Measurement of the extragalactic background light imprint on the spectra of the brightest blazars observed with H.E.S.S.

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Table 3

Spectral modelling of the data sets used to derive the likelihood profiles.

Data set	Spectral model	χ²(α₀)/d.o.f.

Mrk 421 (1)	ELP	21.5/31
Mrk 421 (2)	ELP	46.8/30
Mrk 421 (3)	ELP	34.8/28
PKS 2005-489 (1)	LP	49.5/60
PKS 2005-489 (2)	LP	31.8/46
PKS 2155-304 (2008)	ELP	21.9/37
PKS 2155-304 (1)	PWL	32.3/31
PKS 2155-304 (2)	SEPWL	25.3/28
PKS 2155-304 (3)	SEPWL	35.2/31
PKS 2155-304 (4)	SEPWL	19.1/21
PKS 2155-304 (5)	SEPWL	24.3/27
PKS 2155-304 (6)	LP	29.2/21
PKS 2155-304 (7)	SEPWL	13.6/13
1ES 0229+200	PWL	60.1/60
H 2356-309	LP	70.2/61
1ES 1101-232	PWL	62.6/69
1ES 0347-121	ELP	31.7/35

Notes. The spectral models (see Sect. 2.3) are given in Col. 2, where the acronyms PWL, LP, EPWL, ELP, and SEPWL are explained in Table 2. The χ² for the best fit EBL optical depth normalization α₀ and the number of degrees of freedom d.o.f. are given in Col. 3.

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