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Article: First Detection of X-Ray Polarization from the Accreting Neutron Star 4U 1820-303

TitleFirst Detection of X-Ray Polarization from the Accreting Neutron Star 4U 1820-303
Authors
Issue Date1-Aug-2023
PublisherAmerican Astronomical Society
Citation
Astrophysical Journal Letters, 2023, v. 953, n. 2, p. 1-13 How to Cite?
AbstractThis paper reports the first detection of polarization in the X-rays for atoll-source 4U 1820-303, obtained with the Imaging X-ray Polarimetry Explorer (IXPE) at 99.999% confidence level (CL). Simultaneous polarimetric measurements were also performed in the radio with the Australia Telescope Compact Array. The IXPE observations of 4U 1820-303 were coordinated with Swift X-ray Telescope, Neutron Star Interior Composition Explorer, and Nuclear Spectroscopic Telescope Array aiming to obtain an accurate X-ray spectral model covering a broad energy interval. The source shows a significant polarization above 4 keV, with a polarization degree of 2.0% & PLUSMN; 0.5% and a polarization angle of -55 & DEG; & PLUSMN; 7 & DEG; in the 4-7 keV energy range, and a polarization degree of 10% & PLUSMN; 2% and a polarization angle of -67 & DEG; & PLUSMN; 7 & DEG; in the 7-8 keV energy bin. This polarization also shows a clear energy trend with polarization degree increasing with energy and a hint for a position-angle change of & SIME;90 & DEG; at 96% CL around 4 keV. The spectro-polarimetric fit indicates that the accretion disk is polarized orthogonally to the hard spectral component, which is presumably produced in the boundary/spreading layer. We do not detect linear polarization from the radio counterpart, with a 3 & sigma; upper limit of 50% at 7.25 GHz.
Persistent Identifierhttp://hdl.handle.net/10722/339076
ISSN
2023 Impact Factor: 8.8
2023 SCImago Journal Rankings: 2.766
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorDi Marco, A-
dc.contributor.authorLa Monaca, F-
dc.contributor.authorPoutanen, J-
dc.contributor.authorRussell, TD-
dc.contributor.authorAnitra, A-
dc.contributor.authorFarinelli, R-
dc.contributor.authorMastroserio, G-
dc.contributor.authorMuleri, F-
dc.contributor.authorXie, F-
dc.contributor.authorBachetti, M-
dc.contributor.authorBurderi, L-
dc.contributor.authorCarotenuto, F-
dc.contributor.authorDel Santo, M-
dc.contributor.authorDi Salvo, T-
dc.contributor.authorDovciak, M-
dc.contributor.authorGnarini, A-
dc.contributor.authorIaria, R-
dc.contributor.authorKajava, JJE-
dc.contributor.authorLiu, K-
dc.contributor.authorMiddei, R-
dc.contributor.authorO'Dell, SL-
dc.contributor.authorPilia, M-
dc.contributor.authorRankin, J-
dc.contributor.authorSanna, A-
dc.contributor.authorvan den Ejnden, J-
dc.contributor.authorWeisskopf, MC-
dc.contributor.authorBobrikova, A-
dc.contributor.authorCapitanio, F-
dc.contributor.authorCosta, E-
dc.contributor.authorKaaret, P-
dc.contributor.authorMarino, A-
dc.contributor.authorSoffitta, P-
dc.contributor.authorUrsini, F-
dc.contributor.authorAmbrosino, F-
dc.contributor.authorCocchi, M-
dc.contributor.authorFabiani, S-
dc.contributor.authorMarshall, H-
dc.contributor.authorMatt, G-
dc.contributor.authorMotta, SE-
dc.contributor.authorPapitto, A-
dc.contributor.authorStella, L-
dc.contributor.authorTarana, A-
dc.contributor.authorZane, S-
dc.contributor.authorAgudo, I-
dc.contributor.authorAntonelli, LA-
dc.contributor.authorBaldini, L-
dc.contributor.authorBaumgartner, WH-
dc.contributor.authorBellazzini, R-
dc.contributor.authorBianchi, S-
dc.contributor.authorBongiorno, SD-
dc.contributor.authorBonino, R-
dc.contributor.authorBrez, A-
dc.contributor.authorBucciantini, N-
dc.contributor.authorCastellano, S-
dc.contributor.authorCavazzuti, E-
dc.contributor.authorChen, CT-
dc.contributor.authorCiprini, S-
dc.contributor.authorDe Rosa, A-
dc.contributor.authorDel Monte, E-
dc.contributor.authorDi Gesu, L-
dc.contributor.authorDi Lalla, N-
dc.contributor.authorDonnarumma, I-
dc.contributor.authorDoroshenko, V-
dc.contributor.authorEhlert, SR-
dc.contributor.authorEnoto, T-
dc.contributor.authorEvangelista, Y-
dc.contributor.authorFerrazzoli, R-
dc.contributor.authorGarcia, JA-
dc.contributor.authorGunji, S-
dc.contributor.authorHayashida, K-
dc.contributor.authorHeyl, J-
dc.contributor.authorIwakiri, W-
dc.contributor.authorJorstad, SG-
dc.contributor.authorKaras, V-
dc.contributor.authorKislat, F-
dc.contributor.authorKitaguchi, T-
dc.contributor.authorKolodziejczak, JJ-
dc.contributor.authorKrawczynski, H-
dc.contributor.authorLatronico, L-
dc.contributor.authorLiodakis, I-
dc.contributor.authorMaldera, S-
dc.contributor.authorManfreda, A-
dc.contributor.authorMarin, F-
dc.contributor.authorMarinucci, A-
dc.contributor.authorMarscher, AP-
dc.contributor.authorMassaro, F-
dc.contributor.authorMitsuishi, I-
dc.contributor.authorMizuno, T-
dc.contributor.authorNegro, M-
dc.contributor.authorNg, CY-
dc.contributor.authorOmodei, N-
dc.contributor.authorOppedisano, C-
dc.contributor.authorPavlov, GG-
dc.contributor.authorPeirson, AL-
dc.contributor.authorPerri, M-
dc.contributor.authorPesce-Rollins, M-
dc.contributor.authorPetrucci, PO-
dc.contributor.authorPossenti, A-
dc.contributor.authorPuccetti, S-
dc.contributor.authorRamsey, BD-
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.authorTombesi, F-
dc.contributor.authorTrois, A-
dc.contributor.authorTsygankov, SS-
dc.contributor.authorTurolla, R-
dc.contributor.authorVink, J-
dc.contributor.authorWu, K-
dc.date.accessioned2024-03-11T10:33:42Z-
dc.date.available2024-03-11T10:33:42Z-
dc.date.issued2023-08-01-
dc.identifier.citationAstrophysical Journal Letters, 2023, v. 953, n. 2, p. 1-13-
dc.identifier.issn2041-8205-
dc.identifier.urihttp://hdl.handle.net/10722/339076-
dc.description.abstractThis paper reports the first detection of polarization in the X-rays for atoll-source 4U 1820-303, obtained with the Imaging X-ray Polarimetry Explorer (IXPE) at 99.999% confidence level (CL). Simultaneous polarimetric measurements were also performed in the radio with the Australia Telescope Compact Array. The IXPE observations of 4U 1820-303 were coordinated with Swift X-ray Telescope, Neutron Star Interior Composition Explorer, and Nuclear Spectroscopic Telescope Array aiming to obtain an accurate X-ray spectral model covering a broad energy interval. The source shows a significant polarization above 4 keV, with a polarization degree of 2.0% & PLUSMN; 0.5% and a polarization angle of -55 & DEG; & PLUSMN; 7 & DEG; in the 4-7 keV energy range, and a polarization degree of 10% & PLUSMN; 2% and a polarization angle of -67 & DEG; & PLUSMN; 7 & DEG; in the 7-8 keV energy bin. This polarization also shows a clear energy trend with polarization degree increasing with energy and a hint for a position-angle change of & SIME;90 & DEG; at 96% CL around 4 keV. The spectro-polarimetric fit indicates that the accretion disk is polarized orthogonally to the hard spectral component, which is presumably produced in the boundary/spreading layer. We do not detect linear polarization from the radio counterpart, with a 3 & sigma; upper limit of 50% at 7.25 GHz.-
dc.languageeng-
dc.publisherAmerican Astronomical Society-
dc.relation.ispartofAstrophysical Journal Letters-
dc.rightsThis work is licensed under a Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.-
dc.titleFirst Detection of X-Ray Polarization from the Accreting Neutron Star 4U 1820-303-
dc.typeArticle-
dc.identifier.doi10.3847/2041-8213/acec6e-
dc.identifier.scopuseid_2-s2.0-85169325138-
dc.identifier.volume953-
dc.identifier.issue2-
dc.identifier.spage1-
dc.identifier.epage13-
dc.identifier.eissn2041-8213-
dc.identifier.isiWOS:001053502200001-
dc.publisher.placeBRISTOL-
dc.identifier.issnl2041-8205-

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