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Table A.1.

Summary of VHE gamma-ray data sets used here.

Data set Start End χ2(dof) α ζ Ref.
HEGRA (IACT) 1997 2002 18(15) 1.197 ± 0.005 (1)
H.E.S.S. (IACT) 2003 2005 24(10) 1.065 ± 0.005 (2)
MAGIC (IACT) 2009 2011 11(13) 0.896 ± 0.006 (3)
VERITAS (IACT) 2009 2013 9(11) 1.038 ± 0.002 (4)
HAWC (WCD) 6/2015 12/2017 7(8) 1.093 ± 0.003 (5)
MAGIC (VLZA) 2014 2018 2(6) 0.59 ± 0.25 1.09 ± 0.02 (6)
Tibet ASγ (EAS, WCD) 2014 2017 4(9) 0.32 ± 0.15 1.06 ± 0.02 (7)
VERITAS (flare) 03/2013 03/2013 13(13) 0.42 ± 0.17 1.09 ± 0.01 (8)
H.E.S.S. II (flare) 03/2013 03/2013 17(31) 0.68 ± 0.3 0.96 ± 0.01 (9)
H.E.S.S. II (IACT) 11/2013 1/2014 93(37) 1.100 ± 0.007 (10)
LHAASO (EAS, WCD) 2019 2020 11(16) 0.56 ± 0.06 0.932 ± 0.006 (11)

Notes. Listed data sets include imaging air Cherenkov telescopes’ (IACTs) observations as well as data taken with extended air shower front sampling (EAS) arrays with scintillators or water Cherenkov detectors (WCD). By observing sources with IACTs at very large zenith angles (VLZA) between 70° and 80°, the collection area at large energies beyond 10 TeV is substantially increased. The uncertainty on α is given for a 90 % confidence level and has been estimated from the discrete sampled values of α. For some data sets the χ2 curve is under-sampled while for others, the maximum range of α is not sufficient to cover the confidence interval.

Reference. (1) Aharonian et al. (2004), (2) Aharonian et al. (2006), (3) Aleksić et al. (2015), (4) Wells (2019), (5) Abeysekara et al. (2019), (6) MAGIC Collaboration (2020), (7) Amenomori et al. (2019), (8) Aliu et al. (2014), (i) H. E. S. S. Collaboration (2014), (9) Holler et al. (2015), Holler (2014), (10) LHAASO Collaboration (2021).

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