On the origin of the X-rays and the nature of accretion in NGC 4261

Details On the origin of the X-rays and the nature of accretion in NGC 4261 On the origin of the X-rays and the nature of accretion in NGC 4261

2003-06-24

arxiv.org/abs/astro-ph/0306510v1

Astron.Astrophys.408:949-960,2003

Astronomy and Astrophysics

Astrophysics

12 pages, 6 figures, accepted for publication in A&A

Scientific paper

10.1051/0004-6361:20031050

We report on the X-ray properties of the radio galaxy NGC 4261, combining information from the XMM, Chandra, and SAX satellites. Goals of this study are to investigate the origin of the X-rays from this low-power radio galaxy and the nature of the accretion process onto the central black hole. The X-ray spectrum of the nuclear source extending up to 100--150 keV is well described by a partially covered (covering factor $>$ 0.8) power law with a photon index \~1.5 absorbed by a column density 5e22 cm^-2. The X-ray luminosity associated with the non-thermal component is ~5e41 erg/s. The nuclear source is embedded in a diffuse hot gas (kT~0.6 keV), whose density profile implies a Bondi accretion rate of 4.5e-2 solar masses/year. For the first time rapid X-ray variability is detected in a low-power radio galaxy at more than 99% confidence level. The observed X-ray spectral and variability properties indicate the accretion flow as the most likely origin of the bulk X-ray continuum.This conclusion is strengthened by energetic considerations based on a comparison between the X-ray luminosity and the kinetic power of the jet, whichalso suggest that the Bondi accretion rate overestimates the actual accretion rate onto the black hole.

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