Fiore, F.Pellegrini, S.Matt, G.Antonelli, L. A.Comastri, A.della Ceca, R.Giallongo, E.Mathur, S.Molendi, S.Siemiginowska, AnetaTrinchieri, G.Wilkes, Belinda2017-02-132001Fiore, F., S. Pellegrini, G. Matt, L. A. Antonelli, A. Comastri, R. della Ceca, E. Giallongo, et al. 2001. “The BeppoSAX View of the X‐Ray Active Nucleus of NGC 4258.” The Astrophysical Journal 556 (1) (July 20): 150–157. doi:10.1086/321530.0004-637Xhttp://nrs.harvard.edu/urn-3:HUL.InstRepos:30212163BeppoSAX observed the Seyfert 1.9 galaxy NGC 4258 in 1998 December, when its 2-10 keV luminosity was about 1041 ergs s-1. Large amplitude (100%) variability is observed in the 3-10 keV band on timescales of a few tens of thousands of seconds, while variability of ~20% is observed on timescales as short as 1 hr. The nuclear component is visible above 2 keV only, being obscured by a column density of (9.5 ± 1.2) × 1022 cm-2; this component is detected at up to 70 keV with a signal-to-noise ratio of gsim3 and with a steep power-law energy spectral index of αE = 1.11 ± 0.14. Bremsstrahlung emission for the 2-70 keV X-ray luminosity, as expected in advection-dominated accretion flow models with strong winds, is ruled out by the data. The ratio between the nuclear radio (22 GHz) luminosity and the X-ray (5 keV) luminosity is consistent with that of radio-quiet quasars and Seyfert galaxies. X-ray variability, spectral shape, and radio/X-ray and near-IR/X-ray luminosity ratios suggest that the nucleus of NGC 4258 could be a scaled down version of a Seyfert nucleus and that the X-ray nuclear luminosity can be explained in terms of Comptonization in a hot corona. The soft (E lesssim 2 keV) X-ray emission is complex. There are at least two thermal-like components with temperatures of 0.6 ± 0.1 keV and gsim1.3 keV. The cooler (L0.1-2.4 keV~ 1040 ergs s-1) component is probably associated with the jet, resolved in X-rays by the ROSAT HRI (Cecil et al. 1994). The luminosity of the second component, which can be modeled equally well by an unobscured power-law model with αE = 0.2img1.gif, is L0.1-2.4 keV~ 7 × 1039 ergs s-1, consistent with that expected from discrete X-ray sources (binaries and supernova remnants) in the host galaxy. Observations of NGC 4258 and other maser active galactic nuclei (AGNs) show strong nuclear X-ray absorption. We propose that this large column of gas might be responsible for shielding the regions of water maser emission from X-ray illumination. So a large column density absorbing gas may be a necessary property of masing AGNs.en-USGalaxies: individual (NGC 4258)Galaxies: SeyfertX-rays: galaxiesJournal Article2017-02-1310.1086/321530