Multiple accelerated particle populations in the Cygnus Loop with Fermi-LAT

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Table 3

Test statistics and parameters for various spectral models (0.1–100 GeV) using as spatial model the UV map.

Model	TS ^(a)	Spectral model^(b)	Spectral parameters	Energy flux (0.1–100 GeV)
				(10⁻⁵ MeV cm⁻² s⁻¹)
Power Law (PL)	0	E^−p	p = 2.14 ± 0.01	7.15 ± 0.12

Exp. cut-off PL	324		γ = 1.77 ± 0.03	5.31 ± 0.10
Exp. cut-off PL	324		E_cut = 4.1 ± 0.4 GeV	5.31 ± 0.10

LogParabola	418		α = 2.134 ± 0.016	5.44 ± 0.10
LogParabola	418		β = 0.212 ± 0.013	5.44 ± 0.10

PLSuperExpCutoff4	428		γ₀ = 2.140 ± 0.024	5.62 ± 0.12
			d = 0.350 ± 0.023
			b = − 0.40 ± 0.12

Smoothly broken PL	430		p₁ = 2.68 ± 0.07	5.82 ± 0.11
			p₂ = 1.12 ± 0.12
			E_b = 620 ± 130 MeV
			b = 0.99 ± 0.04

Notes. ^(a) , where and are the maximum likelihood values for the model under consideration and the power-law model, respectively. ^(b) The reference energy E₀ is set to 1 GeVfor all the models.

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