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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/4888
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dc.contributor.authorYokogawa, J.-
dc.contributor.authorPaul, Biswajit-
dc.contributor.authorOzaki, M.-
dc.contributor.authorNagase, F.-
dc.contributor.authorChakrabarty, D.-
dc.contributor.authorTakeshima, T.-
dc.date.accessioned2012-07-14T06:13:46Z-
dc.date.available2012-07-14T06:13:46Z-
dc.date.issued2000-08-
dc.identifier.citationAstrophysical Journal, 2000, Vol. 539, p191-196en
dc.identifier.issn0004-637X-
dc.identifier.issn1538-4357 (Online)-
dc.identifier.urihttp://hdl.handle.net/2289/4888-
dc.descriptionOpen Accessen
dc.description.abstractThe new transient X-ray pulsar XTE J0111.2-7317 was observed with Advanced Satellite for Cosmology and Astrophysics (ASCA) on 1998 November 18, a few days after its discovery with the proportional counter array on board the Rossi X-ray Timing Explorer. The source was detected at a flux level of 3.6×10-10 ergs cm-2 s-1 in the 0.7-10.0 keV band, which corresponds to the X-ray luminosity of 1.8×1038 ergs s-1, if a distance of 65 kpc for this pulsar in the Small Magellanic Cloud is assumed. Nearly sinusoidal pulsations with a period of 30.9497+/-0.0004 s were unambiguously detected during the ASCA observation. The pulsed fraction is low and slightly energy dependent with an average value of ~27%. The energy spectrum shows a large soft excess below ~2 keV when fitted to a simple power-law-type model. The soft excess is eliminated if the spectrum is fitted to an ``inversely broken power-law'' model, in which photon indices below and above a break energy of 1.5 keV are 2.3 and 0.8, respectively. The soft excess can also be described by a blackbody or a thermal bremsstrahlung when the spectrum above ~2 keV is modeled by a power law. In these models, however, the thermal soft component requires a very large emission zone, and hence it is difficult to explain the observed pulsations at energies below 2 keV. A bright state of the source enables us to identify a weak iron line feature at 6.4 keV with an equivalent width of 50+/-14 eV. Pulse phase-resolved spectroscopy revealed a slight hardening of the spectrum and marginal indication of an increase in the iron line strength during the pulse maximum.en
dc.language.isoenen
dc.publisherIOP Publishing Ltden
dc.relation.urihttp://adsabs.harvard.edu/abs/2000ApJ...539..191Yen
dc.relation.urihttp://arxiv.org/abs/astro-ph/0003251en
dc.relation.urihttp://dx.doi.org/10.1086/309202en
dc.rights2000 The American Astronomical Societyen
dc.subjectStars: Binariesen
dc.subjectMagellanic Cloudsen
dc.subjectX-Rays: Starsen
dc.titleASCA observation of the new transient X-Ray pulsar XTE J0111.2-7317 in the small magellanic clouden
dc.typeArticleen
Appears in Collections:Research Papers (A&A)

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