Table 5
Flux and luminosity upper limits (95% CL) for regions around pulsars without detected PWN.
| ATNF name | lg Ė | τc | d | θpred | θint | Significance | F>1 TeV | L1-10 TeV |
|---|---|---|---|---|---|---|---|---|
| (kyr) | (kpc) | (deg) | (deg) | (σ) | (10−12 cm−2 s−1) | (1033 erg s-1) | ||
| J1400−6325 | 37.71 | 12.7 | 7.00 | 0.150 | 0.2 | 1.4 | <0.41 | <8.3 |
| J1124−5916 | 37.08 | 2.85 | 5.00 | 0.137 | 0.2 | 1.0 | <0.27 | <2.8 |
| J1410−6132 | 37.00 | 24.8 | 15.6 | 0.127 | 0.2 | 2.8 | <0.53 | <54 |
| J1935+2025 | 36.67 | 20.9 | 6.21 | 0.29 | 0.4 | 1.9 | <0.88 | <14 |
| J1112−6103 | 36.65 | 32.7 | 12.2 | 0.21 | 0.4 | 3.7 | <1.0 | <62 |
| J1801−2451 | 36.41 | 15.5 | 5.22 | 0.30 | 0.4 | 1.1 | <0.56 | <6.3 |
| J1837−0604 | 36.30 | 33.8 | 6.41 | 0.42 | 0.4 | 9.5 | <2.1 | <36 |
| J1341−6220 | 36.15 | 12.1 | 11.1 | 0.129 | 0.2 | 2.6 | <0.46 | <24 |
| J1055−6028 | 36.08 | 53.5 | 15.5 | 0.25 | 0.4 | 1.1 | <0.70 | <70 |
| J1934+2352 | 35.96 | 21.6 | 11.6 | 0.175 | 0.2 | 1.6 | <1.1 | <64 |
| J1932+2220 | 35.88 | 39.8 | 10.9 | 0.29 | 0.4 | –0.9 | <0.55 | <27 |
| J1702−4310 | 35.80 | 17.0 | 5.14 | 0.35 | 0.4 | 0.9 | <0.59 | <6.5 |
| J1413−6141 | 35.75 | 13.6 | 10.1 | 0.161 | 0.2 | 2.8 | <0.54 | <23 |
| J1909+0749 | 35.65 | 24.7 | 9.48 | 0.24 | 0.4 | 0.9 | <0.41 | <15 |
| J1815−1738 | 35.59 | 40.4 | 8.78 | 0.37 | 0.4 | 8.9 | <2.1 | <68 |
| J1646−4346 | 35.56 | 32.5 | 5.79 | 0.48 | 0.4 | –2.0 | <0.27 | <3.8 |
| J1850−0026 | 35.52 | 67.5 | 11.1 | 0.44 | 0.4 | 3.7 | <0.91 | <46 |
| J1907+0918 | 35.51 | 38.0 | 7.79 | 0.40 | 0.4 | 2.7 | <0.61 | <15 |
| J1406−6121 | 35.34 | 61.7 | 8.15 | 0.56 | 0.4 | 4.4 | <3.3 | <91 |
| J1412−6145 | 35.08 | 50.6 | 7.82 | 0.51 | 0.4 | 5.0 | <3.0 | <75 |
| J1550−5418 | 35.00 | 1.41 | 4.00 | 0.29 | 0.4 | 1.0 | <0.47 | <3.1 |
| J1841−0524 | 35.00 | 30.2 | 5.34 | 0.53 | 0.4 | 20.9 | <7.3 | <86 |
Notes. In addition to the table variables explained in Table 1, θpred is the predicted PWN extension (including offset), θint is the correlation radius of the map where the limit is taken from, and F>1 TeV is the actual flux limit (see Sect. 2.3 for details). In the cases of high significance, the pulsar coincides with a TeV source that is not considered the PWN.
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