The nuclear accretion in the FR I radio galaxy IC4296 from CHANDRA and VLBA observations

Details The nuclear accretion in the FR I radio galaxy IC4296 from CHANDRA and VLBA observations The nuclear accretion in the FR I radio galaxy IC4296 from CHANDRA and VLBA observations

2002-11-14

arxiv.org/abs/astro-ph/0211322v1

Astrophys.J. 585 (2003) 677-686

Astronomy and Astrophysics

Astrophysics

29 pages, 10 figures (Figs. 1 and 2 are color figures). To be published in ApJ

Scientific paper

10.1086/346184

A high angular resolution study of the nucleus of the FR I galaxy IC4296 using Chandra ACIS-S and VLBA observations is presented, with the aim of studying the nature of the accretion process. Pointlike and hard X-ray emission is found, well described by a moderately absorbed power law of Gamma=1.48^{+0.42}_{-0.34}; no iron fluorescence line from cold material is detected. The 0.3-10 keV luminosity is 2.4\times 10^{41} erg/s, that is \sim 400 times lower than the accretion luminosity resulting from the estimated Bondi mass accretion rate and a radiative efficiency of 10%. On the parsec scale a jet and a counter-jet extend out from a central unresolved ``core'' in the 8.4 GHz image. Their orientation is in good agreement with that of the large scale jets and their bulk speed is relativistic. The parsec scale spectrum is convex over 2-22 GHz. The observed nuclear luminosity is not likely to be reconciled with the accretion luminosity by assuming that Compton thick material surrounds the nucleus. Low radiative efficiency accretion flow models (ADAF and its variants) cannot account for the observed emission and spectral shape of the nucleus in the radio band. The power in the jets accounts for a sizable fraction (\ga 10%) of the accretion luminosity; therefore the mass accretion rate needs not to be much different from the estimate obtained using Bondi's theory. A jet dominated origin also for the observed radiative losses of the nucleus is suggested. This could also explain the finding that a nuclear luminosity orders of magnitude lower than that of ``normal'' radio loud AGNs is accompanied by a relatively higher radio emission.

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