Table 6

Parameters of known TeV SNR shells.

HESS source name Identification Dist. Diameter Age Lγ,1 TeV−10 TeV Γγ,PLfit Γγ/Ecutoff Ref.
[kpc] [pc] [kyr] [1033erg s-1] - -/[TeV]
HESS J0852−463 RX J0852.0−4622 0.75 26.2 1.7–4.3 5.7 2.3 1.8/6.7 (1)
HESS J1713−397 RX J1713.7−3946 1 20.2 ≈1 7.2 2.3 2.1/12.9 (2)
HESS J1731−347 G353.6−0.7 3.2/5.2 30.2/49 ≈2.5 8.5/22.4 2.3 (3)
HESS J1442−624 G315.4−2.3 (RCW 86) 2.5 ≈30 ≈1.8 6.3 2.3 1.6/3.5 (4)
HESS J1502−418 SN 1006 (NE) c rowspan="0" c>0 * [0pt]2.2 c rowspan="0" c>0 * [0pt]22.3 c rowspan="0" c>0 * [0pt]≈1 0.46 2.4 c rowspan="0" c>0 * [0pt](5)
HESS J1502−421 SN 1006 (SW) 0.31 2.3

Notes: For each of the sources, diameter and Lγ,1 TeV−10 TeV are calculated based on the parameters quoted in the respective papers. Where power laws with cutoffs better fit the spectra and are used to compute luminosities, the corresponding fit values are also reported. The distance to HESS J1731−347 is debated in the literature (see, e.g., Fukuda et al. 2014; Klochkov et al. 2015); the values reported in the table correspond to the two most probable distance solutions. Flux errors are dominated by their systematic errors of typically 20%, but luminosity errors are dominated by the distance uncertainties and are therefore on the order of 30% or more. Spectral indices have statistical errors of ΔΓ ≈ 0.2 or better. References. (1) Aharonian et al. (2007b); H.E.S.S. Collaboration (2018a); (2) Aharonian et al. (2006c); H.E.S.S. Collaboration (2018c); (3) H.E.S.S. Collaboration (2011); Klochkov et al. (2015); (4) H.E.S.S. Collaboration (2018b); (5) Acero et al. (2010).

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