2006/11/20 by G. Miniutti, G. Ponti, M. Dadina +2 · 2 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Galaxies: Formation, Evolution, Phenomena #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2006.11291.x
published as Mon.Not.Roy.Astron.Soc.375:227-239,2007 · accepted for publication in MNRAS
arxiv created 2006/11/20 · openalex publication_date 2007/01/18 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
We report results from the XMM–Newton observation of IRAS 13197−1627, a luminous infrared (IR) galaxy with a Seyfert 1.8 nucleus. The hard X-ray spectrum is steep (Γ∼ 2.5) and is absorbed by Compton-thin (NH∼ 4 × 1023 cm−2) neutral gas. We detect a Fe Kα emission line at 6.4 keV, consistent with transmission through the absorber. The most striking result of our spectral analysis is the detection of a dominant X-ray reflection component and broad Fe line from the inner accretion disc. The reflection-dominated hard X-ray spectrum is confirmed by the strong Compton hump seen in a previous BeppoSAX observation and could be the sign that most of the primary X-rays are radiated from a compact corona (or base of the jet) within a few gravitational radii from the black hole. We also detect a relatively strong absorption line at 6.81 keV which, if interpreted as Fe xxv resonant absorption, implies an outflow with velocity ∼5 × 103 km s−1. In the soft energy band, the high-resolution gratings and the CCD-resolution data show the presence of both photoionized gas and thermal plasma emission, the latter being most likely associated with a recent starburst of 15–20 M⊙ yr−1.