Table 1
HGPS sources considered as firmly identified pulsar wind nebulae in this paper.
| HGPS name | ATNF name | Canonical name | lg Ė | τc | d | PSR offset | Γ | RPWN | L1-10 TeV |
|---|---|---|---|---|---|---|---|---|---|
| (kyr) | (kpc) | (pc) | (pc) | (1033 erg s-1) | |||||
| J1813−1781 | J1813−1749 | 37.75 | 5.60 | 4.70 | <2 | 2.07 ± 0.05 | 4.0 ± 0.3 | 19.0 ± 1.5 | |
| J1833−105 | J1833−1034 | G21.5−0.92 | 37.53 | 4.85 | 4.10 | <2 | 2.42 ± 0.19 | <4 | 2.6 ± 0.5 |
| J1514−591 | B1509−58 | MSH 15−523 | 37.23 | 1.56 | 4.40 | <4 | 2.26 ± 0.03 | 11.1 ± 2.0 | 52.1 ± 1.8 |
| J1930+188 | J1930+1852 | G54.1+0.34 | 37.08 | 2.89 | 7.00 | <10 | 2.6 ± 0.3 | <9 | 5.5 ± 1.8 |
| J1420−607 | J1420−6048 | Kookaburra (K2)5 | 37.00 | 13.0 | 5.61 | 5.1 ± 1.2 | 2.20 ± 0.05 | 7.9 ± 0.6 | 44 ± 3 |
| J1849−000 | J1849−0001 | IGR J18490−00006 | 36.99 | 42.9 | 7.00 | <10 | 1.97 ± 0.09 | 11.0 ± 1.9 | 12 ± 2 |
| J1846−029 | J1846−0258 | Kes 752 | 36.91 | 0.728 | 5.80 | <2 | 2.41 ± 0.09 | <3 | 6.0 ± 0.7 |
| J0835−455 | B0833−45 | Vela X7 | 36.84 | 11.3 | 0.280 | 2.37 ± 0.18 | 1.89 ± 0.03 | 2.9 ± 0.3 | 0.83 ± 0.11* |
| J1837−0698 | J1838−0655 | 36.74 | 22.7 | 6.60 | 17 ± 3 | 2.54 ± 0.04 | 41 ± 4 | 204 ± 8 | |
| J1418−609 | J1418−6058 | Kookaburra (Rabbit)5 | 36.69 | 10.3 | 5.00 | 7.3 ± 1.5 | 2.26 ± 0.05 | 9.4 ± 0.9 | 31 ± 3 |
| J1356−6459 | J1357−6429 | 36.49 | 7.31 | 2.50 | 5.5 ± 1.4 | 2.20 ± 0.08 | 10.1 ± 0.9 | 14.7 ± 1.4 | |
| J1825−13710 | B1823−13 | 36.45 | 21.4 | 3.93 | 33 ± 6 | 2.38 ± 0.03 | 32 ± 2 | 116 ± 4 | |
| J1119−614 | J1119−6127 | G292.2−0.511 | 36.36 | 1.61 | 8.40 | <11 | 2.64 ± 0.12 | 14 ± 2 | 23 ± 4 |
| J1303−63112 | J1301−6305 | 36.23 | 11.0 | 6.65 | 20.5 ± 1.8 | 2.33 ± 0.02 | 20.6 ± 1.7 | 96 ± 5 | |
Notes. The sources are sorted by decreasing Ė. lg Ė stands for log10 (Ė∕erg s-1), τc is the pulsar characteristic age, d is the pulsar distance, RPWN is the 1-sigma Gaussian extension and L1−10 TeV is the TeV luminosity. The pulsar distances are printed uniformly here, but their uncertainties might often be larger or not available; see ATNF Catalogue references (http://www.atnf.csiro.au/people/pulsar/psrcat/) for detailed information. The limits are 2-sigma limits (see Sect. 2.3).
The luminosity of Vela X is calculated as described in Sect. 2.3.
References. Previous publications on these sources: (1) Funk et al. (2007); (2) Djannati-Ataï et al. (2008); (3) Aharonian et al. (2005b); (4) Acciari et al. (2010); (5) Aharonian et al. (2006e); (6) Terrier et al. (2008); (7) Aharonian et al. (2006a); (8) Gotthelf & Halpern (2008); (9) Renaud et al. (2008); (10) Aharonian et al. (2005c); (11) Acero et al. (2013); (12) H.E.S.S. Collaboration (2012a).
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