The nature of the hard X-ray power-law tail in M87

I); M.Guainazzi (1); Milano; NL; (2) IFC "Occhialini" C.N.R.; Noordwijk; S.Molendi (2) ((1) Astrophysics Division; SSD of ESA

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The nature of the hard X-ray power-law tail in M87

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arxiv astro-ph/9910271 v1 pith:NHA3W3AI submitted 1999-10-14 astro-ph

M.Guainazzi (1) , S.Molendi (2) ((1) Astrophysics Division , SSD of ESA , Noordwijk , NL; (2) IFC "Occhialini" C.N.R. , Milano , I) This is my paper · ORCID

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keywords hardpower-lawradialtailx-rayabundanceaccretionallen

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Spatially-resolved spectroscopy of the elliptical galaxy M87 with the MECS instrument on board BeppoSAX demonstrates that the hard X-ray power-law tail, originally discovered by ASCA (Matsumoto et al 1996; Allen et al. 1999), originates in the innermost 2'. Our results are consistent with it being produced in an Accretion Dominated Flow, although a substantial jet contribution cannot be ruled out. An origin from a Seyfert-like nucleus is disfavored by our data. As a by-product of this result, we present an analysis of the thermal emission coming from the center of the Virgo cluster, which exhibits a strong positive radial temperature gradient, along with a radial decrease of the iron abundance.

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