Table 5.
X-ray fluxes and luminosities of the investigated sources.
| Pulsar | Blackbody (kT = 0.3 keV) |
Power-law (Γ = 1.7) |
||
|---|---|---|---|---|
 |
 |
 |
 |
|
| (10−14 erg s−1 cm−2) | ( 1029 erg s−1) | ( 10−14 erg s−1 cm−2) | ( 1029 erg s−1) | |
| J0340+4130 | 0.46 ± 0.23 | 14.1 ± 7.1 | 1.07 ± 0.58 | 33.4 ± 18.1 |
| J0711–6830 | 0.58 ± 0.32 | 0.10 ± 0.06 | 2.75 ± 1.22 | 0.44 ± 0.21 |
| J0745–5353 | 0.80 ± 0.23 | 3.15 ± 0.90 | 0.92 ± 0.33 | 3.58 ± 1.21 |
| J0942–5552 | 1.38 ± 0.43 | 1.48 ± 0.52 | 0.25 ± 0.30 | 0.23 ± 0.40 |
| J1125–5825 | 1.36 ± 0.48 | 49.3 ± 17.5 | 2.45 ± 1.44 | 88.9 ± 51.2 |
| J1435–5954 | 0.45 ± 0.14 | 6.05 ± 1.3 | 0.59 ± 0.23 | 7.93 ± 3.12 |
| J1535–4114 | 0.31 ± 0.10 | 28.5 ± 6.4 | 0.34 ± 0.10 | 31.2 ± 10.1 |
| J1622–0315 | 0.85 ± 0.24 | 13.2 ± 2.9 | 1.30 ± 0.42 | 20.2 ± 6.5 |
| J1643–1224 | 1.58 ± 0.27 | 10.4 ± 1.8 | 2.23 ± 0.51 | 14.6 ± 3.2 |
| J1831–0952 | 0.41 ± 0.14 | 66.4 ± 22.7 | 2.36 ± 0.40 | 371 ± 60 |
| J1857+0943 | 0.84 ± 0.23 | 13.8 ± 3.4 | 0.54 ± 0.22 | 9.4 ± 4.9 |
| J1926–1314 | 0.20 ± 0.05 | 5.8 ± 1.4 | 0.15 ± 0.11 | 4.3 ± 3.1 |
| J0942–5552 | < 1.21 | < 1.30 | < 2.69 | < 2.90 |
| J0945–4833 | < 0.79 | < 1.16 | < 1.74 | < 2.55 |
| J0954–5430 | < 1.22 | < 2.70 | < 2.65 | < 5.86 |
| J0957–5432 | < 1.57 | < 3.80 | < 3.38 | < 8.19 |
| J1000–5149 | < 0.19 | < 0.03 | < 0.42 | < 0.08 |
| J1003–4747 | < 0.63 | < 1.03 | < 1.39 | < 2.28 |
| J1017–7156 | < 0.49 | < 0.40 | < 1.07 | < 0.87 |
| J1543–5149 | < 0.42 | < 6.65 | < 0.90 | < 14.2 |
| J1725–0732 | < 0.15 | < 0.07 | < 0.32 | < 0.15 |
| J1740–3015 | < 2.96 | < 5.67 | < 6.50 | < 12.4 |
| J1755–0903 | < 0.81 | < 0.51 | < 1.75 | < 1.11 |
Notes. The flux values are based on the EPIC-pn count rates (or limits) and two spectral model assumptions. Funabs represents the unabsorbed X-ray flux whereas LBB and LPL columns represent the X-ray BB and PL luminosities respectively. For the luminosity calculation, distances based on the Yao et al. (2017) electron density model are used. The distance uncertainty is not taken into account for error estimation. For PSR J1831–0952, spectral parameters have been obtained (see Table 6) but here we list the flux derived from typical model parameters for consistency.
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