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eROSITA calibration and performance verification phase: High-mass X-ray binaries in the Magellanic Clouds

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cris.lastimport.scopus2024-02-12T19:54:02Z
dc.abstract.enContext. During its performance verification phase, the soft X-ray instrument eROSITA on board the Spektrum-Roentgen-Gamma (SRG) spacecraft observed large regions in the Magellanic Clouds in which almost 40 known high-mass X-ray binaries (HMXBs, including candidates) are located. Aims: We looked for new HMXBs in the eROSITA data, searched for pulsations in HMXB candidates, and investigated the long-term behaviour of the full sample using archival X-ray and optical data. Methods: For sufficiently bright sources, we performed a detailed spectral and temporal analysis of their eROSITA data. A source detection analysis of the eROSITA images in different energy bands provided count rates and upper limits for the remaining sources. Results: We report the discovery of a new Be/X-ray binary in the Large Magellanic Cloud. The transient SRGEt J052829.5-690345 was detected with a 0.2-8.0 keV luminosity of~10<SUP>35</SUP> erg s<SUP>−1</SUP>. It exhibits a hard X-ray spectrum, typical for this class of HMXBs. The OGLE I-band light curve of the V~15.7mag counterpart shows large variations up to 0.75 mag, which occur with a quasi-period of~511 days. The eROSITA observations of the Small Magellanic Cloud covered 16 Be/X-ray binary pulsars, 5 of which were bright enough for an accurate determination of their current pulse period. The pulse periods for SXP 726 and SXP 1323 measured from eROSITA data are~800 s and~1006 s, respectively, which is very different from their discovery periods. Including archival XMM-Newton observations, we update the spin-period history of the two long-period pulsars, which have shown nearly linear trends in their period evolution for more than 15 yr. The corresponding average spin-down rate for SXP 726 is 4.3 s yr<SUP>−1</SUP>, while SXP 1323 has a spin-up rate of -23.2 s yr<SUP>−1</SUP>. We discuss the spin evolution of the two pulsars in the framework of quasi-spherical accretion.
dc.affiliationUniwersytet Warszawski
dc.contributor.authorHaberl, F.
dc.contributor.authorDoroshenko, V.
dc.contributor.authorMaitra, C.
dc.contributor.authorDai, X.
dc.contributor.authorCarpano, S.
dc.contributor.authorSasaki, M.
dc.contributor.authorUdalski, Andrzej
dc.contributor.authorPostnov, K. A.
dc.contributor.authorShakura, N. I.
dc.contributor.authorDennerl, K.
dc.contributor.authorFreyberg, M. J.
dc.date.accessioned2024-01-24T22:50:00Z
dc.date.available2024-01-24T22:50:00Z
dc.date.copyright2022-05-18
dc.date.issued2022
dc.description.accesstimeAT_PUBLICATION
dc.description.financePublikacja bezkosztowa
dc.description.versionFINAL_PUBLISHED
dc.description.volume661
dc.identifier.doi10.1051/0004-6361/202141878
dc.identifier.issn0004-6361
dc.identifier.urihttps://repozytorium.uw.edu.pl//handle/item/106356
dc.identifier.weblinkhttp://adsabs.harvard.edu/abs/2022A&A...661A..25H
dc.languageeng
dc.pbn.affiliationastronomy
dc.relation.ispartofAstronomy and Astrophysics
dc.relation.pagesA25
dc.rightsCC-BY
dc.sciencecloudnosend
dc.titleeROSITA calibration and performance verification phase: High-mass X-ray binaries in the Magellanic Clouds
dc.typeJournalArticle
dspace.entity.typePublication