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Table 2

Compilation of TeV γ-ray sources with pulsar associations (i.e. PWN or associated Halos), together with estimated electron energy densities within the emission region (see notes below and text for details).

Name ATNF name log10 Ė τc Distance Size log10ETotal log10εe(Ė) log10εe(Lγ)
(erg/s) (kyr) (kpc) (pc) (erg) (eV/cm3) (eV/cm3)
Geminga J0633+1746 34.51 342 0.25(1) 16.2 47.5 − 0.3
                     
B0656+14 B0656+14 34.58 111 0.29(2) 16.2 47.1 − 0.8
                     
CTA 1 J0007+7303 35.65 13.9 1.4 10.0 47.3 0.0
                     
J1858+020 J1857+0143 35.65 71.0 5.8 11.9 48.0 0.5
                     
J1834-087 B1830-08 (2) 35.76 147 4.5 25.7 48.4 − 0.1
                     
J1832-085 B1830-08 (1) 35.76 147 4.5 4.0 48.4 2.4
                     
J1026-582 J1028-5819 35.92 90.0 2.3 8.0 48.4 1.4
                     
J1718-385 J1718-3825 36.11 89.5 3.6 10.9 48.6 1.2
                     
J1303-631 J1301-6305 36.23 11.0 6.7 31.1 47.8 − 1.0
                     
J1809-193 (2) J1809-1917 36.26 51.3 3.5 37.7 48.5 − 0.5
                     
J1804-216 B1800-21 36.34 15.8 4.4 28.7 48.0 − 0.6
                     
J1119-614 J1119-6127 36.36 1.61 8.4 21.1 47.1 − 1.2
                     
J1018-589A J1016-5857 (1) 36.41 21.0 8.0 4.0 48.2 2.2
                     
J1018-589B J1016-5857 (2) 36.41 21.0 8.0 31.7 48.2 − 0.5
                     
J1825-137 B1823-13 36.45 21.4 3.9 48.3 48.3 − 1.0
                     
J1908+063 J1907+0602 36.45 19.5 3.2 41.1 48.2 − 0.9
                     
J1356-645 J1357-6429 36.49 7.31 2.5 15.2 47.9 0.0
                     
J1708-443 B1706-44 36.53 17.5 2.6 19.2 48.3 0.2
                     
J1641-462 J1640-4631 (2) 36.64 3.35 12.8 14.0 47.7 0.0
                     
J1640-465 J1640-4631 (1) 36.64 3.35 12.8 37.7 47.7 − 1.3
                     
J1857+026 J1856+0245 36.66 20.6 9.0 61.9 48.5 − 1.2
                     
J1418-609 J1418-6058 36.69 10.3 5.0(3) 14.2 48.2 0.5
                     
J1837-069 J1838-0655 36.74 22.7 6.6 61.9 48.6 − 1.0
                     
J1809-193 (1) J1811-1925 36.81 23.3 5.0 52.8 48.7 − 0.8
                     
J0835-455 B0833-45 36.84 11.3 0.3 4.4 48.4 2.2
                     
J1846-029 J1846-0258 36.91 0.73 5.8 3.0 47.3 1.6
                     
J1849-000 J1849-0001 36.99 42.9 7.0(4) 16.6 49.1 1.2
                     
J1420-607 J1420-6048 37.00 13.0 5.6 11.9 48.6 1.1
                     
J1023-575 J1023-5746 37.04 4.60 8.0(5) 35.0 48.2 − 0.7
                     
J1930+188 J1930+1852 37.08 2.89 7.0 9.0 48.0 0.9
                     
J1616-508 J1617-5055 37.20 8.13 6.8 42.3 48.6 − 0.5
                     
J1514-591 B1509-58 37.23 1.56 4.4 16.8 47.9 0.0
                     
3C58 J0205+6449 37.43 5.37 2.0(6) 5.0 48.7 2.3
                     
J1833-105 J1833-1034 37.53 4.85 4.1 4.0 48.7 2.7
                     
G0.9+0.1 J1747-2809 37.63 5.31 13.3 7.0 48.9 2.1
                     
J1813-178 J1813-1749 37.75 5.60 4.7 6.0 49.0 2.4
                     
Crab Nebula B0531+21 38.65 1.26 2.0 3.0 49.2 3.6

Notes. The available data on the source candidates were collected from Abdalla et al. (2018b), except for Geminga and B0656+14 (Abeysekara et al. 2017a). HGPS names are used (Abdalla et al. 2018a) except for sources located outside of the HGPS; Geminga, B0656+14, CTA 1, 3C 58, G 0.9+0.1, and the Crab, where instead canonical names are given. The associated pulsar names from the ATNF catalogue (Manchester et al. 2005) are also shown and are numbered in cases where the association is not unique. We note that Ė and τc are the spin down luminosity and characteristic age of the associated pulsar. The sources are sorted by increasing Ė. The estimated distance to the pulsars, which may have large uncertainties, is taken from the ATNF catalogue (Manchester et al. 2005), unless a different reference is provided. The size is the 68% containment radius of the TeV emission. The estimated total energy in electrons and positrons is ETotal = Ėτc. The two estimates of energy densities in electrons and positrons are εe(Ė) and εe (Lγ) (see text in Sect. 3).

References.(1) Halpern & Ruderman (1993); (2) Brisken et al. (2003); (3) Ng et al. (2005); (4) Gotthelf et al. (2011); (5) Rauw et al. (2007); (6) Kothes (2013).

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