  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 $\Gamma =
1.63_{-0.11}^{+0.10}$ and obscured by hydrogen column density of $N_{H} =
3.22_{-0.39}^{+0.41} \cdot 10^{23} cm^{-2}$, narrow $FeK_\alpha$ 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 $\Gamma_{MYTorus} = 1.68_{-0.09}^{+0.09}$ 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 $\Gamma_{BNTorus} =
1.75_{-0.09}^{+0.09}$ 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.
