The X-ray polarization of the Seyfert 1 galaxy IC 4329A

被引：27

作者：

Ingram, A. ^{[1
]}

Ewing, M. ^{[1
]}

Marinucci, A. ^{[2
]}

Tagliacozzo, D. ^{[3
]}

Rosario, D. J. ^{[1
]}

Veledina, A. ^{[4
,5
,6
]}

Kim, D. E. ^{[7
,8
,9
]}

Marin, F. ^{[10
]}

Bianchi, S. ^{[3
]}

Poutanen, J. ^{[4
]}

Matt, G. ^{[3
]}

Marshall, H. L. ^{[11
]}

Ursini, F. ^{[3
]}

De Rosa, A. ^{[7
]}

Petrucci, P-O ^{[12
]}

Madejski, G. ^{[13
,14
]}

Barnouin, T. ^{[10
]}

Gesu, L. Di ^{[2
]}

Dovciak, M. ^{[15
]}

Gianolli, V. E. ^{[3
,12
]}

Krawczynski, H. ^{[16
,17
]}

Loktev, V ^{[4
]}

Middei, R. ^{[7
,18
]}

Podgorny, J. ^{[10
,15
,19
]}

Puccetti, S. ^{[18
]}

Ratheesh, A. ^{[7
]}

Soffitta, P. ^{[7
]}

Tombesi, F. ^{[9
,20
,21
]}

Ehlert, S. R. ^{[22
]}

Massaro, F. ^{[23
,24
]}

Agudo, I ^{[25
]}

Antonelli, L. A. ^{[18
,26
]}

Bachetti, M. ^{[27
]}

Baldini, L. ^{[28
,29
]}

Baumgartner, W. H. ^{[22
]}

Bellazzini, R. ^{[28
]}

Bongiorno, S. D. ^{[22
]}

Bonino, R. ^{[23
,24
]}

Brez, A. ^{[28
]}

Bucciantini, N. ^{[30
,31
,32
]}

Capitanio, F. ^{[7
]}

Castellano, S. ^{[28
]}

Cavazzuti, E. ^{[2
]}

Chen, C-T ^{[33
]}

Ciprini, S. ^{[18
,20
]}

Costa, E. ^{[7
]}

Del Monte, E. ^{[7
]}

Lalla, N. Di ^{[13
,14
]}

Marco, A. Di ^{[7
]}

Donnarumma, I ^{[2
]}

机构：

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

[2] ASI Agenzia Spaziale Italiana, Via Politecnico Snc, I-00133 Rome, Italy

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

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

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

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

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

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

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

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

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

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

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

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

[15] Czech Acad Sci, Astron Inst, Bocni 2 1401-1, CZ-14100 Prague 4, Czech Republic

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

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

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

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

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

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

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

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

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

[25] Inst Astrofis Andalucia CSIC, Glorieta Astron s-n, E-18008 Granada, Spain

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

[27] INAF Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy

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

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

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

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

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

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

[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 Kojirakawamachi, Yamagatashi 9908560, Japan

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

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

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

[41] St Petersburg State Univ, Dept Astrophys, Univ sky pr 28, St Petersburg 198504, Russia

[42] Univ New Hampshire, Dept Phys & Astron, Durham, NH 03824 USA

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

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

[45] Ist Nazl Fis Nucl, Sez Napoli, Str Comunale Cinthia, I-80126 Naples, Italy

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

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

[48] Univ Maryland, 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 / 525卷 / 04期

基金：

美国国家航空航天局;

关键词：

polarization; galaxies: active; galaxies: individual: IC 4329A; galaxies: Seyfert; ACTIVE GALACTIC NUCLEI; PHOTON IMAGING CAMERA; BLACK-HOLES; XMM-NEWTON; ACCRETION DISK; IRON LINE; COMPTON REFLECTION; CYGNUS X-1; NGC; 4151; SPECTRUM;

D O I：

10.1093/mnras/stad2625

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present an X-ray spectro-polarimetric analysis of the bright Seyfert galaxy IC 4329A. The Imaging X-ray Polarimetry Explorer (IXPE) observed the source for -500 ks, supported by XMM-Newton ( -60 ks) and NuSTAR ( -80 ks) exposures. We detect polarization in the 2-8 keV band with 2.97 sigma confidence. We report a polarization degree of 3.3 +/- 1.1 per cent and a polarization angle of 78 degrees +/- 10 degrees (errors are 1 sigma confidence). The X-ray polarization is consistent with being aligned with the radio jet, albeit partially due to large uncertainties on the radio position angle. We jointly fit the spectra from the three observatories to constrain the presence of a relativistic reflection component. From this, we obtain constraints on the inclination angle to the inner disc ( < 39 degrees at 99 per cent confidence) and the disc inner radius ( < 11 gravitational radii at 99 per cent confidence), although we note that modelling systematics in practice add to the quoted statistical error. Our spectropolarimetric modelling indicates that the 2-8 keV polarization is consistent with being dominated by emission directly observed from the X-ray corona, but the polarization of the reflection component is completely unconstrained. Our constraints on viewer inclination and polarization degree tentatively fa v our more asymmetric, possibly out-flowing, coronal geometries that produce more highly polarized emission, but the coronal geometry is unconstrained at the 3 sigma level.

引用

页码：5437 / 5449

页数：13

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