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Article: X-Ray Polarization of the Eastern Lobe of SS 433

TitleX-Ray Polarization of the Eastern Lobe of SS 433
Authors
Kaaret, PFerrazzoli, RSilvestri, SNegro, MManfreda, AWu, KCosta, ESoffitta, PSafi-Harb, SPoutanen, JVeledina, ADi Marco, ASlane, PBianchi, SIngram, ARomani, RWCibrario, NMac, Intyre BMikusincová, RRatheesh, ASteiner, JFSvoboda, JTugliani, SAgudo, IAntonelli, LABachetti, MBaldini, LBaumgartner, WHBellazzini, RBongiorno, SDBonino, RBrez, ABucciantini, NCapitanio, FCastellano, SCavazzuti, EChen, CTCiprini, Sde Rosa, ADel Monte, EDi Gesu, LDi Lalla, NDonnarumma, IDoroshenko, VDovciak, MEhlert, SREnoto, TEvangelista, YFabiani, SGarcía, JAGunji, SHayashida, KHeyl, JIwakiri, WJorstad, SGKaras, VKislat, FKitaguchi, TKolodziejczak, JJKrawczynski, HLa Monaca, FLatronico, LLiodakis, IMaldera, SMarin, FMarinucci, AMarscher, APMarshall, HLMassaro, FMatt, GMitsuishi, IMizuno, TMuleri, FNg, CYO'Dell, SLOmodei, NOppedisano, CPapitto, APavlov, GGPeirson, ALPerri, MPesce-Rollins, MPetrucci, POPilia, MPossenti, APuccetti, SRamsey, BDRankin, JRoberts, OJSgrò, CSpandre, GSwartz, DATamagawa, TTavecchio, FTaverna, RTawara, YTennant, AFThomas, NETombesi, FTrois, ATsygankov, SSTurolla, RVink, JWeisskopf, MCXie, FZane, S
Issue Date1-Jan-2024
PublisherAmerican Astronomical Society
Citation
Astrophysical Journal Letters, 2024, v. 961, n. 1, p. 1-8 How to Cite?
DOI: http://dx.doi.org/10.3847/2041-8213/ad103b
AbstractHow astrophysical systems translate the kinetic energy of bulk motion into the acceleration of particles to very high energies is a pressing question. SS 433 is a microquasar that emits TeV gamma-rays indicating the presence of high-energy particles. A region of hard X-ray emission in the eastern lobe of SS 433 was recently identified as an acceleration site. We observed this region with the Imaging X-ray Polarimetry Explorer and measured a polarization degree in the range 38%-77%. The high polarization degree indicates the magnetic field has a well-ordered component if the X-rays are due to synchrotron emission. The polarization angle is in the range -12 degrees to +10 degrees (east of north), which indicates that the magnetic field is parallel to the jet. Magnetic fields parallel to the bulk flow have also been found in supernova remnants and the jets of powerful radio galaxies. This may be caused by interaction of the flow with the ambient medium.
Persistent Identifierhttp://hdl.handle.net/10722/342097
ISSN
2041-8205
2021 Impact Factor: 8.811
2020 SCImago Journal Rankings: 3.639
ISI Accession Number ID
WOS:001159187000001

 

DC FieldValueLanguage
dc.contributor.authorKaaret, P-
dc.contributor.authorFerrazzoli, R-
dc.contributor.authorSilvestri, S-
dc.contributor.authorNegro, M-
dc.contributor.authorManfreda, A-
dc.contributor.authorWu, K-
dc.contributor.authorCosta, E-
dc.contributor.authorSoffitta, P-
dc.contributor.authorSafi-Harb, S-
dc.contributor.authorPoutanen, J-
dc.contributor.authorVeledina, A-
dc.contributor.authorDi Marco, A-
dc.contributor.authorSlane, P-
dc.contributor.authorBianchi, S-
dc.contributor.authorIngram, A-
dc.contributor.authorRomani, RW-
dc.contributor.authorCibrario, N-
dc.contributor.authorMac, Intyre B-
dc.contributor.authorMikusincová, R-
dc.contributor.authorRatheesh, A-
dc.contributor.authorSteiner, JF-
dc.contributor.authorSvoboda, J-
dc.contributor.authorTugliani, S-
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.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.authorDovciak, M-
dc.contributor.authorEhlert, SR-
dc.contributor.authorEnoto, T-
dc.contributor.authorEvangelista, Y-
dc.contributor.authorFabiani, S-
dc.contributor.authorGarcía, 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.authorLa Monaca, F-
dc.contributor.authorLatronico, L-
dc.contributor.authorLiodakis, I-
dc.contributor.authorMaldera, S-
dc.contributor.authorMarin, F-
dc.contributor.authorMarinucci, A-
dc.contributor.authorMarscher, AP-
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.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.authorPuccetti, S-
dc.contributor.authorRamsey, BD-
dc.contributor.authorRankin, J-
dc.contributor.authorRoberts, OJ-
dc.contributor.authorSgrò, C-
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.authorWeisskopf, MC-
dc.contributor.authorXie, F-
dc.contributor.authorZane, S-
dc.date.accessioned2024-04-02T08:25:32Z-
dc.date.available2024-04-02T08:25:32Z-
dc.date.issued2024-01-01-
dc.identifier.citationAstrophysical Journal Letters, 2024, v. 961, n. 1, p. 1-8-
dc.identifier.issn2041-8205-
dc.identifier.urihttp://hdl.handle.net/10722/342097-
dc.description.abstractHow astrophysical systems translate the kinetic energy of bulk motion into the acceleration of particles to very high energies is a pressing question. SS 433 is a microquasar that emits TeV gamma-rays indicating the presence of high-energy particles. A region of hard X-ray emission in the eastern lobe of SS 433 was recently identified as an acceleration site. We observed this region with the Imaging X-ray Polarimetry Explorer and measured a polarization degree in the range 38%-77%. The high polarization degree indicates the magnetic field has a well-ordered component if the X-rays are due to synchrotron emission. The polarization angle is in the range -12 degrees to +10 degrees (east of north), which indicates that the magnetic field is parallel to the jet. Magnetic fields parallel to the bulk flow have also been found in supernova remnants and the jets of powerful radio galaxies. This may be caused by interaction of the flow with the ambient medium.-
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.titleX-Ray Polarization of the Eastern Lobe of SS 433-
dc.typeArticle-
dc.identifier.doi10.3847/2041-8213/ad103b-
dc.identifier.scopuseid_2-s2.0-85182773843-
dc.identifier.volume961-
dc.identifier.issue1-
dc.identifier.spage1-
dc.identifier.epage8-
dc.identifier.eissn2041-8213-
dc.identifier.isiWOS:001159187000001-
dc.publisher.placeBRISTOL-
dc.identifier.issnl2041-8205-

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