Table 5
Results of spectral fitting of neutron star atmosphere models (nsa).
| Model | B |  (d.o.f.) |
N H | T eff,1 | T eff,2 | ϵ 1 | E W 1 | ϵ 2 | E W 2 | M ns |
|
|
log (LX) | d |
|
|
||||||||||||||
| (G) | (1021 cm-2) | (105 K) | (105 K) | (keV) | (keV) | (M⊙) | (km) | (km) | (erg s-1) | (kpc) | ||||
|
|
||||||||||||||
| (a) | 0 | 1.92 (169) | 4.85(11) |
|
– | – | – | 1.4 | 13 | – |
|
0.17 | ||
| 1e12 | 1.63 (169) |
|
|
– | – | – | 2 | 18 | – |
|
|
|||
| 1e13 | 1.81 (169) |
|
|
– | – | – | 2.5 | 25 | – |
|
2.58(4) | |||
| (b) | 0 | 2.19 (166) |
|
|
10 | – | – | 1.4⋆ |
|
6 |
|
|
||
| 1e12 | 1.68 (166) |
|
|
|
– | – | 1.4⋆ | 23 | 6 |
|
|
|||
| 1e13 | 1.96 (166) |
|
|
|
– | – | 1.4⋆ | 23 | 6 |
|
|
|||
| (c) | 0 | 1.57 (165) | 4.98(11) |
|
– | – | – | 1.5 | 13 | – |
|
0.12 | ||
| 1e12 | 1.32 (165) |
|
|
– | – | – | 1.9 | 18 | – |
|
|
|||
| 1e13 | 1.89 (165) |
|
|
– | – | – | 0.8 | 11 | – |
|
0.10 | |||
| (d) | 0 | 1.39 (166) | 2.80(3) |
|
|
– | 1.346(15) | 0.3 | 1.4⋆ | 23 |
|
|
|
|
| 1e12 | 1.15 (166) |
|
6(4) |
|
– |
|
0.25 | 1.4⋆ | 23 | 6 | 35(5) |
|
||
| 1e13 | 1.28 (166) |
|
|
|
– |
|
0.2 | 1.4⋆ | 23 | 6 |
|
|
||
| (e) | 0 | 1.08 (165) | 2.9(3) |
|
– |
|
0.07 |
|
0.26 | 1.4⋆ | 13 | – |
|
0.654(6) |
| 1e12 | 1.05 (165) |
|
|
– |
|
0.07 |
|
0.22 | 1.4⋆ | 13 | – |
|
1.997(19) | |
| 1e13 | 1.12 (165) |
|
|
– |
|
0.08 |
|
0.28 | 1.4⋆ | 13 | – |
|
|
|
Notes. Errors are 1σ confidence levels (unconstrained parameters are shown with no errors for illustrative purposes). All tbabs models assume Wilms et al. (2000) abundances. All listed models consist of hydrogen atmospheres. Models: (a) tbabs(nsa); (b) tbabs(nsa+nsa); (c) vphabs(nsa), with best-fit oxygen overabundance of ZO ~ 1.3−1.7 in solar units; (d) tbabs(nsa+nsa+gauss), with fixed Gaussian σ2 = 0.2 keV; (e) tbabs(nsa+gauss+gauss), with fixed Gaussian σ1 = 0.1 keV and σ2 = 0.2 keV.
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