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Timing six energetic rotation-powered X-ray pulsars, including the fast-spinning young PSR J0058-7218 and Big Glitcher PSR J0537-6910

dc.contributor.authorHO, Wynn C.G.
dc.contributor.authorKUIPER, Lucien
dc.contributor.authorESPINOZA, Cristobal M.
hal.structure.identifierInstitut de recherche en astrophysique et planétologie [IRAP]
hal.structure.identifierCentre National d'Études Spatiales [Toulouse] [CNES]
dc.contributor.authorGUILLOT, Sebastien
dc.contributor.authorRAY, Paul S.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorSMITH, D.A.
dc.contributor.authorBOGDANOV, Slavko
dc.contributor.authorANTONOPOULOU, Danai
dc.contributor.authorARZOUMANIAN, Zaven
dc.contributor.authorBEJGER, Michal
dc.contributor.authorENOTO, Teruaki
dc.contributor.authorESPOSITO, Paolo
dc.contributor.authorHARDING, Alice K.
dc.contributor.authorHASKELL, Brynmor
dc.contributor.authorLEWANDOWSKA, Natalia
dc.contributor.authorMAITRA, Chandreyee
hal.structure.identifierObservatoire astronomique de Strasbourg [ObAS]
dc.contributor.authorVASILOPOULOS, Georgios
dc.date.issued2022
dc.description.abstractEnMeasuring a pulsar's rotational evolution is crucial to understanding the nature of the pulsar. Here we provide updated timing models for the rotational evolution of six pulsars, five of which are rotation phase-connected using primarily NICER X-ray data. For the newly-discovered fast energetic young pulsar, PSR J0058-7218, we increase the baseline of its timing model from 1.4 days to 8 months and not only measure more precisely its spin-down rate nudot = (-6.2324+/-0.0001)x10^-11 Hz s^-1 but also for the first time the second time derivative of spin rate nuddot = (4.2+/-0.2)x10^-21 Hz s^-2. For the fastest and most energetic young pulsar, PSR J0537-6910 (with 16 ms spin period), we detect 4 more glitches, for a total of 15 glitches over 4.5 years of NICER monitoring, and show that its spin-down behavior continues to set this pulsar apart from all others, including a long-term braking index n = -1.234+/-0.009 and interglitch braking indices that asymptote to <~ 7 for long times after a glitch. For PSR J1101-6101, we measure a much more accurate spin-down rate that agrees with a previous value measured without phase-connection. For PSR J1412+7922 (also known as Calvera), we extend the baseline of its timing model from our previous 1-year model to 4.4 years, and for PSR J1849-0001, we extend the baseline from 1.5 years to 4.7 years. We also present a long-term timing model of the energetic pulsar, PSR J1813-1749, by fitting previous radio and X-ray spin frequencies from 2009-2019 and new ones measured here using 2018 NuSTAR and 2021 Chandra data.
dc.language.isoen
dc.rights.urihttp://creativecommons.org/licenses/by/
dc.title.enTiming six energetic rotation-powered X-ray pulsars, including the fast-spinning young PSR J0058-7218 and Big Glitcher PSR J0537-6910
dc.typeArticle de revue
dc.identifier.doi10.3847/1538-4357/ac8743
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
dc.identifier.arxiv2205.02865
bordeaux.journalAstrophys.J
bordeaux.page7
bordeaux.volume939
bordeaux.issue1
bordeaux.peerReviewedoui
hal.identifierhal-03676099
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-03676099v1
bordeaux.COinSctx_ver=Z39.88-2004&amp;rft_val_fmt=info:ofi/fmt:kev:mtx:journal&amp;rft.jtitle=Astrophys.J&amp;rft.date=2022&amp;rft.volume=939&amp;rft.issue=1&amp;rft.spage=7&amp;rft.epage=7&amp;rft.au=HO,%20Wynn%20C.G.&amp;KUIPER,%20Lucien&amp;ESPINOZA,%20Cristobal%20M.&amp;GUILLOT,%20Sebastien&amp;RAY,%20Paul%20S.&amp;rft.genre=article


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