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The BeppoSAX view of the X-ray active nucleus of NGC4258

F. Fiore·S. Pellegrini·G. Matt·L. A. Antonelli·A. Comastri·R. Della Ceca·E. Giallongo·S. Mathur·S. Molendi·A. Siemiginowska·G. Trinchieri·B. Wilkes
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Abstract

BeppoSAX observed NGC4258 on December 1998, when its 2-10 keV luminosity was \~1E41 erg/s. 100% variability is observed in the 3-10 keV band on timescales of a half a day while 20% variability is observed on timescales of one hour. The nuclear component is visible above 2 keV only, being obscured by a column density of (9.5+/-1.2)E22 cm-2; this component is detected up to 70 keV with S/N>=3 and with the steep power law energy index of 1.11+/-0.14. Bremsstrahlung emission for the 2-70 keV X-ray luminosity, as expected in ADAF models with strong winds, is ruled out by the data. The ratio between the nuclear radio and the X-ray luminosities is <=1E-5, similar to that of radio quiet AGN. X-ray variability and spectral shape, radio to X-ray and NIR to X-ray luminosity ratios suggest that the nucleus of NGC4258 could be a scaled-down version of a Seyfert nucleus. The soft (E<=2keV) X-ray emission is complex. There are at least two thermal-like components, with T1=0.6+/-0.1 keV and T2>=1.3 keV. The cooler (L(0.1-2.4keV)=1E40 erg/s) component is probably associated with the jet, resolved in X-rays by the ROSAT HRI. The second component, which can be modeled equally well by an unobscured power law model, has L(0.1-2.4keV)~7E39 erg/s, consistent with that expected from discrete X-ray sources in the host galaxy. NGC4258 and other maser AGNs show strong nuclear X-ray absorption. We propose that this large column of gas might be responsible for shielding the regions of maser emission from X-ray illumination. So a large column density gas may be a necessary property of masing AGNs.

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F. Fiore, S. Pellegrini, G. Matt, L. A. Antonelli, A. Comastri, R. Della Ceca, E. Giallongo, S. Mathur, S. Molendi, A. Siemiginowska, G. Trinchieri, B. Wilkes. 2001-02-26. The BeppoSAX view of the X-ray active nucleus of NGC4258. https://doi.org/10.1086/321530

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