Status Report

The X-ray-faint Emission of the Supermassive Nuclear Black Hole of IC1459

By SpaceRef Editor
January 16, 2003
Filed under , ,

Astrophysics, abstract
astro-ph/0301297


From: Martin Elvis <[email protected]>
Date: Wed, 15 Jan 2003 17:26:25 GMT (102kb)

The X-ray-faint Emission of the Supermassive Nuclear Black Hole of
IC1459


Authors:
G. Fabbiano (1),
M. Elvis (1),
S. Markoff (2),
A. Siemiginowska (1),
S. Pellegrini (3),
A. Zezas (1),
F. Nicastro (1),
G. Trinchieri (4),
J. McDowell (1) ((1) Harvard-Smithsonian Center for Astrophysics, (2) Center for Space Research, MIT, (3) Universita’ di Bologna, Italy, (4) Osservatorio di Brera, Milano, Italy)

Comments: 33 pages including 7 figures (1 full color, 2 with colored lines) and
5 tables. Astrophysical Journal, in press


Chandra observations of the supermassive black hole in the nucleus of IC1459
show a weak [L_X=8×10(40)erg s(-1), 0.3-8keV], unabsorbed nuclear X-ray source,
with a slope Gamma=1.88+/-0.09, and no strong Fe-K line at 6.4keV (EW$<382 eV).
This describes a normal AGN X-ray spectrum, but lies at 3×10(-7) below the
Eddington limit. The SED of the IC1459 nucleus is extremely radio loud compared
to normal radio-loud quasars. The nucleus is surrounded by hot ISM (kT~0.5-0.6
keV) with an average density of 0.3cm(-3), within the central ~180 pc radius,
which is comparable to the gravitational capture radius, r_A~140 pc. We
estimate that for a standard AGN efficiency of 10%, the Bondi accretion would
correspond to a luminosity of ~6×10(44)erg s(-1), nearly four orders of
magnitude higher than L_X. ADAF solutions can explain the X-ray spectrum, but
not the high radio/X-ray ratio. A jet model fits the radio-100micron and X-ray
spectra well. The total power in this jet is ~10% of L(Bondi), implying that
accretion close to the Bondi rate is needed.

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