Detection of very-high-energy γ-ray emission from the colliding wind binary η Car with H.E.S.S.

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Table 3

Estimated contributions to the systematic uncertainties in the spectral measurements for the mono analyses presented in this work follow the description in H.E.S.S. Collaboration (2017) and we assume similar systematics as for the PG 1553+113 source, which has a similarly steep spectral index as η Car.

Source of uncertainty	Energy scale	Flux	Index	Flux	Index
		DS-I	DS-I	DS-II	DS-II
MC shower interactions		1%		1%
MC atmosphere simulation	7%

Instrument simulation/calibration	10%	10%		10%
Broken pixels		10%		10%
Live time		<5%		<5%

Reconstruction and selection cuts	15%	15%	0.96	15%	0.34
Background subtraction		10%/55%	0.46	10%/55%	0.46

Total	19%	24%/60%	1.06	24%/60%	0.57

Notes. Values quoted are for upward/downward or symmetric errors. See text for more details on the differences. The energy scale uncertainty in this analysis is estimated to be larger than for PG 1553+113.

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