X-raying the ζ Tau binary system | Astronomy & Astrophysics (A&A)

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Table 1

Results of the spectral fitting of XMM-Newton spectra.

ObsID	HJD-2.4e6	ϕ	norm₁ (10⁻⁴ cm⁻⁵) norm_G	norm₂ (10⁻⁶ cm⁻⁵) χ²/dof	kT₃ (keV)	norm₃ (10⁻⁵ cm⁻⁵) $F_{X}^{obs}$ $\[F_{\mathrm{X}}^{\text {obs }}\]$ in erg cm⁻² s⁻¹	N_H (10²² cm⁻²)	norm₄ (10⁻² cm⁻⁵)
2nd row			(10⁻⁵ ph cm⁻² s⁻¹)		(0.5–10.) (10⁻¹¹)	(0.5–2.) (10⁻¹⁴)	(2.–10.) (10⁻¹¹)
0920020301	60 024.054	0.02	3.55 ± 0.40	6.05 ± 1.51	4.16 ± 1.80	2.95 ± 3.03	17.21 ± 0.20	2.63 ± 0.03
			2.52 ± 0.31	648.87/565	1.77 ± 0.02	4.65 ± 0.56	1.76 ± 0.01
0920020401	60 221.177	0.50	2.49 ± 0.37	7.51 ± 1.65	2.58 ± 1.39	4.16 ± 1.13	9.41 ± 0.10	2.00 ± 0.02
			2.60 ± 0.25	854.63/658	1.70 ± 0.01	11.5 ± 0.7	1.69 ± 0.01

0920020301	60 024.054	0.02	3.56 ± 0.40	6.10 ± 1.50	= kT₄	3.44 ± 0.77	17.26 ± 0.19	2.64 ± 0.03
			2.51 ± 0.31	649.12/566	1.77 ± 0.03	4.68 ± 0.26	1.76 ± 0.01
0920020401	60 221.177	0.50	2.43 ± 0.36	7.05 ± 1.62	= kT₄	5.87 ± 1.01	9.47 ± 0.09	2.01 ± 0.02
			2.59 ± 0.25	858.86/659	1.70 ± 0.01	11.6 ± 0.4	1.69 ± 0.01

Notes. The absorbed thermal model has the form phabs(ISM) × [apec₁ + apec₂ + apec₃ + phabs × apec₄ + Gaussian]. The ephemerids of Nazé et al. (2022c) are used, i.e. P = 132.987 days and T₀ = 2458 159.8 (with ϕ = 0 corresponding to the Be star in front of its companion). The interstellar absorption is fixed to $N_{H}^{I S M} = 2.7 \times 10^{20} {c m}^{- 2}$ $\[N_{\mathrm{H}}^{\mathrm{ISM}}=2.7 \times 10^{20} \mathrm{~cm}^{-2}\]$ (Nazé et al. 2022c). The errors correspond to 1σ errors, with the largest values provided if asymmetric. In the models of the top part of the Table, kT₁ = 0.085 keV, kT₂ = 0.55 keV, and kT₄ = 9.1 keV while for the bottom part kT₁ = 0.085 keV, kT₂ = 0.55 keV, and kT₃ = kT₄ = 9.05 keV.

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