The 0.9 Ms XRISM/Resolve Spectrum of the Seyfert 1 Active Galactic Nucleus NGC 4151

NGC 4151 is the brightest Seyfert 1 galaxy in the band of the Resolve calorimeter aboard XRISM. It has been observed on 14 occasions. Herein, we report on an analysis of its time-averaged 893 ks spectrum. The narrow Fe Kα emission-line complex requires contributions from the torus and optical broad-line region (BLR). Models assuming an emissivity index of q = 2 for these components are statistically preferred, consistent with a “bowl” geometry for the central engine. A smooth red wing of these line components is consistent with Compton scattering from bound electrons, signaling the presence of dust in the base of the BLR and in the torus. The data statistically prefer relativistic reflection from a disk with an inner radius of (Formula presented) r = 3.2^+3.5_−2.0 GM/c², and an inclination of (Formula presented) θ =2 9.7^+0.5_−0.4 degrees. The Fe K edge at 7.1 keV is best modeled with contributions from multiple charge states, consistent with cool, kT ≃ 5 eV collisional gas or photoionized gas. Slow “warm absorber” winds spanning Fe XX–XXVI, faster winds seen via Fe XXV and Fe XXVI lines, and ultra-fast outflows (UFOs) are detected simultaneously. The warm absorbers are “failed” winds; the data constrain their radius, density, filling factor, and distribution. For the most conservative volume filling factors, the UFOs may not be able to halt star formation. However, the UFOs may generate galaxy-altering feedback for larger filling factors and/or during certain intervals.