Table 4
Estimates of the spin-down energy of the putative pulsar PS1 based on empirical relations between Ė and the X-ray emission of the pulsar and its PWN.
| Relation | Ref. | Notes | Ė (erg s−1) |
|---|---|---|---|
| 1) log Lpsr = 1.34 log Ė − 15.30 | (a) | Lpsr: nonthermal pulsar luminosity in (2.0–10.0) keV | 9.7 × 1036 |
2)  |
(b) | Γpsr: keV photon index of the pulsar. Ė40 = Ė∕(1040 erg s−1) | 1.6 × 1037 |
3)  |
(c) |  : upper limit of the pulsar luminosity in (0.5–8.0) keV |
>1.7 × 1035 |
| 4) log Lpwn = 1.39 log Ė − 16.6 | (d) | Lpwn: PWN luminosity in (0.2–4.0) keV | 2.5 × 1036 |
5)  |
(b) | Γpwn: keV photon index of the PWN. Ė40 = Ė∕(1040 erg s−1) | 1.8 × 1037 |
6)  |
(e) |  : upper limit of the PWN luminosity in (0.5–8.0) keV |
>5.1 × 1036 |
Notes. For the photon indexes of PS1 and G29.4+0.1 we used the results of Sects. 3.2 and 3.3, respectively: Γpwn = 1.87 and Γpsr = 1.35. Luminosities in the different spectral ranges were calculated from the best-fit power-law models considering a distance of 6.5 kpc.
References. (a) Possenti et al. (2002), (b) Gotthelf (2003), (c) Kargaltsev & Pavlov (2008), (d) Seward & Wang (1988), and (e) Kargaltsev et al. (2013).
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