A deep Chandra ACIS study of NGC 4151. III. the line emission and spectral analysis of the ionization cone

This paper is the third in a series in which we present deep Chandra ACIS-S imaging spectroscopy of the Seyfert1 galaxy NGC 4151, devoted to study its complex circumnuclear X-ray emission. Emission features in the soft X-ray spectrum of the bright extended emission (L _{0.3-2 keV} ∼ 10 ⁴⁰ erg s^-1) at r > 130pc (2″) are consistent with blended brighter O VII, O VIII, and Ne IX lines seen in the Chandra HETGS and XMM-Newton RGS spectra below 2keV. We construct emission line images of these features and find good morphological correlations with the narrow-line region clouds mapped in [O III] λ5007. Self-consistent photoionization models provide good descriptions of the spectra of the large-scale emission, as well as resolved structures, supporting the dominant role of nuclear photoionization, although displacement of optical and X-ray features implies a more complex medium. Collisionally ionized emission is estimated to be ≲12% of the extended emission. Presence of both low- and high-ionization spectral components and extended emission in the X-ray image perpendicular to the bicone indicates leakage of nuclear ionization, likely filtered through warm absorbers, instead of being blocked by a continuous obscuring torus. The ratios of [O III]/soft X-ray flux are approximately constant (∼15) for the 1.5kpc radius spanned by these measurements, indicating similar relative contributions from the low- and high-ionization gas phases at different radial distances from the nucleus. If the [O III] and X-ray emission arise from a single photoionized medium, this further implies an outflow with a wind-like density profile. Using spatially resolved X-ray features, we estimate that the mass outflow rate in NGC 4151 is ∼2 M _⊙yr^-1 at 130pc and the kinematic power of the ionized outflow is 1.7 × 10⁴¹ erg s^-1, approximately 0.3% of the bolometric luminosity of the active nucleus in NGC 4151.