Table 6
asurv fit results.
RPWN (Ė ) | RPWN (τc ) | L1−10 TeV (Ė ) | L1−10 TeV (τc) | S(Ė) | dP-P(εTeV) | dP-P(Ė), | dP-P(τc) | |
---|---|---|---|---|---|---|---|---|
p-value | 0.012 | 0.047 | 0.010 | 0.13 | 0.0013 | 0.0004 | 0.035 | 0.0086 |
σlg Y | 0.32 | 0.39 | 0.83 | 0.91 | 0.28 | 0.18 | 0.49 | 0.42 |
p0 | 1.48 ± 0.20 | 0.38 ± 0.22 | 33.22 ± 0.27 | 34.1 ± 0.4 | 30.62 ± 0.13 | 1.97 ± 0.16 | 1.07 ± 0.25 | − 0.9 ± 0.5 |
p1 | − 0.65 ± 0.20 | 0.55 ± 0.23 | 0.59 ± 0.21 | − 0.46 ± 0.36 | 0.81 ± 0.14 | 0.52 ± 0.07 | − 0.75 ± 0.29 | 1.4 ± 0.5 |
Notes. p0 and p1 relate to Eq. (7). The p-value is calculated after the Cox proportional hazards model. The fit used (withinasurv) is the “EM algorithm”. P is given in 0.1 s , Ṗ in 10−13 s s-1, Ė in 1036 erg s-1, and τc in kyr . RPWN is given in pc , L1−10 TeV in erg s-1 , S in erg s-1 pc−2. The 2D pulsar-PWN offset dP-P is given in parsecs, and εTeV = L1−10 TeV∕Ė is the apparent TeV efficiency.
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