2003/01/15 by G. Fabbiano, M. Elvis, Sera Markoff +10 · 1 citation
Physics and Astronomy · #Accretion (finance) #Active galactic nucleus #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Cosmic Phenomena #Black hole (networking) #Eddington luminosity #Galaxies: Formation, Evolution, Phenomena #Galaxy #Luminosity #Physics #Quasar #RADIUS #Spectral line #Supermassive black hole #astro-ph
paper · pdf · doi:10.1086/374040
published as Astrophys.J. 588 (2003) 175-185 · 33 pages including 7 figures (1 full color, 2 with colored lines) and 5 tables. Astrophysical Journal, in press
arxiv created 2003/01/15 · openalex publication_date 2003/05/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Chandra observations of the supermassive black hole in the nucleus of IC 1459 show a weak ( L X = 8 × 10 40 ergs s -1 , 0.3-8 keV), unabsorbed nuclear X-ray source, with a slope Γ = 1.88 ± 0.09, and no strong Fe K line at 6.4 keV (EW < 382 eV). This describes a normal active galactic nucleus (AGN) X-ray spectrum but lies at 3 × 10 -7 below the Eddington limit. The spectral energy distribution of the IC 1459 nucleus is extremely radio-loud compared to normal radio-loud quasars. The nucleus is surrounded by a hot interstellar medium ( kT ~ 0.5-0.6 keV) with an average density of 0.3 cm -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 ergs s -1 , nearly 4 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-100 μm 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.