2004MNRAS.354..666J


Query : 2004MNRAS.354..666J

2004MNRAS.354..666J - Mon. Not. R. Astron. Soc., 354, 666-674 (2004/November-1)

Optical and X-ray observations of the neutron star soft X-ray transient XTE J1709-267.

JONKER P.G., GALLOWAY D.K., McCLINTOCK J.E., BUXTON M., GARCIA M. and MURRAY S.

Abstract (from CDS):

In this paper we report on the discovery of the optical counterpart to the neutron star soft X-ray transient (SXT) XTE J1709-267 at an R-band magnitude of R= 20.5±0.1 and 22.24±0.03, in outburst and quiescence, respectively. We further report the detection of type I X-ray bursts in RXTE data obtained during an outburst of the source in 2002. These bursts show a precursor before the onset of the main burst event, reminiscent of photospheric radius expansion bursts. Sifting through the archival RXTE data for the burster 4U 1636-53, we found a nearly identical burst with precursor in 4U 1636-53. A comparison of this burst to true photospheric radius expansion bursts in 4U 1636-53 leads us to conclude that these bursts-with-precursor do not reach the Eddington limit. Nevertheless, from the burst properties we can derive that the distance to XTE J1709-267 is consistent with the distance of the Globular Cluster NGC 6293. We further report on the analysis of a 22.7 ks observation of XTE J1709-267 obtained with the Chandra satellite when the source was in quiescence. We found that the source has a soft quiescent spectrum which can be fit well by an absorbed black body or neutron star atmosphere model. A power law contributes less than ∼20 per cent to the 0.5-10 keV unabsorbed flux of (1.0±0.3)x10–13 erg/cm2/s. This flux is only slightly lower than the flux measured right after the outburst in 2002. This is in contrast to the recent findings for MXB 1659-29, where the quiescent source flux decreased gradually by a factor of ∼7-9 over a period of 18 months. Finally, we compared the fractional power-law contribution to the unabsorbed 0.5-10 keV luminosity for neutron star SXTs in quiescence for which the distance is well-known. We find that the power-law contribution is low only when the source quiescent luminosity is close to ∼1-2x1033 erg/s. Both at higher and lower values the power-law contribution to the 0.5-10 keV luminosity increases. We discuss how models for the quiescent X-ray emission can explain these trends.

Abstract Copyright: 2004 RAS

Journal keyword(s): accretion, accretion discs - binaries: general - stars: individual: XTE J1709-267 - stars: individual: 4U 1636-53 - stars: neutron - X-rays: binaries

CDS comments: Table 3, figure 4: stars 1 to 6 are not identified in SIMBAD, except No. 3 = USNO-B1.0 0633-00521091 and No. 5 = USNO-B1.0 0633-00520981

Simbad objects: 30

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Number of rows : 30
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 NGC 104 GlC 00 24 05.359 -72 04 53.20     4.09     ~ 4158 0
2 V* BW Ant LXB 09 29 20.19 -31 23 03.2   18.50 18.63     ~ 194 0
3 NGC 5139 GlC 13 26 47.28 -47 28 46.1           ~ 3677 0
4 V* V822 Cen LXB 14 58 21.9347842080 -31 40 07.515432768 11.95 12.85 12.8     K3-K7V 555 0
5 V* QX Nor LXB 16 12 43.0 -52 25 26           ~ 946 1
6 M 80 GlC 16 17 02.41 -22 58 33.9           ~ 780 0
7 V* V801 Ara LXB 16 40 55.5976953528 -53 45 04.948107156 17.50 18.20 17.5   17.07 ~ 921 0
8 MXB 1658-298 LXB 17 02 06.54 -29 56 44.1 18.35 18.75 18.3     ~ 381 0
9 USNO-B1.0 0633-00520757 * 17 09 26.8309332024 -26 39 11.661230628     15.4     ~ 1 0
10 USNO-B1.0 0633-00520833 * 17 09 27.5211665784 -26 39 05.633690724   18.5 18.1     ~ 1 0
11 USNO-B1.0 0633-00520873 * 17 09 28.0126507608 -26 39 35.532378072   19.2 19.4     ~ 1 0
12 USNO-B1.0 0633-00520981 * 17 09 29.1067428168 -26 39 31.942697400   18.1 17.7     ~ 1 0
13 USNO-B1.0 0633-00520994 PM* 17 09 29.3501807616 -26 39 03.531519036     19.6     ~ 1 0
14 USNO-B1.0 0633-00521064 * 17 09 29.9529765000 -26 39 32.171006088   18.4 17.7     ~ 1 0
15 USNO-B1.0 0633-00521091 * 17 09 30.2775403752 -26 39 29.613081024   20.8 19.8     ~ 1 0
16 RX J1709.5-2639 LXB 17 09 30.5 -26 39 26           ~ 130 0
17 USNO-B1.0 0633-00521161 * 17 09 31.1957673792 -26 39 10.693019376   20.4 20.7     ~ 1 0
18 USNO-B1.0 0633-00521300 * 17 09 32.6361075408 -26 39 31.441278816   18.3 18.0     ~ 1 0
19 NGC 6293 GlC 17 10 10.42 -26 34 54.2           ~ 309 0
20 KS 1731-260 LXB 17 34 13.46 -26 05 18.6       22.8 20.9 ~ 437 0
21 NGC 6397 GlC 17 40 42.09 -53 40 27.6     5.17     ~ 2103 0
22 Cl Terzan 5 Cl* 17 48 05.00 -24 46 48.0           ~ 948 1
23 NAME TER 5 X-1 LXB 17 48 05.225 -24 46 47.66           ~ 229 1
24 NGC 6440 GlC 17 48 52.67 -20 21 34.5           ~ 592 0
25 SAX J1808.4-3658 LXB 18 08 27.58 -36 58 43.9           ~ 1051 0
26 V* V4722 Sgr LXB 18 10 44.47 -26 09 01.2   21.5     18.449 ~ 99 0
27 X Aql X-1 LXB 19 11 16.0571313336 +00 35 05.868232692           ~ 1186 1
28 V* LZ Aqr LXB 21 23 14.54 -05 47 52.9 15.90 16.78 16.8     ~ 154 0
29 M 30 GlC 21 40 22.12 -23 10 47.5     7.10     ~ 1121 0
30 SAX J2224.9+5421 X 22 24 52 +54 21.9           ~ 22 1

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