Table 4

Spectral fit results from the power-law fits to the H.E.S.S. data.

Source Emin Emax E0 N0 Γ
HESS [TeV] [TeV] [TeV] [cm-2 s-1 TeV-1]
J1534−571 0.42 61.90 1.40 (1.29 ± 0.12stat ± 0.39syst) × 10−12 2.51 ± 0.09stat ± 0.20syst
J1614−518 0.32 38.31 1.15 (5.86 ± 0.34stat ± 1.76syst) × 10−12 2.42 ± 0.06stat ± 0.20syst
J1912+101 0.68 61.90 2.25 (4.82 ± 0.43stat ± 1.45syst) × 10−13 2.56 ± 0.09stat ± 0.20syst
Source N0,1 TeV energy flux (1 − 10 TeV)
HESS [cm-2 s-1 TeV-1] [erg cm-2 s-1]
J1534−571 (2.99 ± 0.30stat ± 0.90syst) × 10−12 (6.5 ± 0.7stat ± 2.0syst) × 10−12
J1614−518 (8.33 ± 0.49stat ± 2.50syst) × 10−12 (2.0 ± 0.2stat ± 0.6syst) × 10−11
J1912+101 (3.89 ± 0.45stat ± 1.17syst) × 10−12 (8.1 ± 0.7stat ± 2.4syst) × 10−12

Notes: Both statistical and systematic errors are given for the fit parameters. The systematic uncertainties result from deviations from the nominal parameters of the simulations of the instrument, nonoptimized observation strategy, and the large size of the sources, which lead to substantial susceptibility of the spectral results to potential errors in the background estimation (see Sect. 2.2.2), and are estimated to 30% for N0 and energy flux and to 0.2 for Γ, respectively.To simplify a comparison between the sources, the normalization at 1 TeV, N0,1 TeV, and the energy flux from 1 TeV to 10 TeV are given as well.

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