\pm 0.2$]{} & [$0.23 \pm 0.11$]{} & [$0.72 \pm 0.16$]{}\
EW$_{\textsc{ga}}$ (eV) && [$140^{+ 10}_{- 20}$]{} & [$20 \pm 10$]{} & [$70^{+ 10}_{- 20}$]{}\
${\chi^{2}/\textrm{dof}}$ &947/1007&&&\
\
${kT_{\textrm{e}}}$ (keV) & [$75^{+ 20}_{- 15}$]{}&(t)&(t)&(t)\
$y$ & [$1.20^{+ 0.01}_{- 0.02}$]{}&(t)&(t)&(t)\
$N_{\textsc{compps}}$ ([$10^{4}$]{}) &[$5.6^{+ 0.4}_{- 0.3}$]{} &(t)&(t)&(t)\
${\chi^{2}/\textrm{dof}}$ &971/1007&&&\

![\[fig:plot\_2110\] Upper panel: spectra of NGC 2110 with best-fitting [[compps]{}]{} model. Second panel: residuals, plotted as $\Delta \chi = $ (data-model)/error. Third panel: best-fitting model $E^2 f(E)$. The data were binned for plotting purposes.](plot_2110){width="\columnwidth"}

Discussion and conclusions {#sec:discussion}
==========================

We presented the hard X-ray spectra of the two X-ray bright Seyferts [NGC 4388]{} and [NGC 2110]{}, from [[*INTEGRAL*]{}]{}’s IBIS data taken from 2003 to early 2015. From a joint fit with [[*XMM–Newton*]{}]{} and [[*NuSTAR*]{}]{} data, we find that the spectrum up to 300 keV is in both cases well described by an absorbed power law with a well-constrained high-energy cut-off. In agreement with past observations, we find no evidence of a Compton hump. The primary continuum is generally consistent with being constant in spectral slope among the time-averaged IBIS spectrum and the [[*XMM–Newton*]{}]{} and [[*NuSTAR*]{}]{} observations, with some absorption variability seen in [NGC 2110]{}. This is consistent with the lack of clear evidence of 