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X-Ray Observations of XTE J1550-564 During the Decay of the 2000 Outburst - I. Chandra and RXTE Energy Spectra | | John A. Tomsick
; Stephane Corbel
; Philip Kaaret
; | | Date: |
22 May 2001 | | Subject: | astro-ph | | Affiliation: | CASS/UCSD), Stephane Corbel (Universite Paris VII and Service d’Astrophysique, CEA Saclay) and Philip Kaaret (Harvard-Smithsonian CfA | | Abstract: | We report on the evolution of the X-ray energy spectrum for the black hole candidate (BHC) X-ray transient XTE J1550-564 during the decay of the 2000 outburst. The Rossi X-ray Timing Explorer (RXTE) and Chandra observations span nearly five orders of magnitude in luminosity. The RXTE spectra are dominated by a power-law component and a comparatively weak soft component was also detected for the first two observations. The source made a transition to the canonical hard state near a luminosity of 9E36 erg/s over several observations as evidenced by a drop in the flux of the soft component in the RXTE energy band and a hardening of the power-law component to a photon index near 1.6. The power-law did not exhibit this behavior for the previous XTE J1550-564 outburst. For some observations, we detect a high energy cutoff and find that the cutoff is more significant and at lower energy during the transition than in the hard state. The cutoff in the hard state is at higher energy than has been seen for most previous accreting BHCs. The Chandra spectrum provides evidence for spectral evolution after the hard state transition. It is well, but not uniquely, described by a power-law with a photon index of 2.30^{+0.41}_{-0.48} (90% confidence) and interstellar absorption. Advection-dominated accretion flow models predict gradual spectral softening as the luminosity drops, but our observations do not allow us to determine if the spectral evolution is gradual or sudden. The lowest luminosity we measure for XTE J1550-564 with Chandra is 5E32 erg/s (0.5-7 keV, for a distance of 4 kpc). Although this is probably not the true quiescent luminosity, it represents a useful upper limit on this quantity. | | Source: | arXiv, astro-ph/0105394 | | Services: | Forum | Review | PDF | Favorites | |
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