X-Ray Polarization of the Eastern Lobe of SS 433

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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.authorMarco AD
dc.contributor.authorSlane P
dc.contributor.authorBianchi S
dc.contributor.authorIngram A
dc.contributor.authorRomani RW
dc.contributor.authorCibrario N
dc.contributor.authorIntyre BM
dc.contributor.authorMikus̆incová 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 C
dc.contributor.authorCiprini S
dc.contributor.authorRosa AD
dc.contributor.authorMonte ED
dc.contributor.authorGesu LD
dc.contributor.authorLalla ND
dc.contributor.authorDonnarumma I
dc.contributor.authorDoroshenko V
dc.contributor.authorDovčiak 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.authorMonaca FL
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 C
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 P
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.contributor.organizationfi=Tuorlan observatorio|en=Tuorla Observatory|
dc.contributor.organization-code1.2.246.10.2458963.20.90670098848
dc.converis.publication-id381279088
dc.converis.urlhttps://research.utu.fi/converis/portal/Publication/381279088
dc.date.accessioned2025-08-28T02:30:23Z
dc.date.available2025-08-28T02:30:23Z
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 γ-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° to +10° (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.identifier.eissn2041-8213
dc.identifier.jour-issn2041-8205
dc.identifier.olddbid209210
dc.identifier.oldhandle10024/192237
dc.identifier.urihttps://www.utupub.fi/handle/11111/40782
dc.identifier.urlhttps://dx.doi.org/10.3847/2041-8213/ad103b
dc.identifier.urnURN:NBN:fi-fe2025082792286
dc.language.isoen
dc.okm.affiliatedauthorPoutanen, Juri
dc.okm.affiliatedauthorVeledina, Alexandra
dc.okm.affiliatedauthorTsygankov, Sergey
dc.okm.discipline115 Astronomy and space scienceen_GB
dc.okm.discipline115 Avaruustieteet ja tähtitiedefi_FI
dc.okm.internationalcopublicationinternational co-publication
dc.okm.internationalityInternational publication
dc.okm.typeA1 ScientificArticle
dc.publisherInstitute of Physics Publishing
dc.publisher.countryUnited Kingdomen_GB
dc.publisher.countryBritanniafi_FI
dc.publisher.country-codeGB
dc.relation.articlenumberL12
dc.relation.doi10.3847/2041-8213/ad103b
dc.relation.ispartofjournalAstrophysical Journal Letters
dc.relation.issue1
dc.relation.volume961
dc.source.identifierhttps://www.utupub.fi/handle/10024/192237
dc.titleX-Ray Polarization of the Eastern Lobe of SS 433
dc.year.issued2024

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