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Title:
X-ray Observation of SWIFT J1753.5-0127 with RXTE & XMM-Newton
Authors:
Sarkar, R.; Chakrabarti, S. K.; Nandi, A.
Affiliation:
AA(Indian Centre for Space Physics, Chalantika 43, Garia Station Rd., 700084, India), AB(Indian Centre for Space Physics, Chalantika 43, Garia Station Rd., 700084, India; S. N. Bose National Center for Basic Sciences, JD-Block, Salt Lake, Kolkata, 700098 India), AC(Indian Centre for Space Physics, Chalantika 43, Garia Station Rd., 700084, India; On deputation from ISRO HQ, Bangalore, 560094, India)
Publication:
OBSERVATIONAL EVIDENCE FOR BLACK HOLES IN THE UNIVERSE: Proceedings of the 2nd Kolkata Conference on Observational Evidence for Black Holes in the Universe held in Kolkata India, 10-15 February 2008 and the Satellite Meeting on Black Holes, Neutron Stars, and Gamma-Ray Bursts held 16-17 February 2008. AIP Conference Proceedings, Volume 1053, pp. 215-218 (2008). (AIPC Homepage)
Publication Date:
10/2008
Origin:
AIP
PACS Keywords:
X-ray binaries, Galactic nuclei , circumnuclear matter, and bulges, X-ray emission spectra and fluorescence
DOI:
10.1063/1.3009485
Bibliographic Code:
2008AIPC.1053..215S

Abstract

The X-ray transient source SWIFT J1753.5-0127 was identified to be a galactic black hole from the results of the analysis of RXTE and XMM-Newton data. We re-analyze the entire observational data made by RXTE and XMM-Newton to quantify the nature of X-ray emission by studying the accreting disk structure. Detailed timing and spectral studies support that the accretion disk was receding away from the compact object as indicated by the diminishing value of the QPO frequency from its highest value ~0.89 Hz to the minimum frequency (detectable). At the same time, the X-ray source remained in the low/hard state tending to go to harder state.
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