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Table 1

Main properties of the observed subdwarf binaries and results of Swift/XRT observations.

Name Period Distance NH MC Companiona Net exposure time Count rateb LXc
(days) (kpc) (1020 cm-2) (M⊙) (s) (ct s-1) (erg s-1)
PG 1043+760 0.12 0.66 3.5  >0.1d WD 5401  <3.8  ×  10-3  <7.3  ×  1030
PG 1432+159 0.22 0.8 1.4 1.49–4.6 NS/BH 3390  <3.8  ×  10-3  <9.8  ×  1030
PG 2345+318 0.24 0.9 4.4 ...e WD 3804  <4.0  ×  10-3  <1.5  ×  1031
HE 0532-4503 0.27 2.8 3.3 2.08–3.94 NS/BH 4729  <2.3  ×  10-3  <7.8  ×  1031
CPD -64 481 0.28 0.21 4.3 0.38–1.04 WD 4572  <3.8  ×  10-3  <7.9  ×  1029
PG 1101+249 0.35 0.39 1.0 1.09–2.44 WD/NS/BH 5263  <2.8  ×  10-3  <1.7  ×  1030
PG 1232-136 0.36 0.57 3.4  >6 BH 5589  <1.8  ×  10-3  <2.6  ×  1030
GD 687 0.38 1.1 2.0 0.50–0.93 WD 5149  <2.1  ×  10-3  <1.1  ×  1031
HE 0929-0424 0.44 1.9 3.0 1.18–2.7 WD/NS/BH 5566  <2.0  ×  10-3  <3.2  ×  1031
PG 1743+477 0.52 1 2.5  >1.66 NS/BH 3342  <4.3  ×  10-3  <1.8  ×  1031
PG 0101+039 0.57 0.33 2.5 0.52–0.92 WD 4851  <2.3  ×  10-3  <1.0  ×  1030
TON S 183 0.83 0.54 1.2 0.63–1.33 WD 4980  <2.1  ×  10-3  <2.5  ×  1030

Notes. 

(a)

WD = white dwarf, NS = neutron star, BH = black hole.

(b)

3σ upper limit in the 0.3–10 keV energy range.

(c)

In the 0.3–10 keV range, corrected for the absorption.

(d)

The presence of a white dwarf in this system with high inclination and short period is suggested by the non-detection of a variable reflection component in the light curve (Maxted et al. 2004).

(e)

This sdB does not rotate synchronously, but the eclipse observed in this system indicates the presence of a white dwarf companion (Green et al. 2004).

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