Chandra observations of the faintest low-mass X-ray binaries

被引:33
作者
Wilson, CA
Patel, SK
Kouveliotou, C
Jonker, PG
van der Klis, M
Lewin, WHG
Belloni, T
Méndez, M
机构
[1] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England
[2] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands
[3] Univ Amsterdam, Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands
[4] MIT, Dept Phys, Cambridge, MA 02138 USA
[5] MIT, Ctr Space Res, Cambridge, MA 02138 USA
[6] Osserv Astron Brera, I-23807 Merate, LC, Italy
[7] SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands
[8] Natl Space Sci & Technol Ctr, Space Sci Res Ctr SD 50, Huntsville, AL 35805 USA
关键词
accretion; accretion disks; binaries : close; X-rays : binaries; X-rays : stars;
D O I
10.1086/377473
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
A group of persistently faint Galactic X-ray sources exist that, based on their location in the Galaxy, high L-X=L-opt, association with X-ray bursts, and absence of low-frequency X-ray pulsations, are thought to be low-mass X-ray binaries (LMXBs). We present results from Chandra observations for eight of these systems: 4U 1708-408, 2S 1711-339, KS 1739-304, SLX 1735-269, GRS 1736-297, SLX 1746-331, 1E 1746.7-3224, and 4U 1812-12. Locations for all these sources, excluding GRS 1736-297, SLX 1746-331, and KS 1739-304 (which were not detected), were improved to 0."6 error circles (90% confidence). Our observations support earlier findings of transient behavior of GRS 1736-297, KS 1739-304, SLX 1746-331, and 2S 1711-339 (which we detect in one of two observations). Energy spectra for 4U 1708-408, 2S 1711-339, SLX 1735-269, 1E 1746.7-3224, and 4U 1812-12 are hard, with power-law indices typically 1.4-2.1, which is consistent with typical faint LMXB spectra.
引用
收藏
页码:1220 / 1228
页数:9
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