A Suzaku observation of the ULIRG IRAS19254-7245: discerning the AGN component

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Table 1:

Results of the spectral fit.
Model	$\Gamma$	$N_{\rm H}$	$E_{\rm c}/\xi$	$\sigma^{a}$	EW^b	L(2-10 keV)^c	L(10-30 keV)^c	$\chi^2/$ d.o.f.
		10²⁴ cm^-2	keV/erg cm s^-1	keV	keV	10 ⁴⁴erg s^-1	10 ⁴⁴erg s^-1
A	1.8^f	$\rm 4.2^{+2.7}_{-0.9}$	$\rm 6.67^{+0.05}_{-0.05}$	$\rm0.11^{+0.06}_{-0.06}$	$\rm0.60^{+0.12}_{-0.22}$	4.0	3.6	164/145
B^d	1.8^f	$\rm 3.1^{+1.2}_{-0.4}$	$\rm 6.66^{+0.04}_{-0.05}$	$\rm0.14^{+0.07}_{-0.06}$	$\rm0.86^{+0.24}_{-0.25}$	2.1	1.9	181/146
C^d	$\rm 1.20^{+0.11}_{-0.04}$	$\rm 4.1^{+1.3}_{-1.3}$	$\rm 6.67^{+0.05}_{-0.04}$	$\rm0.12^{+0.06}_{-0 .05}$	$\rm0.67^{+0.16}_{-0.15}$	1.7	3.9	154/145
D^d	$\rm 1.87^{+0.11}_{-0.28}$	$\rm 3.2^{+1.3}_{-0.5}$	$\rm 1000^{+170}_{-430}$	-	-	2.6	2.2	199/147

^a The values of $\sigma$ are the measured ones, which are not corrected for width of the calibration lines, $\sigma_{\rm lamp}$ . ^b The EW is measured against the total observed continuum. ^c The luminosities are derived from the XIS front illuminated CCDs. ^d These models do not include a cold reflected component.

Source LaTeX | All tables | In the text

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