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.2.

Model 2: Best-fitting model parameters when the soft excess and hot corona are allowed to be associated with different covering fraction ( $C_{f}^{(SE)}$ $Mathematical equation: $ C_{\mathrm{f}}^\mathrm{{(SE)}} $$ and $C_{f}^{(HC)}$ $Mathematical equation: $ C_{\mathrm{f}}^\mathrm{{(HC)}} $$ respectively).

First eclipse

Spec. #	N_H	log ξ

1-8	4.8 ± 1.0	0.64 ± 0.37

	$C_{f}^{(SE)}$ $Mathematical equation: $ C_{\mathrm{f}}^\mathrm{{(SE)}} $$	$C_{f}^{(HC)}$ $Mathematical equation: $ C_{\mathrm{f}}^\mathrm{{(HC)}} $$

1	0.69 ± 0.15	0.43 ± 0.09

2	0.65 ± 0.06	$= C_{f}^{(SE)}$ $Mathematical equation: $ =C_{\mathrm{f}}^\mathrm{{(SE)}} $$

3	0.77 ± 0.04	$= C_{f}^{(SE)}$ $Mathematical equation: $ =C_{\mathrm{f}}^\mathrm{{(SE)}} $$

4	0.83 ± 0.03	$= C_{f}^{(SE)}$ $Mathematical equation: $ =C_{\mathrm{f}}^\mathrm{{(SE)}} $$

5	0.80 ± 0.04	$= C_{f}^{(SE)}$ $Mathematical equation: $ =C_{\mathrm{f}}^\mathrm{{(SE)}} $$

6	0.67 ± 0.12	0.48 ± 0.06

7	0.65 ± 0.12	0.25 ± 0.09

8	0.20 ± 0.12	≤0.07

Second eclipse

Spec. #	N_H	log ξ

9-12	0.7 ± 0.5	≤0.8

	$C_{f}^{(SE)}$ $Mathematical equation: $ C_{\mathrm{f}}^\mathrm{{(SE)}} $$	$C_{f}^{(HC)}$ $Mathematical equation: $ C_{\mathrm{f}}^\mathrm{{(HC)}} $$

9	≤0.08	$= C_{f}^{(SE)}$ $Mathematical equation: $ =C_{\mathrm{f}}^\mathrm{{(SE)}} $$

10	0.16 ± 0.07	$= C_{f}^{(SE)}$ $Mathematical equation: $ =C_{\mathrm{f}}^\mathrm{{(SE)}} $$

11	0.32 ± 0.06	$= C_{f}^{(SE)}$ $Mathematical equation: $ =C_{\mathrm{f}}^\mathrm{{(SE)}} $$

12	≤0.08	$= C_{f}^{(SE)}$ $Mathematical equation: $ =C_{\mathrm{f}}^\mathrm{{(SE)}} $$

Global fit

1-12		C/ν = 5793/6519

Notes. Column densities are given in units of 10²² cm⁻². The X-ray continuum and Fe line parameters as well as X-ray fluxes are all consistent within errors with those reported in Table A.1.

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