute for Astronomy & GRAPPA, University of Amsterdam, Science Park 904, Amsterdam,1098 XH, Netherlands

来源：

Astronomy and Astrophysics | 2024年 / 689卷

基金：

美国国家航空航天局;

关键词：

Active Galactic Nuclei - Direct sequence systems - Ellipsometry - Light polarization - Linear accelerators - Luminescence - Photons - White dwarfs - Wigglers - X ray apparatus - X ray radiography;

D O I：

10.1051/0004-6361/202449760

中图分类号：

学科分类号：

摘要：

Context. NGC 1068 is the most observed radio-quiet active galactic nucleus (AGN) in polarimetry, yet its high-energy polarization has never been probed before due to a lack of dedicated polarimeters. Aims. Using the first X-ray polarimeter sensitive enough to measure the polarization of AGNs, we want to probe the orientation and geometric arrangement of (sub)parsec-scale matter around the X-ray source. Methods. We used the Imaging X-ray Polarimetry Explorer (IXPE) satellite to measure, for the first time, the 2- 8 keV polarization of NGC 1068. We pointed IXPE at the target for a net exposure time of 1.15 Ms, in addition to using two Chandra snapshots of ∼10 ks each in order to account for the potential impact of several ultraluminous X-ray sources (ULXs) within IXPE's field of view. Results. We measured a 2- 8 keV polarization degree of 12.4% ± 3.6% and an electric vector polarization angle of 101 ± 8 at a 68% confidence level. If we exclude the spectral region containing bright Fe K lines and other soft X-ray lines where depolarization occurs, the polarization fraction rises to 21.3% ± 6.7% in the 3.5- 6.0 keV band, with a similar polarization angle. The observed polarization angle is found to be perpendicular to the parsec-scale radio jet. Using a combined Chandra and IXPE analysis plus multiwavelength constraints, we estimated that the circumnuclear torusmay sustain a half-opening angle of 50- 55 (from the vertical axis of the system). Conclusions. Thanks to IXPE, we have measured the X-ray polarization of NGC 1068 and found comparable results, both in terms of the polarization angle orientation with respect to the radio jet and the torus half-opening angle, to the X-ray polarimetric measurement achieved for the other archetypal Compton-thick AGN: the Circinus galaxy. Probing the geometric arrangement of parsec-scale matter in extragalactic objects is now feasible thanks to X-ray polarimetry. © 2024 The Authors.

引用

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