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Nuclear obscuration structure in Mrk 417 based on NuSTAR and Swift/BAT data

We present the results of X-ray spectral analysis of the Seyfert type 2 galaxy Mrk 417 observed by the NuSTAR (3-60 keV) and the Swift/BAT (14-150) observatories. The NuSTAR data shows a good fit with a baseline model which composed of an absorbed cutoff power-law component and reflected emission from the cold neutral medium. We found that the spectrum is steep $Γ= 1.63_{-0.11}^{+0.10}$ and obscured by hydrogen column density of $N_{H} = 3.22_{-0.39}^{+0.41} \cdot 10^{23} cm^{-2}$, narrow $FeK_α$ emission line has an equivalent width of $EW = 115_{-1}^{+2}$ eV that suggests this feature is originated in a moderate density of obscurer. In combining NuSTAR data with Swift/BAT spectrum we also applied a more physically motivated approach using complex physical models MYTorus and BNTorus. For the first case the photon index of $Γ_{MYTorus} = 1.68_{-0.09}^{+0.09}$ and the line-of-sight column density of the absorber $N_{H,l.o.s} = 3.36_{-0.07}^{+0.04} \cdot 10^{23} cm^{-2}$. Applying BNTorus model shows the photon index $Γ_{BNTorus} = 1.75_{-0.09}^{+0.09}$ and absorption $N_{H,l.o.s} = 3.72_{-0.39}^{+0.49} \cdot 10^{23} cm^{-2}$. Based on the results we get an estimation of gas-dust torus covering factor $f_{c} = 0.29-0.34$ and an intrinsic X-ray luminosity in 2-10 keV of $\approx 3.16\cdot 10^{43}$ erg/s. Further analysis of Mid-Infrared (MIR) observational data, indicates that the covering factor maybe even smaller $f_{c} \approx 0.12$. Our results allow us to suggest that obscuring material of Mrk 417 has preferably a ring-like geometry.