The X-ray Emission of γ Cassiopeiae During the 2020–2021 disc eruption

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Table 4

Fluorescent Fe Kα line strength, X-ray fluxes, and flux hardness ratio.

Obs.	HJD–2 450 000	EW(Fe Kα) (eV)	f_X,obs (10⁻¹¹ erg cm⁻² s⁻¹)		HR_flux	f_x,unabs (10⁻¹¹ erg cm⁻² s⁻¹)
			S	H		S	H
Aug. 01	2132.202	34 ± 14	4.31 ± 0.09	15.42 ± 0.10	0.56 ± 0.01	4.41	15.43
Feb. 04	3041.662	35 ± 5	5.00 ± 0.02	12.01 ± 0.03	0.41 ± 0.01	5.14	12.02
Jul. 10a	5384.901	55 ± 11	4.46 ± 0.06	14.55 ± 0.07	0.53 ± 0.01	4.56	14.56
Jul. 10b	5401.741	57 ± 14	3.89 ± 0.03	12.36 ± 0.04	0.52 ± 0.01	3.98	12.37
Aug. 10a	5411.182	51 ± 10	5.87 ± 0.06	17.67 ± 0.07	0.50 ± 0.01	6.01	17.68
Aug. 10b	5428.685	52 ± 12	3.88 ± 0.02	12.17 ± 0.05	0.52 ± 0.01	3.97	12.18
Jul. 14	6863.268	59 ± 7	5.28 ± 0.06	20.45 ± 0.29	0.59 ± 0.01	5.40	20.47
Jan. 21	9219.190	45 ± 7	1.44 ± 0.01	12.33 ± 0.01	0.79 ± 0.01	1.46	12.34
Feb. 21	9263.018	56 ± 11	4.79 ± 0.16	13.16 ± 0.29	0.47 ± 0.02	4.89	13.17
Jul. 21	9420.564	40 ± 10	5.28 ± 0.16	15.83 ± 0.05	0.50 ± 0.01	5.39	15.85
Jan. 22	9598.080	55 ± 11	2.59 ± 0.03	14.13 ± 0.02	0.69 ± 0.01	2.64	14.14

Notes. The fluxes in Cols. 4 and 5, and the inferred flux hardness ratio in Col. 6, are observed values, not corrected for interstellar absorption. The fluxes in the last two columns are corrected for the absorption by the interstellar medium.

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