X-ray eclipse tomography: Resolving the extent of X-ray-emitting region(s) in the Seyfert galaxy ESO 362-G18

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Volume 711 (July 2026)

A&A, 711 (2026) A250

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Table A.1.

Model 1: Best-fitting model parameters assuming a single X-ray-emitting region.

Continuum and Fe line

Spec. #	Γ	$k T_{e}^{(hot)}$ $Mathematical equation: $ kT_{\mathrm{e}}^{\mathrm{(hot)}} $$	$k T_{e}^{(warm)}$ $Mathematical equation: $ kT_{\mathrm{e}}^{\mathrm{(warm)}} $$

1-12	1.71 ± 0.03	100^f	120 ± 10

	τ^(warm)	σ_Fe	EW_Fe

1-12	≥25	480 ± 220	220 ± 130

First eclipse

Spec. #	N_H log ξ

1-8	4.5 ± 1.0 0.65 ± 0.35

	C_f	$F_{0.3 - 10}^{obs}$ $Mathematical equation: $ F_\mathrm{{0.3-10}}^{\mathrm{obs}} $$	$F_{0.3 - 10}^{int}$ $Mathematical equation: $ F_\mathrm{{0.3-10}}^{\mathrm{int}} $$

1	0.48 ± 0.08	1.56 ± 0.09	2.27 ± 0.24

2	0.64 ± 0.06	1.30 ± 0.09	2.21 ± 0.24

3	0.77 ± 0.04	1.25 ± 0.09	2.39 ± 0.25

4	0.82 ± 0.03	1.34 ± 0.09	2.73 ± 0.27

5	0.79 ± 0.04	1.02 ± 0.08	2.02 ± 0.23

6	0.53 ± 0.06	3.11 ± 0.15	4.65 ± 0.41

7	0.35 ± 0.06	3.45 ± 0.11	4.32 ± 0.31

8	≤0.14	4.46 ± 0.13	4.72 ± 0.13

Second eclipse

Spec. #	N_H log ξ

9-12	0.7 ± 0.5 ≤0.8

	C_f	$F_{0.3 - 10}^{obs}$ $Mathematical equation: $ F_\mathrm{{0.3-10}}^{\mathrm{obs}} $$	$F_{0.3 - 10}^{int}$ $Mathematical equation: $ F_\mathrm{{0.3-10}}^{\mathrm{int}} $$

9	≤0.08	5.61 ± 0.13	5.80 ± 0.13

10	0.15 ± 0.07	4.29 ± 0.14	4.78 ± 0.39

11	0.31 ± 0.06	4.10 ± 0.13	4.89 ± 0.38

12	≤0.08	3.10 ± 0.07	3.22 ± 0.09

Global fit

1-12			C/ν = 5819/6523

Notes. Column densities are given in units of 10²² cm⁻². $k T_{e}^{(warm)}$ $Mathematical equation: $ kT_{\mathrm{e}}^{\mathrm{(warm)}} $$ , σ_Fe, and EW_Fe are in units of eV while $k T_{e}^{(hot)}$ $Mathematical equation: $ kT_{\mathrm{e}}^{\mathrm{(hot)}} $$ is fixed and in units of keV. The model is also absorbed by Galactic column density fixed at 1.35 × 10²⁰ cm⁻² (HI4PI Collaboration 2016). Observed and intrinsic (unabsorbed) X-ray fluxes are in units of 10⁻¹¹ erg s⁻¹ cm⁻². The first column (Spec. #) indicates the spectrum or range of spectra from which the reported parameters have been constrained (see e.g. the upper panel of Fig. 5 as reference). The continuum and Fe line parameters (upper part) are common for all spectra (Spec. #1-12).

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