Table 3
Best-fit parameters of the X-ray spectra.
| Src-No | Model | NH (1022 cm−2) | Photon index | Temperature | Abundance | x2 (d.o.f.) | Unabsorbed FX (10−14 erg s−1 cm−2) | Unabsorbed LX(*) (ergs−1) |
|---|---|---|---|---|---|---|---|---|
| 320 | tbabs x(apec) |  |
- | >1.32 keV | - | 1.15(10) |  |
1.23 x 1032 |
| tbabs x(bb) |  |
 |
0.950(11) |  |
2.90 x 1031 | |||
| tbabs x (nsa)(**) |  |
log(T): 6.48 K | 0.961(11) |  |
2.11 x 1031 | |||
| 340 | tbabs x(bb+po) |  |
 |
< 0.90 keV | 1.05 (116) |  |
2.80 x 1032 | |
| tbabs x(nsa+po) | <0.05 |  |
 |
0.97 (116) |  |
2.14 x 1032 | ||
| 341 | tbabs x (apec+po) | <0.19 |  |
<0 2 | - | 0.80(24) |  |
3.82 x 1031 |
| 453 | tbabs x(apec+apec) |  |
– |  |
 |
1.07 (58) |  |
1.12 x 1029(***) |
| – |  |
|||||||
| 480 | tbabs x(apec+apec) |  |
– |  |
– | 1.03 (38) |  |
1.37 x 1032 |
 |
||||||||
| tbabs x (bb+po) |  |
 |
<0.66 keV | 0.68(38) |  |
9.01 x 1031 | ||
| 481 | tbabs x (bb) |  |
– |  |
– | 1.08 (30) |  |
3.90 x 1031 |
| tbabs x(nsa) |  |
– |  |
– | 1 09 (30) |  |
8.81 x 1031 | |
| 501 | tbabs x(apec+apec) |  |
– |  |
– | 1.27 (80) |  |
1.49 x 1032 |
 |
||||||||
| tbabs x(nsa+po) |  |
 |
 |
1.43 (81) |  |
1.45 x 1032 |
Notes. Errors are at the 90% confidence level. (*)We assumed a distance of 4.45 kpc to estimate the X-ray luminosity of sources in 47 Tuc (see Sect. 1). (**)The non-magnetic neutron star atmosphere (nsa) model (Zavlin et al. 1996) was applied for the systems that might have a neutron star as their compact object. We assumed a mass and radius of Mns = 1. 4 M⊙ and RNS = 10 km for the neutron star, as was used in the nsa model for the QLMXBs and MSPs spectra (e.g. Bogdanov et al. 2006; Wijnands et al. 2005). (***)For Src-No. 453, we considered the distance of the counterpart, which is a foreground star located at ~200 pc.
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