Open AccessIRAS 13197−1627 has them all: Compton‐thin absorption, photoionized gas, thermal plasmas and a broad Fe line ★
Author(s) -
Miniutti G.,
Ponti G.,
Dadina M.,
Cappi M.,
Malaguti G.
Publication year - 2007
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2006.11291.x
Subject(s) - physics , astrophysics , spectral line , galaxy , plasma , line (geometry) , absorption (acoustics) , emission spectrum , accretion (finance) , active galactic nucleus , spectral resolution , reflection (computer programming) , astronomy , optics , nuclear physics , geometry , mathematics , computer science , programming language
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 ( N H ∼ 4 × 10 23 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 × 10 3 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 .