Table 4: Spectral fitting results (see Sect. 4.2.3 and Fig. 4).
Sourcea Mb $N_{\rm H}$c kTd Ze Rf $\theta_{\rm obs}^{g}$ $\Gamma^{h}$ $E_{\rm Fe}^{i}$ $\sigma_{\rm Fe}^{j}$ EWk Fluxl $\chi^{2}/{\rm d.o.f.}$
      [keV]         [keV] [ev] [keV]    
NGC 2782 $_{\rm Int}$ ${\rm I}$ >10 $\rm0.66^{+0.03}_{-0.03}$ $\rm0.15^{+0.01}_{-0.01}$ 0.004 $\rm 75.5^{+3.4}_{-4.7}$ $\rm 1.68^{+0.09}_{-0.08}$ - - - 4.39 52/44
  ${\rm II}$ $\rm 12.7^{+4.2}_{-2.3}$ $\rm0.66^{+0.03}_{-0.03}$ $\rm0.16^{+0.01}_{-0.01}$ 0.130 - $\rm0.25^{+0.08}_{-0.06}$ - - - 4.80 49/45
NGC 2782 $_{\rm Nuc}$ ${\rm I}$ >10 $\rm0.45^{+0.15}_{-0.12}$ 1.00 0.000 $\rm 70.4^{+5.3}_{-7.0}$ $\rm 2.14^{+0.11}_{-0.11}$ $\rm 6.39^{+0.10}_{-0.12}$ $\rm 86^{+159}_{-86}$ 0.99 1.86 15/10
  ${\rm II}$ $\rm 4.3^{+2.5}_{-1.6}$ $\rm0.28^{+0.04}_{-0.05}$ $\rm0.47^{+0.21}_{-0.20}$ 0.666 - $\sim $0.07 $\rm 6.35^{+0.11}_{-0.09}$ <160 1.32 2.02 15/10
NGC 5728 $_{\rm Int}$ ${\rm I}$ >10 $\rm0.61^{+0.04}_{-0.03}$ $\rm0.02^{+0.01}_{-0.01}$ 0.037 $\rm 2.6^{+44.7}_{-2.6}$ $\rm -0.81^{+0.07}_{-0.07}$ $\rm 6.33^{+0.33}_{-0.33}$ $\rm 120^{+47}_{-111}$ 1.55 13.0 45/26
  ${\rm II}$ $\rm 7.7^{+0.55}_{-0.51}$ $\rm0.49^{+0.04}_{-0.03}$ $\rm0.03^{+0.01}_{-0.01}$ 0.033 - $\rm0.77^{+0.07}_{-0.06}$ $\rm 6.33^{+0.33}_{-0.33}$ $\rm 98^{+41}_{-33}$ 1.13 13.2 35/27
NGC 5728 $_{\rm Nuc}$ ${\rm I}$ >10 $\rm0.61^{+0.08}_{-0.08}$ $\rm0.04^{+0.01}_{-0.02}$ 0.005 $\rm 9.7^{+34.9}_{-9.7}$ $\rm -1.09^{+0.08}_{-0.07}$ $\rm 6.32^{+0.04}_{-0.03}$ $\rm 108^{+43}_{-37}$ 1.29 9.54 23/15
  ${\rm II}$ $\rm 8.2^{+0.53}_{-0.50}$ $\rm0.15^{+0.01}_{-0.01}$ $\rm0.14^{+0.03}_{-0.03}$ 0.011 - $\rm0.94^{+0.08}_{-0.07}$ $\rm 6.32^{+0.04}_{-0.04}$ $\rm 85^{+43}_{-39}$ 0.89 9.34 16/16
a Source $_{\rm Int}$: integrated spectra from circular areas with a radius of 10 $^{\prime \prime }$ around the nuclear position; source $_{\rm Nuc}$: nuclear spectra from smaller areas of 1 $^{\prime \prime }$ in radius.
b M: Model I: a Compton-thick high-energy reflection spectrum (wabs*zwabs(mekal+hrefl(pow+gau)) in XSPEC); Model II: a partially absorbed power law spectrum (wabs*zwabs(mekal+pow+zwabs(pow+gau)) in XSPEC). The galactic absorbing column densities are 1.76 $\times$ 1020 cm-2 and 7.83 $\times$ 1020 cm-2 for NGC 2782 and NGC 5728, respectively (from Dickey & Lockman 1990).
c X-ray absorbing column density in units of 1023 cm-2.
d Temperature of the thermal MEKAL plasma in keV.
e Metallicity of the thermal MEKAL plasma as a fraction of solar metallicity (in the case of model I of NGC 2782 $_{\rm Nuc}$, this relative metallicity is not constrained by the data and was therefore fixed to unity).
f Ratio between the directly seen continuum and the scattered/absorbed continuum.
g Disk inclination.
h Photon index.
i There is no obvious line in the integrated spectrum of NGC 2782 (NGC 2782 $_{\rm int}$). Intrinsically present line emission may be buried in the relatively bright extended continuum.
j Width of the line feature that is tentative in the case of NGC 2782 (its strength does not significantly affect the other parameters).
k Equivalent width of the line feature, see footnote j.
l Flux from 0.3 to 8 keV in units of 10-13 erg cm-2 s-1 (corrected for galactic absorption).

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