Broadband characterisation of the very intense TeV flares of the blazar 1ES 1959+650 in 2016

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Table 1.

Fitting parameters of the VHE spectra during the highest-flux nights in 2016.

Time	Flux ^(a)	Fit model	F₀	E_cut	β	E_peak^(b)	χ²/d.o.f
	(10⁻¹⁰ cm⁻² ⋅ s⁻¹)		(10⁻⁹ TeV⁻¹ ⋅ cm⁻² ⋅ s⁻¹)	(TeV)		(TeV)
13th June		(1) PL		...	...	...	34.0/10

02:15–04:37		(2) PL w/ cutoff			...	...	14.1/9

(MJD 57552.094	4.06 ± 0.13	(3) LogP		...			11.4/9

–57552.192)		(4) LogP w/ cutoff		+∞^c			11.4/8

14th June		(1) PL		...	...	...	35.3/10

02:07–03:35		(2) PL w/ cutoff			...	...	5.9/9

(MJD 57553.088	3.28 ± 0.13	(3) LogP		...			6.0/9

–57553.149)		(4) LogP w/ cutoff					5.3/8

23:59 30th June		(1) PL		...	...	...	85.4/10

–04:58 1st July		(2) PL w/ cutoff			...	...	11.7/9

(MJD 57569.999	3.76 ± 0.08	(3) LogP		...			22.5/9

–57570.207)		(4) LogP w/ cutoff				+∞^c	11.5/8

Notes. The functions of PL, PL w/ cutoff, LogP, and LogP w/ cutoff are defined in Appendix B as Eqs. (B.1)–(B.4), respectively. The normalization energy E₀ is 0.3 TeV. The EBL absorption has been corrected with the model of Franceschini et al. (2008).

^(a)

For an energy range E > 300 GeV.

^(b)

Separate from the other parameters, only E_peak is determined by another fitting process by expressions with E_peak, namely, Eqs. (B.5) and (B.6).

^(c)

Here +∞ means that the energy is higher than the fitting range and reaches the upper limit of the parameter.

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