area close to the source. The spectra were binned to have a signal-to-noise ratio larger than 3 in each spectral channel and not to oversample the instrumental resolution by a factor greater than 2.5. The spectra from the two detectors were analysed jointly but not combined.

Both [NGC 4388]{} and [NGC 2110]{} are detected with a good signal-to-noise in the hard X-ray band with IBIS ($> 6 \sigma$ in the 150–300 keV band, see Table \[tab:src\]). Here we use the data collected by the [[*INTEGRAL*]{}]{} Soft Gamma-Ray Imager [ISGRI: @isgri], that is the low-energy camera of the IBIS telescope. We used data up to [[*INTEGRAL*]{}]{} orbit 1500, that is from the launch in 2002 to the end of January 2015. ISGRI images for each available pointing were generated in 14 energy bands using the ISDC offline scientific analysis (OSA) software [@osa], version 10.2. Count rates at the position of the source were extracted from individual images to provide light curves in 14 energy bands between 20 and 300 keV. Weighted mean fluxes were then extracted in each band and combined to produce an average source spectrum [see @bird2007; @bird2010 for details]. Corresponding weighted response (arf) files for each source were 