H.E.S.S. and Suzaku observations of the Vela X pulsar wind nebula

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Volume 627 (July 2019)

A&A, 627 (2019) A100

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Table 2

Best-fit parameters for the spectral models of the gamma-ray spectrum of the Vela X cocoon in the three regions shown in Fig. 1.

Pointing	Model	Flux > 1 TeV	Γ	E_cut	TS
		(10⁻⁸ cm⁻² s⁻¹ sr⁻¹)		(TeV)
0	PL	3.6 ± 0.4_stat ± 0.7_sys	1.75 ± 0.10_stat ± 0.14_sys	–	–
	ECPL	3.5 ± 0.5_stat ± 0.7_sys	1.2 ± 0.3_stat ± 0.1_sys	16 ± 7_stat ± 6_sys	6.4

1	PL	4.1 ± 0.2_stat ± 1.0_sys	1.92 ± 0.06_stat ± 0.10_sys	–	–
	ECPL	4.1 ± 0.3_stat ± 1.5_sys	1.47 ± 0.16_stat ± 0.16_sys	14 ± 5_stat ± 6_sys	13.4

2	PL	4.6 ± 0.3_stat ± 0.9_sys	1.84 ± 0.06_stat ± 0.11_sys	–	–
	ECPL	4.6 ± 0.3_stat ± 1.4_sys	1.27 ± 0.14_stat ± 0.10_sys	12 ± 3_stat ± 6_sys	25.7

Notes. Errors correspond to 1σ uncertainties. The functional forms used to model the spectra are given in Eqs. (1) and (2). TS is the test statistic for the improvement of the fit when the ECPL model is used, see text for definition.

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