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Title:
Chandra Observations of the Bursting X-Ray Transient SAX J1747.0-2853 during Low-Level Accretion Activity
Authors:
Wijnands, Rudy; Miller, Jon M.; Wang, Q. Daniel
Affiliation:
AA(Center for Space Research, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139-4307 .; Chandra Fellow.), AB(Center for Space Research, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139-4307 .), AC(Astronomy Department, University of Massachusetts, Amherst, MA 01003.)
Publication:
The Astrophysical Journal, Volume 579, Issue 1, pp. 422-429. (ApJ Homepage)
Publication Date:
11/2002
Origin:
UCP
ApJ Keywords:
Accretion, Accretion Disks, Stars: Individual: Alphanumeric: SAX J1747.0-2853, Stars: Neutron, X-Rays: Stars
DOI:
10.1086/342788
Bibliographic Code:
2002ApJ...579..422W

Abstract

We present Chandra/ACIS observations of the bursting X-ray transient SAX J1747.0-2853 performed on 2001 July 18. We detected a bright source at the position of R.A. = 17h47m02.60s and decl. = -28°52'58.9" (J2000.0, with a 1 σ error of ~0.7"), consistent with the BeppoSAX and ASCA positions of SAX J1747.0-2853 and with the Ariel V position of the transient GX +0.2-0.2, which was active during the 1970s. The 0.5-10 keV luminosity of the source during our observations was ~3×1035 ergs s-1 (assuming a distance of 9 kpc), demonstrating that the source was in a low-level accretion state. We also report on the long-term light curve of the source as observed with the all-sky monitor on board the Rossi X-Ray Timing Explorer. After the initial 1998 outburst, two more outbursts (in 2000 and 2001) were detected with peak luminosities about 2 orders of magnitude larger than our Chandra luminosity. Our Chandra observation falls between those two outbursts, making the outburst history for SAX J1747.0-2853 complex. Those bright 2000 and 2001 outbursts, combined with the likely extended period of low-level activity between those outbursts, strongly suggest that the classification of SAX J1747.0-2853 as a faint X-ray transient was premature. It might be possible that the other faint X-ray transients can also exhibit bright, extended outbursts that would eliminate the need for a separate subclass of X-ray transients. We discuss our results also in the context of the behavior of X-ray binaries accreting at low levels with luminosities around 1035 ergs s-1, a poorly studied accretion rate regime.
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