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Article: The geometry of the hot corona in MCG-05-23-16 constrained by X-ray polarimetry

TitleThe geometry of the hot corona in MCG-05-23-16 constrained by X-ray polarimetry
Authors
Keywordsgalaxies: Active
galaxies: Seyfert
polarization
X-rays: galaxies
X-rays: individual: MCG-05-23-16
Issue Date1-Sep-2023
PublisherOxford University Press
Citation
Monthly Notices of the Royal Astronomical Society, 2023, v. 525, n. 3, p. 4735-4743 How to Cite?
AbstractWe report on the second observation of the radio-quiet active galactic nucleus (AGN) MCG-05-23-16 performed with the Imaging X-ray Polarimetry Explorer (IXPE). The observation started on 2022 November 6 for a net observing time of 640 ks, and was partly simultaneous with NuSTAR (86 ks). After combining these data with those obtained in the first IXPE pointing on May 2022 (simultaneous with XMM-Newton and NuSTAR) we find a 2-8 keV polarization degree Pi = 1.6 +/- 0.7 (at 68 per cent confidence level), which corresponds to an upper limit Pi = 3.2 per cent (at 99 per cent confidence level). We then compare the polarization results with Monte Carlo simulations obtained with the MONK code, with which different coronal geometries have been explored (spherical lamppost, conical, slab and wedge). Furthermore, the allowed range of inclination angles is found for each geometry. If the best fit inclination value from a spectroscopic analysis is considered, a cone-shaped corona along the disc axis is disfavoured.
Persistent Identifierhttp://hdl.handle.net/10722/339077
ISSN
2023 Impact Factor: 4.7
2023 SCImago Journal Rankings: 1.621
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorTagliacozzo, D-
dc.contributor.authorMarinucci, A-
dc.contributor.authorUrsini, F-
dc.contributor.authorMatt, G-
dc.contributor.authorBianchi, S-
dc.contributor.authorBaldini, L-
dc.contributor.authorBarnouin, T-
dc.contributor.authorRodriguez, NC-
dc.contributor.authorDe Rosa, A-
dc.contributor.authorDi Gesu, L-
dc.contributor.authorDovciak, M-
dc.contributor.authorHarper, D-
dc.contributor.authorIngram, A-
dc.contributor.authorKaras,-
dc.contributor.authorKim, DE-
dc.contributor.authorKrawczynski, H-
dc.contributor.authorMadejski, G-
dc.contributor.authorMarin, F-
dc.contributor.authorMiddei, R-
dc.contributor.authorMarshall, HL-
dc.contributor.authorMuleri, F-
dc.contributor.authorPanagiotou, C-
dc.contributor.authorPetrucci, PO-
dc.contributor.authorPodgorny, J-
dc.contributor.authorPoutanen, J-
dc.contributor.authorPuccetti, S-
dc.contributor.authorSoffitta, P-
dc.contributor.authorTombesi, F-
dc.contributor.authorVeledina, A-
dc.contributor.authorZhang, W-
dc.contributor.authorAgudo,-
dc.contributor.authorAntonelli, LA-
dc.contributor.authorBachetti, M-
dc.contributor.authorBaumgartner, WH-
dc.contributor.authorBellazzini, R-
dc.contributor.authorBongiorno, SD-
dc.contributor.authorBonino, R-
dc.contributor.authorBrez, A-
dc.contributor.authorBucciantini, N-
dc.contributor.authorCapitanio, F-
dc.contributor.authorCastellano, S-
dc.contributor.authorCavazzuti, E-
dc.contributor.authorChen, CT-
dc.contributor.authorCiprini, S-
dc.contributor.authorCosta, E-
dc.contributor.authorDel Monte, E-
dc.contributor.authorDi Lalla, N-
dc.contributor.authorDi Marco, A-
dc.contributor.authorDonnarumma,-
dc.contributor.authorDoroshenko,-
dc.contributor.authorEhlert, SR-
dc.contributor.authorEnoto, T-
dc.contributor.authorEvangelista, Y-
dc.contributor.authorFabiani, S-
dc.contributor.authorFerrazzoli, R-
dc.contributor.authorGarcia, JA-
dc.contributor.authorGunji, S-
dc.contributor.authorHeyl, J-
dc.contributor.authorIwakiri, W-
dc.contributor.authorJorstad, SG-
dc.contributor.authorKaaret, P-
dc.contributor.authorKislat, F-
dc.contributor.authorKitaguchi, T-
dc.contributor.authorKolodziejczak, JJ-
dc.contributor.authorLa Monaca, F-
dc.contributor.authorLatronico, L-
dc.contributor.authorLiodakis,-
dc.contributor.authorMaldera, S-
dc.contributor.authorManfreda, A-
dc.contributor.authorMarscher, AP-
dc.contributor.authorMassaro, F-
dc.contributor.authorMitsuishi,-
dc.contributor.authorMizuno, T-
dc.contributor.authorNegro, M-
dc.contributor.authorNg, CY-
dc.contributor.authorO'Dell, SL-
dc.contributor.authorOmodei, N-
dc.contributor.authorOppedisano, C-
dc.contributor.authorPapitto, A-
dc.contributor.authorPavlov, GG-
dc.contributor.authorPeirson, AL-
dc.contributor.authorPerri, M-
dc.contributor.authorPesce-Rollins, M-
dc.contributor.authorPilia, M-
dc.contributor.authorPossenti, A-
dc.contributor.authorRamsey, BD-
dc.contributor.authorRankin, J-
dc.contributor.authorRatheesh, A-
dc.contributor.authorRoberts, OJ-
dc.contributor.authorRomani, RW-
dc.contributor.authorSgrò, C-
dc.contributor.authorSlane, P-
dc.contributor.authorSpandre, G-
dc.contributor.authorSwartz, DA-
dc.contributor.authorTamagawa, T-
dc.contributor.authorTavecchio, F-
dc.contributor.authorTaverna, R-
dc.contributor.authorTawara, Y-
dc.contributor.authorTennant, AF-
dc.contributor.authorThomas, NE-
dc.contributor.authorTrois, A-
dc.contributor.authorTsygankov, SS-
dc.contributor.authorTurolla, R-
dc.contributor.authorVink, J-
dc.contributor.authorWeisskopf, MC-
dc.contributor.authorWu, K-
dc.contributor.authorXie, F-
dc.contributor.authorZane, S-
dc.date.accessioned2024-03-11T10:33:42Z-
dc.date.available2024-03-11T10:33:42Z-
dc.date.issued2023-09-01-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2023, v. 525, n. 3, p. 4735-4743-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/10722/339077-
dc.description.abstractWe report on the second observation of the radio-quiet active galactic nucleus (AGN) MCG-05-23-16 performed with the Imaging X-ray Polarimetry Explorer (IXPE). The observation started on 2022 November 6 for a net observing time of 640 ks, and was partly simultaneous with NuSTAR (86 ks). After combining these data with those obtained in the first IXPE pointing on May 2022 (simultaneous with XMM-Newton and NuSTAR) we find a 2-8 keV polarization degree Pi = 1.6 +/- 0.7 (at 68 per cent confidence level), which corresponds to an upper limit Pi = 3.2 per cent (at 99 per cent confidence level). We then compare the polarization results with Monte Carlo simulations obtained with the MONK code, with which different coronal geometries have been explored (spherical lamppost, conical, slab and wedge). Furthermore, the allowed range of inclination angles is found for each geometry. If the best fit inclination value from a spectroscopic analysis is considered, a cone-shaped corona along the disc axis is disfavoured.-
dc.languageeng-
dc.publisherOxford University Press-
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society-
dc.subjectgalaxies: Active-
dc.subjectgalaxies: Seyfert-
dc.subjectpolarization-
dc.subjectX-rays: galaxies-
dc.subjectX-rays: individual: MCG-05-23-16-
dc.titleThe geometry of the hot corona in MCG-05-23-16 constrained by X-ray polarimetry-
dc.typeArticle-
dc.identifier.doi10.1093/mnras/stad2627-
dc.identifier.scopuseid_2-s2.0-85173579465-
dc.identifier.volume525-
dc.identifier.issue3-
dc.identifier.spage4735-
dc.identifier.epage4743-
dc.identifier.eissn1365-2966-
dc.identifier.isiWOS:001079289800010-
dc.publisher.placeOXFORD-
dc.identifier.issnl0035-8711-

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