purposes.](plot_4388){width="\columnwidth"}

[ l c c c c]{} & all obs. & XMM1 & XMM2 & NUS\
\
$\Gamma$ & [$1.60^{+ 0.07}_{- 0.06}$]{}&(t)&(t)&(t)\
${E_{\textrm{c}}}$ (keV)& [$200^{+ 75}_{- 40}$]{}&(t)&(t)&(t)\
$N_{\textsc{pow}}$ ([$10^{-2}$]{}) & [$1.8^{+ 0.4}_{- 0.2}$]{}&(t)&(t)&(t)\
$K_{\textrm{IBIS--pn}}$ && [$0.29 \pm 0.02$]{} &[$0.86 \pm 0.04$]{}& -\
$K_{\textrm{IBIS--NusA}}$ &&- &-& [$0.29 \pm 0.01$]{}\
$K_{\textrm{IBIS--NusB}}$ &&- &-& [$0.30 \pm 0.01$]{}\
${N_{\textrm{H}}}$ ([$10^{23}$]{} [cm$^{-2}$]{}) & [$3.8^{+ 0.5}_{- 0.2}$]{}&(t)&(t)&(t)\
${\textrm{C}_{\textrm{F}}}$ & [$0.95^{+ 0.03}_{- 0.02}$]{} &(t)&(t)&(t)\
$E_{\textsc{ga}}$ (keV) & [$6.39^{+ 0.02}_{- 0.01}$]{}&(t)&(t)&(t)\
$N_{\textsc{ga}}$ ([$10^{-4}$]{}) && [$3.5 \pm 0.8$]{} & [$1.6^{+ 0.3}_{- 0.2}$]{} & [$2.7 \pm 0.6$]{}\
EW$_{\textsc{ga}}$ (eV) && [$390^{+ 100}_{- 90}$]{} & [$180 \pm 30$]{} & [$300 \pm 70$]{}\
${\chi^{2}/\textrm{dof}}$ &433/432&&&\
\
${kT_{\textrm{e}}}$ (keV)& [$80^{+ 40}_{- 20}$]{}&(t)&(t)&(t)\
$y$ & [$1.08^{+ 0.05}_{- 0.08}$]{}&(t)&(t)&(t)\
$N_{\textsc{compps}}$ ([$10^{4}$]{}) &[$6.5^{+ 1.5}_{- 1.0}$]{} &(t)&(t)&(t)\
${\chi^{2}/\textrm{dof}}$ &444/432&&&\

NGC 2110
--------

The soft X-ray emission of [NGC 2110]{} below $\sim 2-3$ keV is affected by variable absorption from a complex medium [@evans2007; @rivers2014]. Therefore, we restricted the spectral analysis to the data above 3 keV. We fitted the [[*XMM–Newton*]{}]{} and [[*NuSTAR*]{}]{} spectra over the 3–10 keV and 3–79 keV energy bands.

### The IBIS spectrum

As we did for [NGC 4388]{}, we first focused on the IBIS spectrum. The spectrum above 20 keV is not strongly 