2009/03/25 by T. J. Turner, L. Miller, S. B. Kraemer +2 · 2 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics and Star Formation Studies #Extrapolation #Luminosity #Optical depth #RADIUS #Radiative transfer #Solar and Space Plasma Dynamics #astro-ph.CO #astro-ph.HE
paper · pdf · doi:10.1088/0004-637x/698/1/99
published as Astrophys.J.698:99-105,2009 · Accepted for publication in ApJ. 14 pages, 4 color figures
arxiv created 2009/03/25 · openalex publication_date 2009/05/19 · arxiv updated 2011/02/11 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We present results from a 200 ks Suzaku observation of 1H 0419 − 577 taken during 2007 July. The source shows a strong excess of counts above 10 keV compared to the extrapolation of models based on previous data in the 0.5–10 keV band. The "hard excess" in 1H 0419 − 577 can be explained by the presence of a Compton-thick partial-covering absorber that covers ∼70% of the source. The Compton-thick gas likely originates from a radius inside of the optical broad-line region and may form part of a clumpy disk wind. The fluorescent Fe Kα luminosity measured by Suzaku is consistent with that expected from an equatorial disk wind.