File Download

There are no files associated with this item.

  Links for fulltext
     (May Require Subscription)
Supplementary

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

TitleUncovering the geometry of the hot X-ray corona in the Seyfert galaxy NGC 4151 with IXPE
Authors
Keywordsgalaxies: active
galaxies: individual: NGC 4151
galaxies: Seyfert
polarization
Issue Date8-Jun-2023
PublisherRoyal Astronomical Society
Citation
Monthly Notices of the Royal Astronomical Society, 2023, v. 523, n. 3, p. 4468-4476 How to Cite?
Abstract

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.


Persistent Identifierhttp://hdl.handle.net/10722/331920
ISSN
2023 Impact Factor: 4.7
2023 SCImago Journal Rankings: 1.621
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorGianolli, VE-
dc.contributor.authorKim, DE-
dc.contributor.authorBianchi, S-
dc.contributor.authorAgis-Gonzalez, B-
dc.contributor.authorMadejski, G-
dc.contributor.authorMarin, F-
dc.contributor.authorMarinucci, A-
dc.contributor.authorMatt, G-
dc.contributor.authorMiddei, R-
dc.contributor.authorPetrucci, PO-
dc.contributor.authorSoffitta, P-
dc.contributor.authorTagliacozzo, D-
dc.contributor.authorTombesi, F-
dc.contributor.authorUrsini, F-
dc.contributor.authorBarnouin, T-
dc.contributor.authorDe, Rosa, A-
dc.contributor.authorDi, Gesu, L-
dc.contributor.authorIngram, A-
dc.contributor.authorLoktev, V-
dc.contributor.authorPanagiotou, C-
dc.contributor.authorPodgorny, J-
dc.contributor.authorPoutanen, J-
dc.contributor.authorPuccetti, S-
dc.contributor.authorRatheesh, A-
dc.contributor.authorVeledina, A-
dc.contributor.authorZhang, W-
dc.contributor.authorAgudo, I-
dc.contributor.authorAntonelli, LA-
dc.contributor.authorBachetti, M-
dc.contributor.authorBaldini, L-
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, I-
dc.contributor.authorDoroshenko, V-
dc.contributor.authorDovciak, M-
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.authorKaras, V-
dc.contributor.authorKislat, F-
dc.contributor.authorKitaguchi, T-
dc.contributor.authorKolodziejczak, JJ-
dc.contributor.authorKrawczynski, H-
dc.contributor.authorLa, Monaca, F-
dc.contributor.authorLatronico, L-
dc.contributor.authorLiodakis, I-
dc.contributor.authorMaldera, S-
dc.contributor.authorManfreda, A-
dc.contributor.authorMarscher, AP-
dc.contributor.authorMarshall, HL-
dc.contributor.authorMassaro, F-
dc.contributor.authorMitsuishi, I-
dc.contributor.authorMizuno, T-
dc.contributor.authorMuleri, F-
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.authorRoberts, OJ-
dc.contributor.authorRomani, RW-
dc.contributor.authorSgro, 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.accessioned2023-09-28T04:59:37Z-
dc.date.available2023-09-28T04:59:37Z-
dc.date.issued2023-06-08-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2023, v. 523, n. 3, p. 4468-4476-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/10722/331920-
dc.description.abstract<p>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.</p>-
dc.languageeng-
dc.publisherRoyal Astronomical Society-
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society-
dc.subjectgalaxies: active-
dc.subjectgalaxies: individual: NGC 4151-
dc.subjectgalaxies: Seyfert-
dc.subjectpolarization-
dc.titleUncovering the geometry of the hot X-ray corona in the Seyfert galaxy NGC 4151 with IXPE-
dc.typeArticle-
dc.identifier.doi10.1093/mnras/stad1697-
dc.identifier.scopuseid_2-s2.0-85163967361-
dc.identifier.volume523-
dc.identifier.issue3-
dc.identifier.spage4468-
dc.identifier.epage4476-
dc.identifier.eissn1365-2966-
dc.identifier.isiWOS:001023556700020-
dc.publisher.placeOXFORD-
dc.identifier.issnl0035-8711-

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats