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Article: X-Ray Polarization of the BL Lacertae Type Blazar 1ES 0229+200

TitleX-Ray Polarization of the BL Lacertae Type Blazar 1ES 0229+200
Authors
Issue Date6-Dec-2023
PublisherAmerican Astronomical Society
Citation
Astrophysical Journal, 2023, v. 959, n. 1, p. 1-11 How to Cite?
Abstract

We present polarization measurements in the 2-8 keV band from blazar 1ES 0229+200, the first extreme high synchrotron peaked source to be observed by the Imaging X-ray Polarimetry Explorer (IXPE). Combining two exposures separated by about two weeks, we find the degree of polarization to be Pi(X) = 17.9% +/- 2.8% at an electric-vector position angle psi(X) = 25(degrees).0 +/- 4(degrees).6 using a spectro-polarimetric fit from joint IXPE and XMM-Newton observations. There is no evidence for the polarization degree or angle varying significantly with energy or time on both short timescales (hours) or longer timescales (days). The contemporaneous polarization degree at optical wavelengths was >7x lower, making 1ES 0229+200 the most strongly chromatic blazar yet observed. This high X-ray polarization compared to the optical provides further support that X-ray emission in high-peaked blazars originates in shock-accelerated, energy-stratified electron populations, but is in tension with many recent modeling efforts attempting to reproduce the spectral energy distribution of 1ES 0229+200, which attribute the extremely high energy synchrotron and Compton peaks to Fermi acceleration in the vicinity of strongly turbulent magnetic fields.


Persistent Identifierhttp://hdl.handle.net/10722/340781
ISSN
2023 Impact Factor: 4.8
2023 SCImago Journal Rankings: 1.905
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorEhlert, SR-
dc.contributor.authorLiodakis, I-
dc.contributor.authorMiddei, R-
dc.contributor.authorMarscher, AP-
dc.contributor.authorTavecchio, F-
dc.contributor.authorAgudo, I-
dc.contributor.authorKouch, PM-
dc.contributor.authorLindfors, E-
dc.contributor.authorNilsson, K-
dc.contributor.authorMyserlis, I-
dc.contributor.authorGurwell, M-
dc.contributor.authorRao, RMS-
dc.contributor.authorAceituno, FJ-
dc.contributor.authorBonnoli, G-
dc.contributor.authorCasanova, V-
dc.contributor.authorAgis-Gonzalez, B-
dc.contributor.authorEscudero, J-
dc.contributor.authorHusillos, C-
dc.contributor.authorSantos, JO-
dc.contributor.authorSota, A-
dc.contributor.authorAngelakis, E-
dc.contributor.authorKraus, A-
dc.contributor.authorKeating, GK-
dc.contributor.authorAntonelli, LA-
dc.contributor.authorBachetti, M-
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.authorCapitanio, F-
dc.contributor.authorCastellano, S-
dc.contributor.authorCavazzuti, E-
dc.contributor.authorChen, CT-
dc.contributor.authorCiprini, S-
dc.contributor.authorCosta, E-
dc.contributor.authorde Rosa, A-
dc.contributor.authorDel Monte, E-
dc.contributor.authorDi Gesu, L-
dc.contributor.authorDi Lalla, N-
dc.contributor.authorDi Marco, A-
dc.contributor.authorDonnarumma, I-
dc.contributor.authorDoroshenko, V-
dc.contributor.authorDovciak, M-
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.authorHayashida, K-
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.authorMaldera, S-
dc.contributor.authorManfreda, A-
dc.contributor.authorMarin, F-
dc.contributor.authorMarinucci, A-
dc.contributor.authorMarshall, HL-
dc.contributor.authorMassaro, F-
dc.contributor.authorMatt, G-
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.authorPetrucci, PO-
dc.contributor.authorPilia, M-
dc.contributor.authorPossenti, A-
dc.contributor.authorPoutanen, J-
dc.contributor.authorPuccetti, S-
dc.contributor.authorRamsey, BD-
dc.contributor.authorRankin, J-
dc.contributor.authorRatheesh, A-
dc.contributor.authorRoberts, OJ-
dc.contributor.authorRomani, RW-
dc.contributor.authorSgro, C-
dc.contributor.authorSlane, P-
dc.contributor.authorSoffitta, P-
dc.contributor.authorSpandre, G-
dc.contributor.authorSwartz, DA-
dc.contributor.authorTamagawa, T-
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.authorWeisskopf, MC-
dc.contributor.authorWu, KW-
dc.contributor.authorXie, F-
dc.contributor.authorZane, S-
dc.date.accessioned2024-03-11T10:47:04Z-
dc.date.available2024-03-11T10:47:04Z-
dc.date.issued2023-12-06-
dc.identifier.citationAstrophysical Journal, 2023, v. 959, n. 1, p. 1-11-
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/10722/340781-
dc.description.abstract<p>We present polarization measurements in the 2-8 keV band from blazar 1ES 0229+200, the first extreme high synchrotron peaked source to be observed by the Imaging X-ray Polarimetry Explorer (IXPE). Combining two exposures separated by about two weeks, we find the degree of polarization to be Pi(X) = 17.9% +/- 2.8% at an electric-vector position angle psi(X) = 25(degrees).0 +/- 4(degrees).6 using a spectro-polarimetric fit from joint IXPE and XMM-Newton observations. There is no evidence for the polarization degree or angle varying significantly with energy or time on both short timescales (hours) or longer timescales (days). The contemporaneous polarization degree at optical wavelengths was >7x lower, making 1ES 0229+200 the most strongly chromatic blazar yet observed. This high X-ray polarization compared to the optical provides further support that X-ray emission in high-peaked blazars originates in shock-accelerated, energy-stratified electron populations, but is in tension with many recent modeling efforts attempting to reproduce the spectral energy distribution of 1ES 0229+200, which attribute the extremely high energy synchrotron and Compton peaks to Fermi acceleration in the vicinity of strongly turbulent magnetic fields.</p>-
dc.languageeng-
dc.publisherAmerican Astronomical Society-
dc.relation.ispartofAstrophysical Journal-
dc.rightsThis work is licensed under a Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.-
dc.titleX-Ray Polarization of the BL Lacertae Type Blazar 1ES 0229+200-
dc.typeArticle-
dc.identifier.doi10.3847/1538-4357/ad05c4-
dc.identifier.scopuseid_2-s2.0-85180102724-
dc.identifier.volume959-
dc.identifier.issue1-
dc.identifier.spage1-
dc.identifier.epage11-
dc.identifier.eissn1538-4357-
dc.identifier.isiWOS:001116439900001-
dc.publisher.placeBRISTOL-
dc.identifier.issnl0004-637X-

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