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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/3755
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dc.contributor.authorKaur, Ramanpreet-
dc.contributor.authorWijnands, Rudy-
dc.contributor.authorPatruno, A.-
dc.contributor.authorTesta, Vincenzo-
dc.contributor.authorIsrael, Gianluca-
dc.contributor.authorDegenaar, Nathalie-
dc.contributor.authorPaul, Biswajit-
dc.contributor.authorKumar, Brijesh-
dc.date.accessioned2009-05-15T11:04:57Z-
dc.date.available2009-05-15T11:04:57Z-
dc.date.issued2009-04-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2009, Vol. 394(3), p1597-1604en
dc.identifier.issn0035-8711-
dc.identifier.issn1365-2966 (Online)-
dc.identifier.urihttp://hdl.handle.net/2289/3755-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en
dc.description.abstractWe present results from our Chandra and XMM–Newton observations of two low-luminosity X-ray pulsators SAX J1324.4−6200 and SAX J1452.8−5949 which have spin periods of 172 and 437 s, respectively. The XMM–Newton spectra for both sources can be fitted well with a simple power-law model of photon index, Γ∼ 1.0 . A blackbody model can equally well fit the spectra with a temperature, kT∼ 2 keV, for both sources. During our XMM–Newton observations, SAX J1324.4−6200 is detected with coherent X-ray pulsations at a period of 172.86 ± 0.02 s while no pulsations with a pulse fraction greater than 18 per cent (at 95 per cent confidence level) in 0.2–12 keV energy band are detected in SAX J1452.8−5949 . The spin period of SAX J1324.4−6200 is found to be increasing on a time-scale of which would suggest that the accretor is a neutron star and not a white dwarf. Using subarcsec spatial resolution of the Chandra telescope, possible counterparts are seen for both sources in the near-infrared images obtained with the son of infrared spectrometer and array camera (SOFI) instrument on the New Technology Telescope. The X-ray and near-infrared properties of SAX J1324.4−6200 suggest it to be a persistent high-mass accreting X-ray pulsar at a distance ≤8 kpc . We identify the near-infrared counterpart of SAX J1452.8−5949 to be a late-type main-sequence star at a distance ≤10 kpc, thus ruling out SAX J1452.8−5949 to be a high-mass X-ray binary. However, with the present X-ray and near-infrared observations, we cannot make any further conclusive conclusion about the nature of SAX J1452.8−5949 .en
dc.language.isoenen
dc.publisherBlackwell Publishing for the RASen
dc.relation.urihttp://adsabs.harvard.edu/abs/2009MNRAS.tmp..298Ken
dc.relation.urihttp://arxiv.org/abs/0809.1268en
dc.relation.urihttp://dx.doi.org/10.1111/j.1365-2966.2009.14438.xen
dc.rights2009 The Royal Astronomical Societyen
dc.titleChandra and XMM-Newton observations of the low-luminosity X-ray pulsators SAX J1324.4-6200 and SAX J1452.8-5949en
dc.typeArticleen
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