Table 2: Best-fit parameters and results for the EPIC spectra of the ESO509-IG066 Galaxy Pair members. $f_{\rm s}$ is the scattering fraction ( $1-f_{\rm s}$ is the absorber covering fraction in the "leaky absorber'' scenario). F is the observed flux in the 0.5-2/2-10 keV energy bands. L is the absorption-corrected luminosity in the 0.5-10 keV energy band.
Absorbed power-law Soft excess K $_{\alpha}$ iron line Fluxes and luminosities

Source $N_{\rm H}$ $\Gamma$ $f_{\rm s}$ $E_{\rm c}$ EW F L $\chi^2/\nu$

(10²² cm^-2) (%) (keV) (eV) (10^-12 erg cm^-2 s^-1) (10⁴³ erg s^-1)

W $7.1 \pm^{0.6}_{0.5}$ $1.81 \pm 0.13$ $2.3 \pm^{0.5}_{0.6}$ $6.35 \pm 0.05$ $120 \pm^{60}_{50}$ 0.12/5.2 $3.3 \pm 0.4$ 105.8/130

E $0.51 \pm^{0.46}_{0.10}$ $1.64 \pm^{0.72}_{0.07}$ $5.8 \pm^{14.5}_{5.2}$ 6.4^a <90 0.6/3.0 $1.43 \pm 0.08$ 170.2/167

^a Fixed.

**Table 2:** Best-fit parameters and results for the EPIC spectra of the ESO509-IG066 Galaxy Pair members. $f_{\rm s}$ is the scattering fraction ( $1-f_{\rm s}$ is the absorber covering fraction in the "leaky absorber'' scenario). F is the observed flux in the 0.5-2/2-10 keV energy bands. L is the absorption-corrected luminosity in the 0.5-10 keV energy band.
	Absorbed power-law	Soft excess	K $_{\alpha}$ iron line	Fluxes and luminosities
Source	$N_{\rm H}$	$\Gamma$	$f_{\rm s}$	$E_{\rm c}$	EW	F	L	$\chi^2/\nu$
	(10²² cm^-2)		(%)	(keV)	(eV)	(10^-12 erg cm^-2 s^-1)	(10⁴³ erg s^-1)
W	$7.1 \pm^{0.6}_{0.5}$	$1.81 \pm 0.13$	$2.3 \pm^{0.5}_{0.6}$	$6.35 \pm 0.05$	$120 \pm^{60}_{50}$	0.12/5.2	$3.3 \pm 0.4$	105.8/130
E	$0.51 \pm^{0.46}_{0.10}$	$1.64 \pm^{0.72}_{0.07}$	$5.8 \pm^{14.5}_{5.2}$	6.4^a	<90	0.6/3.0	$1.43 \pm 0.08$	170.2/167

Source LaTeX | All tables | In the text

	1 Introduction
	2 The data
	3 Discussion
	References