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tokens: to account for the radiative recombination continuum and lines, a cutoff power-law model to account for the off-nuclear X-ray sources, in addition to the AGN-related emission, which is parametrized by two different MYTorus scattered and line components, in addition to the transmitted one described by the zeroth-order component of that model. In our fitting, in addition to our baseline model, we added the Bremsstrahlung and cutoff power law with all parameters fixed at the values provided by Bauer et al. ( 2015 ), and a Gaussian line to roughly model the excess around 6.5 keV. To account for the multiple absorption components, we also added a second Borus model, whose best-fitting parameters are , CFtor = 83 per cent, and A Fe = 1. Our best-fitting parameters are broadly consistent with the results presented by Bauer et al. ( 2015 ). The observed flux in the 2–10 keV energy band is 5.4 × 10 −12 erg cm −2 s −1 , and the intrinsic one (i.e. corrected for absorption) 1.3 × 10 −10 erg cm −2 s −1 . A0.2 NGC 1194 The starting model for the spectral fit of this source is provided by the work of Masini et al. ( 2016 ), who fitted the NuSTAR spectrum with the MYTorus model in the decoupled mode, with the addition of a Gaussian line at 6.8 keV, and a scattering fraction of the primary continuum of . In our fitting, we used our baseline model and found the main parameters (Γ, N H , and f s ) to be fully consistent with their best-fit results. The 2–10 keV observed flux is 1.2 × 10 −12 erg cm −2 s −1 , and the intrinsic one 1.0 × 10 −11 erg cm −2 s −1 . A0.3 NGC 2273 The starting spectral model for this source is again provided by the work of Masini et al. ( 2016 ), who fitted the NuSTAR spectrum with the Torus model that favoured a heavily absorbed scenario with . In our fitting, we used our baseline model, which yielded a best fit broadly consistent with their results. The 2–10 keV observed flux is 9.2 × 10 −13 erg cm −2 s −1 , and the intrinsic one 3.6 × 10 −10 erg cm −2 s −1 . A0.4 NGC 3079 The starting spectral model for this source is again provided by the work of Masini et al. ( 2016 ), who fitted the NuSTAR spectrum with the MYTorus model in a coupled mode. The results obtained with our baseline model are consistent within the respective uncertainties with their results. The 2–10 keV observed flux is 6.4 × 10 −13 erg cm −2 s −1 , and the intrinsic one 1.2 × 10 −10 erg cm −2 s −1 . A0.5 NGC 3393 The starting spectral model for this source is provided by the work of Koss et al. ( 2015 ) and Masini et al. ( 2016 ), who fitted the NuSTAR spectrum with both MYTorus and Torus models. The results obtained with our baseline model are broadly consistent with the results presented by these authors with a slightly larger value of N H (10 25 versus ). The 2–10 keV observed flux is 4.4 × 10 −13 erg cm −2 s −1 , and the intrinsic one 8.3 × 10 −11 erg cm −2 s −1 . A0.6 NGC 4388 The starting spectral model for this source is once more provided by the work of