Polarization constraints on the X-ray corona in Seyfert Galaxies: MCG-05-23-16

被引:41
作者
Marinucci, A. [1 ]
Muleri, F. [2 ]
Dovciak, M. [3 ]
Bianchi, S. [4 ]
Marin, F. [5 ]
Matt, G. [4 ]
Ursini, F. [4 ]
Middei, R. [6 ,7 ]
Marshall, H. L. [8 ]
Baldini, L. [9 ,10 ]
Barnouin, T. [5 ]
Rodriguez, N. Cavero [11 ,12 ]
De Rosa, A. [2 ]
Di Gesu, L. [1 ]
Harper, D. [11 ,12 ]
Ingram, A. [13 ]
Karas, V [3 ]
Krawczynski, H. [11 ,12 ]
Madejski, G. [14 ,15 ]
Panagiotou, C. [8 ]
Petrucci, P. O. [16 ]
Podgorny, J. [3 ,5 ,17 ]
Puccetti, S. [6 ]
Tombesi, F. [18 ,19 ,20 ]
Veledina, A. [21 ,22 ,23 ,24 ]
Zhang, W. [25 ]
Agudo, I [26 ]
Antonelli, L. A. [6 ,7 ]
Bachetti, M. [27 ]
Baumgartner, W. H. [28 ]
Bellazzini, R. [9 ]
Bongiorno, S. D. [28 ]
Bonino, R. [29 ,30 ]
Brez, A. [9 ]
Bucciantini, N. [31 ,32 ,33 ]
Capitanio, F. [2 ]
Castellano, S. [9 ]
Cavazzuti, E. [1 ]
Ciprini, S. [6 ,19 ]
Costa, E. [2 ]
Del Monte, E. [2 ]
Di Lalla, N. [14 ,15 ]
Di Marco, A. [2 ]
Donnarumma, I [1 ]
Doroshenko, V [24 ,34 ]
Ehlert, S. R. [28 ]
Enoto, T. [35 ]
Evangelista, Y. [2 ]
Fabiani, S. [2 ]
Ferrazzoli, R. [2 ]
机构
[1] ASI Agenzia Spaziale Italiana, Via Politecn Snc, I-00133 Rome, Italy
[2] INAF Ist Astrofis & Planetol Spaziali, Via Fosso Cavaliere 100, I-00133 Rome, Italy
[3] Czech Acad Sci, Astron Inst, Bocni II 1401-1, Prague 14100 4, Czech Republic
[4] Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy
[5] Univ Strasbourg, Observ Astron Strasbourg, CNRS, UMR 7550, F-67000 Strasbourg, France
[6] Agenzia Spaziale Italiana, Space Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy
[7] INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, RM, Italy
[8] MIT, MIT Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA
[9] Ist Nazl Fis Nucl, Sez Pisa, Largo B Pontecorvo 3, I-56127 Pisa, Italy
[10] Univ Pisa, Dipartimento Fis, Largo B Pontecorvo 3, I-56127 Pisa, Italy
[11] Washington Univ, Dept Phys, St Louis, MO 63130 USA
[12] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA
[13] Newcastle Univ, Sch Math Stat & Phys, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England
[14] Stanford Univ, Dept Phys, Stanford, CA 94305 USA
[15] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA
[16] Univ Grenoble Alpes, IPAG, CNRS, F-38000 Grenoble, France
[17] Charles Univ Prague, Astron Inst, V Holesovickach 2, CZ-18000 Prague, Czech Republic
[18] Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, I-00133 Rome, Italy
[19] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, Via Ric Sci 1, I-00133 Rome, Italy
[20] Univ Maryland, Dept Astron, College Pk, MD 20742 USA
[21] Univ Turku, Dept Phys & Astron, FI-20014 Turku, Finland
[22] KTH Royal Inst Technol, NORDITA, Hannes Alfvens Vag 12, SE-10691 Stockholm, Sweden
[23] Stockholm Univ, Hannes Alfvens Vag 12, SE-10691 Stockholm, Sweden
[24] Russian Acad Sci, Space Res Inst, Profsoyuznaya Str 84-32, Moscow 117997, Russia
[25] Chinese Acad Sci, Natl Astron Observ, 20A Datun Rd, Beijing 100101, Peoples R China
[26] CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, E-18008 Granada, Spain
[27] INAF Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy
[28] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA
[29] Ist Nazl Fis Nucl, Sez Torino, Via Pietro Giuria 1, I-10125 Turin, Italy
[30] Univ Torino, Dipartimento Fis, Via Pietro Giuria 1, I-10125 Turin, Italy
[31] INAF Osservatorio Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy
[32] Univ Firenze, Dipartimento Fis & Astron, Via Sansone 1, I-50019 Sesto Fiorentino, FI, Italy
[33] Ist Nazl Fis Nucl, Sez Firenze, Via Sansone 1, I-50019 Sesto Fiorentino, FI, Italy
[34] Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany
[35] RIKEN, Cluster Pioneering Res, 2-1 Hirosawa, Wako, Saitama 3510198, Japan
[36] CALTECH, Pasadena, CA 91125 USA
[37] Yamagata Univ, 1-4-12 Kojirakawa Machi, Yamagata 9908560, Japan
[38] Osaka Univ, 1-1 Yamadaoka, Suita, Osaka 5650871, Japan
[39] Univ British Columbia, Vancouver, BC V6T 1Z4, Canada
[40] Chuo Univ, Fac Sci & Engn, Dept Phys, Bunkyo Ku, 1-13-27 Kasuga, Tokyo 1128551, Japan
[41] Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA
[42] St Petersburg State Univ, Dept Astrophys, Univ Sky Pr 28, St Petersburg 198504, Russia
[43] Univ Turku, Finnish Ctr Astron ESO, Turku 20014, Finland
[44] Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan
[45] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, 1-3-1 Kagamiyama, Higashihiroshima, Hiroshima 7398526, Japan
[46] Univ Hong Kong, Dept Phys, Pokfulam, C694 RP Ma Liu Shui, Hong Kong, Peoples R China
[47] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA
[48] Ctr Astrophys Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02138 USA
[49] INAF Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, LC, Italy
[50] Univ Padua, Dipartimento Fis & Astron, Via Marzolo 8, I-35131 Padua, Italy
基金
美国国家航空航天局;
关键词
galaxies: active; galaxies: individual: MCG-05-23-16-polarization; galaxies: Seyfert; HOT ACCRETION FLOWS; ACTIVE GALACTIC NUCLEI; PHOTON IMAGING CAMERA; XMM-NEWTON; BEPPOSAX OBSERVATIONS; CYGNUS X-1; MODEL; EMISSION; SPECTRUM; COMPTONIZATION;
D O I
10.1093/mnras/stac2634
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We report on the first observation of a radio-quiet active galactic nucleus (AGN) in polarized X-rays: the Seyfert 1.9 galaxy MCG-05-23-16. This source was pointed at with the Imaging X-ray Polarimetry Explorer (IXPE) starting on 2022 May 14 for a net observing time of 486 ks, simultaneously with XMM-Newton (58 ks) and NuSTAR (83 ks). A polarization degree pi smaller than 4.7 per cent (at the 99 per cent confidence level) is derived in the 2-8 keV energy range, where emission is dominated by the primary component ascribed to the hot corona. The broad-band spectrum, inferred from a simultaneous fit to the IXPE, NuSTAR, and XMM-Newton data, is well reproduced by a power law with photon index Gamma = 1.85 +/- 0.01 and a high-energy cutoff E-C = 120 +/- 15 keV. A comparison with Monte Carlo simulations shows that a lamp-post and a conical geometry of the corona are consistent with the observed upper limit, a slab geometry is allowed only if the inclination angle of the system is less than 50 degrees.
引用
收藏
页码:5907 / 5913
页数:7
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