Uncovering the geometry of the hot X-ray corona in the Seyfert galaxy NGC 4151 with IXPE

被引：40

作者：

Gianolli, V. E. ^{[1
,2
]}

Kim, D. E. ^{[3
,4
,5
]}

Bianchi, S. ^{[2
]}

Agis-Gonzalez, B. ^{[6
]}

Madejski, G. ^{[7
,8
]}

Marin, F. ^{[9
]}

Marinucci, A. ^{[10
]}

Matt, G. ^{[2
]}

Middei, R. ^{[3
,11
]}

Petrucci, P. O. ^{[1
]}

Soffitta, P. ^{[3
]}

Tagliacozzo, D. ^{[2
]}

Tombesi, F. ^{[12
,13
]}

Ursini, F. ^{[2
]}

Barnouin, T. ^{[9
]}

De Rosa, A. ^{[3
]}

Di Gesu, L. ^{[10
]}

Ingram, A. ^{[14
]}

Loktev, V. ^{[15
]}

Panagiotou, C. ^{[16
]}

Podgorny, J. ^{[9
,17
,18
]}

Poutanen, J. ^{[15
]}

Puccetti, S. ^{[11
]}

Ratheesh, A. ^{[3
]}

Veledina, A. ^{[15
,19
,20
]}

Zhang, W. ^{[21
]}

Agudo, I. ^{[6
]}

Antonelli, L. A. ^{[11
,22
]}

Bachetti, M. ^{[23
]}

Baldini, L. ^{[24
,25
]}

Baumgartner, W. H. ^{[26
]}

Bellazzini, R. ^{[24
]}

Bongiorno, S. D. ^{[26
]}

Bonino, R. ^{[27
,28
]}

Brez, A. ^{[24
]}

Bucciantini, N. ^{[29
,30
,31
]}

Capitanio, F. ^{[3
]}

Castellano, S. ^{[24
]}

Cavazzuti, E. ^{[10
]}

Chen, C. T. ^{[32
]}

Ciprini, S. ^{[11
,12
]}

Costa, E. ^{[3
]}

Del Monte, E. ^{[3
]}

Di Lalla, N. ^{[7
,8
]}

Di Marco, A. ^{[3
]}

Donnarumma, I. ^{[10
]}

Doroshenko, V. ^{[33
]}

Dovciak, M. ^{[17
]}

Ehlert, S. R. ^{[26
]}

Enoto, T. ^{[34
]}

机构：

[1] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France

[2] Univ Rome Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy

[3] INAF Ist Astrofis & Planetol Spaziali, Via Fosso Cavaliere 100, I-00133 Rome, Italy

[4] Univ Roma La Sapienza, Dipartimento Fis, Piazzale Aldo Moro 5, I-00185 Rome, Italy

[5] Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, I-00133 Rome, Italy

[6] CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, E-18008 Granada, Spain

[7] Stanford Univ, Dept Phys, Stanford, CA 94305 USA

[8] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA

[9] Univ Strasbourg, CNRS, Observ Astron Strasbourg, UMR 7550, F-67000 Strasbourg, France

[10] ASI Agenzia Spaziale Italiana, Via Politecn Snc, I-00133 Rome, Italy

[11] Agenzia Spaziale Italiana, Space Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy

[12] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, Via Ric Sci 1, I-00133 Rome, Italy

[13] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[14] Newcastle Univ, Sch Math Stat & Phys, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England

[15] Univ Turku, Dept Phys & Astron, FI-20014 Turku, Finland

[16] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[17] Czech Acad Sci, Astron Inst, Bocni II 1401-1, CZ-141004 Prague 4, Czech Republic

[18] Charles Univ Prague, Astron Inst, V Holesovickach 2, CZ-18000 Prague, Czech Republic

[19] KTH Royal Inst Technol, Nordita, Hannes Alfvens vag 12, SE-10691 Stockholm, Sweden

[20] Stockholm Univ, Hannes Alfvens vag 12, SE-10691 Stockholm, Sweden

[21] Chinese Acad Sci, Natl Astron Observ, 20A Datun Rd, Beijing 100101, Peoples R China

[22] INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy

[23] INAF Osservatorio Astron Cagliari, Via Scienza 5, I-09047 Selargius, CA, Italy

[24] Ist Nazl Fis Nucl, Sez Pisa, Largo B Pontecorvo 3, I-56127 Pisa, Italy

[25] Univ Pisa, Dipartimento Fis, Largo B Pontecorvo 3, I-56127 Pisa, Italy

[26] NASA Marshall Space Flight Ctr, Huntsville, AL 35812 USA

[27] Ist Nazl Fis Nucl, Sez Torino, Via Pietro Giuria 1, I-10125 Turin, Italy

[28] Univ Turin, Dipartimento Fis, Via Pietro Giuria 1, I-10125 Turin, Italy

[29] INAF Osservatorio Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy

[30] Univ Firenze, Dipartimento Fis & Astron, Via Sansone 1, I-50019 Sesto Fiorentino, FI, Italy

[31] Ist Nazl Fis Nucl, Sez Firenze, Via Sansone 1, I-50019 Sesto Fiorentino, FI, Italy

[32] Univ Space Res Assoc, Inst Sci & Technol, Huntsville, AL 35805 USA

[33] Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany

[34] RIKEN Cluster Pioneering Res, 2-1 Hirosawa, Wako, Saitama 3510198, Japan

[35] CALTECH, Pasadena, CA 91125 USA

[36] Yamagata Univ, 1-4-12 Kojirakawamachi, Yamagatashi 9908560, Japan

[37] Univ British Columbia, Vancouver, BC V6T IZ4, Canada

[38] Chiba Univ, Int Ctr Hadron Astrophys, Chiba 2638522, Japan

[39] Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA

[40] St Petersburg State Univ, Dept Astrophys, Univ pr 28,Petrodvoretz, St Petersburg 198504, Russia

[41] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA

[42] Univ New Hampshire, Astron & Space Sci Ctr, Durham, NH 03824 USA

[43] Washington Univ St Louis, Phys Dept, St Louis, MO 63130 USA

[44] Washington Univ St Louis, McDonnell Ctr Space Sci, St Louis, MO 63130 USA

[45] Univ Turku, Finnish Ctr Astron ESO, FI-20014 Turku, Finland

[46] Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Furocho,Chikusaku, Nagoya, Aichi 4648602, Japan

[47] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, 1-3-1 Kagamiyama, Higashihiroshima, Hiroshima 7398526, Japan

[48] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA

[49] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[50] NASA GSFC, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2023年 / 523卷 / 03期

基金：

美国国家航空航天局;

关键词：

polarization; galaxies: active; galaxies: individual: NGC 4151; galaxies: Seyfert; NARROW-LINE REGION; ACTIVE GALACTIC NUCLEI; PHOTON IMAGING CAMERA; GAS PIXEL DETECTOR; XMM-NEWTON; RELATIVISTIC REFLECTION; ACCRETION DISK; BLACK-HOLES; MODEL; SPECTRA;

D O I：

10.1093/mnras/stad1697

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present an X-ray spectropolarimetric analysis of the bright Seyfert galaxy NGC 4151. The source has been observed with the Imaging X-ray Polarimetry Explorer (IXPE) for 700 ks, complemented with simultaneous XMM-Newton (50 ks) and NuSTAR (100 ks) pointings. A polarization degree & pi; = 4.9 & PLUSMN; 1.1 per cent and angle & psi; = 86 & DEG; & PLUSMN; 7 & DEG; east of north (68 per cent confidence level) are measured in the 2-8 keV energy range. The spectropolarimetric analysis shows that the polarization could be entirely due to reflection. Given the low reflection flux in the IXPE band, this requires, however, a reflection with a very large (>38 per cent) polarization degree. Assuming more reasonable values, a polarization degree of the hot corona ranging from & SIM;4 to & SIM;8 per cent is found. The observed polarization degree excludes a 'spherical' lamppost geometry for the corona, suggesting instead a slab-like geometry, possibly a wedge, as determined via Monte Carlo simulations. This is further confirmed by the X-ray polarization angle, which coincides with the direction of the extended radio emission in this source, supposed to match the disc axis. NGC 4151 is the first active galactic nucleus with an X-ray polarization measure for the corona, illustrating the capabilities of X-ray polarimetry and IXPE in unveiling its geometry.

引用

页码：4468 / 4476

页数：9

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