Table 7.
Results of the best-fit partially ionized neutron star atmosphere model with a Gaussian absorption line (per observation and camera).
| obsid |  |
d.o.f. | NHP | NH | Teff | d | Rem | ϵ | σ | EW | fXa |
|---|---|---|---|---|---|---|---|---|---|---|---|
| (%) | (1020 cm−2) | (105 K) | (3σ, pc) | (km) | (eV) | (eV) | (eV) | ||||
| pn | |||||||||||
| 2012 | 1.18 | 185 | 5 | 4.07(17) |
 |
< 107 |
 |
 |
89(5) |
 |
6.581(23) |
| 201 | 0.88 | 205 | 89 |
 |
 |
< 120 |
 |
 |
 |
 |
 |
| 301 | 1.07 | 196 | 25 |
 |
 |
< 105 |
 |
390(6) | 84(4) |
 |
6.589(18) |
| 401 | 0.96 | 196 | 65 |
 |
 |
< 110 |
 |
 |
 |
50(5) |
 |
| 501 | 1.00 | 197 | 50 |
 |
 |
113(6) |
 |
 |
 |
 |
 |
| MOSb | |||||||||||
| 2012 | 1.06 | 182 | 29 | 3.4(4) |
 |
< 117 |
 |
 |
87(8) |
 |
 |
| 201 | 1.10 | 200 | 16 | 3.12(29) |
 |
< 110 |
 |
 |
104(6) |
 |
 |
| 301 | 0.98 | 188 | 54 |
 |
 |
< 105 |
 |
396(7) | 82(4) |
 |
6.072(25) |
| 401 | 1.07 | 186 | 25 |
 |
 |
< 110 |
 |
 |
 |
 |
 |
| 501 | 1.12 | 189 | 12 |
 |
 |
< 110 |
 |
 |
 |
 |
6.602(27) |
| EPICc | |||||||||||
| 2012 | 1.16 | 371 | 1.8 |
 |
 |
< 110 |
 |
 |
 |
 |
6.419(18) |
| 201 | 1.01 | 409 | 44 | 3.50(16) |
 |
< 110 |
 |
 |
 |
 |
6.391(10) |
| 301 | 1.03 | 388 | 31 | 4.11(10) | 6.18(7) | < 105 |
 |
392(4) | 83.2(2.5) |
 |
 |
| 401 | 1.02 | 386 | 39 |
 |
 |
< 110 | 8.7(6) |
 |
91(6) | 58(4) | 6.769(16) |
| 501 | 1.10 | 390 | 10 |
 |
 |
< 110 |
 |
 |
 |
62(3) |
 |
| Multi-epoch fitsd | |||||||||||
| pn | 1.03 | 995 | 26 | 4.85(14) |
 |
 |
 |
 |
 |
 |
 |
| MOS | 1.13 | 1739 | < 1 |
 |
 |
< 105 |
 |
 |
 |
 |
 |
| EPIC | 1.14 | 1203 | < 1 | 3.82(10) |
 |
< 105 |
 |
 |
 |
 |
 |
Notes. Errors are 1σ confidence levels. The model fitted to the data in XSPEC is tbabs(nsmaxg-gauss), assuming a magnetic field intensity of B = 1013 G and a 1.4 M⊙ neutron star. The effective temperature and radius are given at the source’s rest frame (unredshifted).
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