Table 6.
Results of the best-fit fully ionized neutron star atmosphere model with a Gaussian absorption line (per observation and camera).
| obsid |  |
d.o.f | NHP | NH | Teff | d | ϵ | σ | EW | fXa |
|---|---|---|---|---|---|---|---|---|---|---|
| (%) | (1020 cm−2) | (105 K) | (pc) | (eV) | (eV) | (eV) | ||||
| pn | ||||||||||
| 2012 | 1.19 | 184 | 4 | 3.0(4) |
 |
116(8) |
 |
 |
 |
6.622(23) |
| 201 | 0.90 | 204 | 84 |
 |
5.83(5) | 130(5) |
 |
 |
 |
6.965(16) |
| 301 | 1.07 | 195 | 25 | 2.9(3) | 5.68(7) | 116(6) |
 |
 |
 |
6.650(18) |
| 401 | 0.97 | 195 | 62 | 2.2(3) | 5.85(7) |
 |
 |
 |
 |
6.912(21) |
| 501 | 1.01 | 196 | 45 |
 |
5.92(7) | 137(7) |
 |
 |
 |
6.909(21) |
| MOSb | ||||||||||
| 2012 | 1.05 | 181 | 30 | 2.2(5) |
 |
 |
 |
 |
 |
6.42(3) |
| 201 | 1.11 | 199 | 14 | 1.81(4) |
 |
 |
 |
 |
 |
 |
| 301 | 0.98 | 187 | 59 | 3.3(4) | 5.70(7) |
 |
 |
 |
 |
6.081(25) |
| 401 | 1.08 | 185 | 23 | 1.9(5) | 5.72(9) |
 |
 |
 |
 |
6.682(29) |
| 501 | 1.12 | 188 | 12 | 1.8(6) |
 |
 |
 |
 |
 |
7.02(3) |
| EPICc | ||||||||||
| 2012 | 1.17 | 370 | 1.3 |
 |
5.78(6) | 124(5) |
 |
 |
 |
6.546(18) |
| 201 | 1.02 | 408 | 36 |
 |
5.81(4) |
 |
 |
 |
 |
6.976(11) |
| 301 | 1.03 | 387 | 31 | 3.03(23) | 5.71(5) | 129(6) |
 |
 |
 |
6.471(19) |
| 401 | 1.03 | 385 | 34 | 2.03(28) | 5.79(5) | 129(5) |
 |
 |
 |
6.893(22) |
| 501 | 1.10 | 389 | 8 | 2.18(28) | 5.83(5) |
 |
 |
 |
 |
6.974(16) |
| Multi-epoch fitsd | ||||||||||
| pn | 1.04 | 994 | 17 | 2.45(14) | 5.81(3) |
 |
 |
87(4) |
 |
6.842(9) |
| MOS | 1.13 | 1738 | < 1 |
 |
 |
 |
 |
93(4) |
 |
7.016(13) |
| EPIC | 1.15 | 1202 | < 1 |
 |
 |
 |
 |
 |
 |
6.805(6) |
Notes. Errors are 1σ confidence levels. The model fitted to the data in XSPEC is tbabs(nsa-gauss), assuming a magnetic field intensity of B = 1013 G and canonical neutron star mass and radius. The effective temperature is given at the source’s rest frame (unredshifted).
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