Table 3
Spectral results for the γ-ray pulsar PSR J1124–5916.
| Source | Phase | Г | d | b | Energy Flux ( > 50 MeV) (10-11 erg cm-2 s-1) | TS |
|---|---|---|---|---|---|---|
| PSR J1124–5916 | ON P1 | –2.134 ± 0.037 | 0.406 ± 0.048 | 0.66 | 50.1 ± 2.3 | 3519 |
| PSR J1124–5916 | ON P2 | –2.421 ± 0.041 | 0.461 ± 0.068 | 0.66 | 46.5 ± 2.7 | 2172 |
| PSR J1124–5916 | TOT Dataset | –2.287 ± 0.021 | 0.38 ± 0.03 | 0.66 | 6.946 ± 0.186 | 6054 |
| PWN | OFF | –1.991 ± 0.145 | 0.79 ± 0.18 | 38 | ||
| PWN | TOT Dataset | –2.061 ± 0.077 | 0.66 ± 0.01 | 49 | ||
Notes. Maximum likelihood spectral fit results for PSR J1124-5916 in on-phase and average-phase analyses, and for our new PWN candidate hosted by G292.0+1.8, in off-phase and average-phase total dataset analyses. The pulsar spectrum is modeled with a sub-exponentially cutoff power law, following the approach applied to significantly curved pulsars in the 4FGL-DR3 catalog (Abdollahi et al. 2022). For each pulsar fit, the integral energy flux for E>50MeV, the low-energy photon index (Γ), the exponential factor (d), and the exponential index (b) are given. The PWN spectrum is well described by a simple power-law model, with the integral energy flux for E>50 MeV, along with the photon index Γ reported. The phased analysis (ON P1, ON P2, and OFF) covers 50 MeV–300 GeV, whereas the full dataset analysis extends over 50 MeV–1 TeV.
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