We present the results of X-ray spectral analysis of the Seyfert type 2 galaxy Mrk 417 ( ɀ ≈ 0.0327 ) based on data from the NuSTAR (3-60 keV) and Swift/BAT (14-150 keV) space observatories. The spectrum from the NuSTAR observatory is well described by a basic power-law model with neutral absorption and an additional reflection component from a cold neutral medium (power-law index \( \Gamma ={1.63}_{-0.11}^{+0.10} \), absorption \( {\mathrm{N}}_{\mathrm{H}}={3.22}_{-0.39}^{+0.41}\cdot {10}^{23}{cm}^{-2} \)). A narrow Fe K_α emission line with an equivalent width \( {\mathrm{EW}}_{{\mathrm{FeK}}_{\upalpha}}={115}_{-1}^{+2}e\mathrm{V} \) is present and indicates a moderate density of the medium in which this line is formed. The NuSTAR data together with the Swift/BAT data were analyzed using the more complicated physical models MYTorus and BNTorus. In the first case a power-law index \( {\Gamma}_{\mathrm{MYTorus}}={1.68}_{-0.09}^{+0.09} \) and an absorption along the line of sight of \( {\mathrm{N}}_{\mathrm{HI}.\mathrm{o}.\mathrm{s}}={3.36}_{-0.07}^{+0.04}\cdot {10}^{23}{cm}^{-2} \) were obtained. The BNTorus model yields a power-law index of \( {\Gamma}_{\mathrm{BNTorus}}={1.75}_{-0.09}^{+0.09} \) and an absorption along the line of sight of \( {\mathrm{N}}_{\mathrm{HI}.\mathrm{o}.\mathrm{s}}={3.72}_{-0.39}^{+0.49}\cdot {10}^{23}{cm}^{-2} \). These results provide an estimate of the covering factor for the gas-dust torus of fc ≈ 0.29 − 0.34 and derive absorption-corrected X-ray luminosity of L_{intr2 ‐ 10keV} ∼ 3.16 ⋅ 10⁴³erg/s. Additional analysis of the observational data in the near IR indicates that the covering factor may even be smaller, at f_c ∼ 0.12. These results indicate that the gas-dust torus is most likely compressed along the vertical and has preferably a ring-like geometry.

我们根据来自NuSTAR（3-60 keV）和Swift / BAT（14-150 keV）空间观测站的数据，介绍了塞弗特2型星系Mrk 417（ɀ≈0.0327）的X射线光谱分析结果。NuSTAR天文台的光谱通过具有中性吸收的基本幂律模型以及来自冷中性介质的附加反射分量（幂律指数\（\ Gamma = {1.63} _ {-0.11} ^ {+ 0.10} \），吸收\（{\ mathrm {N}} _ {\ mathrm {H}} = {3.22} _ {-0.39} ^ {+ 0.41} \ cdot {10} ^ {23} {cm} ^ {-2} \））。窄的Feķ _α具有等同宽度发射线{ - 1} ^ {+ 2}ë\（{\ mathrm {EW}} _ {{\ mathrm {FEK}} _ {\ upalpha}} = {115} _ \ mathrm {V} \）存在时，表示形成该线的介质的中等密度。使用更复杂的物理模型MYTorus和BNTorus对NuSTAR数据和Swift / BAT数据进行了分析。在第一种情况下，幂律索引\（{\ Gamma} _ {\ mathrm {MYTorus}} = {1.68} _ {-0.09} ^ {+ 0.09} \）和沿\（ {\ mathrm {N}} _ {\ mathrm {HI}。\ mathrm {o}。\ mathrm {s}} = {3.36} _ {-0.07} ^ {+ 0.04} \ cdot {10} ^ {23}已获得{cm} ^ {-2} \）。BNTorus模型产生\（{\ Gamma} _ {\ mathrm {BNTorus}} = {1.75} _ {-0.09} ^ {+ 0.09} \）的幂律指数，并沿\ （{\ mathrm {N}} _ {\ mathrm {HI}。\ mathrm {o}。\ mathrm {s}} = {3.72} _ {-0.39} ^ {+ 0.49} \ cdot {10} ^ {23 } {cm} ^ {-2} \）。这些结果为的气体尘埃环面提供覆盖系数的估计FC  ≈0.29 - 0.34和派生吸收校正的X射线光度大号_{intr2 - 10keV}  〜3.16⋅10 ⁴³尔格/小号。在近IR中的观测数据的额外分析表明，覆盖因子可以甚至更小，在˚F _Ç  〜0.12。这些结果表明，尘埃圆环很可能沿垂直方向被压缩，并且优选地具有环形的几何形状。