TY - JOUR
T1 - Simultaneous XMM-newton and HST-COS observation of 1H0419-577
T2 - The absorbing and emitting ionized gas
AU - Di Gesu, L.
AU - Costantini, E.
AU - Arav, N.
AU - Borguet, B.
AU - Detmers, R. G.
AU - Ebrero, J.
AU - Edmonds, D.
AU - Kaastra, J. S.
AU - Piconcelli, E.
AU - Verbunt, F.
N1 - Funding Information:
This work is based on observations with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). SRON is supported financially by NWO, the Netherlands Organization for Scientific Research. N.A. acknowledge support from NASA grants NNX09AT29G and HST-GO-11686.
PY - 2013
Y1 - 2013
N2 - In this paper we analyze the X-ray, UV, and optical data of the Seyfert 1.5 galaxy 1H0419-577 with the aim of detecting and studying an ionized-gas outflow. The source was observed simultaneously in the X-rays with XMM-Newton and in the UV with HST-COS. Optical data were also acquired with the XMM-Newton Optical Monitor. We detected a thin, lowly ionized warm absorber (log ξ ≈ 0.03, log NH ≈ 19.9 cm-2) in the X-ray spectrum, which is consistent to be produced by the same outflow already detected in the UV. Provided the gas density estimated in the UV, the outflow is consistent to be located in the host galaxy at ∼kpc scale. Narrow emission lines were detected in the X-rays, in the UV and also in the optical spectrum. A single photoionized-gas model cannot account for all the narrow lines emission, indicating that the narrow line region is probably a stratified environment, differing in density and ionization. X-ray lines are unambiguously produced in a more highly ionized gas phase than the one emitting the UV lines. The analysis also suggests that the X-ray emitter may just be a deeper portion of the same gas layer producing the UV lines. Optical lines are probably produced in another disconnected gas system. The different ionization condition and the ∼pc scale location, suggested by the line width for the narrow lines emitters, are evidences against a connection between the warm absorber and the narrow line region in this source.
AB - In this paper we analyze the X-ray, UV, and optical data of the Seyfert 1.5 galaxy 1H0419-577 with the aim of detecting and studying an ionized-gas outflow. The source was observed simultaneously in the X-rays with XMM-Newton and in the UV with HST-COS. Optical data were also acquired with the XMM-Newton Optical Monitor. We detected a thin, lowly ionized warm absorber (log ξ ≈ 0.03, log NH ≈ 19.9 cm-2) in the X-ray spectrum, which is consistent to be produced by the same outflow already detected in the UV. Provided the gas density estimated in the UV, the outflow is consistent to be located in the host galaxy at ∼kpc scale. Narrow emission lines were detected in the X-rays, in the UV and also in the optical spectrum. A single photoionized-gas model cannot account for all the narrow lines emission, indicating that the narrow line region is probably a stratified environment, differing in density and ionization. X-ray lines are unambiguously produced in a more highly ionized gas phase than the one emitting the UV lines. The analysis also suggests that the X-ray emitter may just be a deeper portion of the same gas layer producing the UV lines. Optical lines are probably produced in another disconnected gas system. The different ionization condition and the ∼pc scale location, suggested by the line width for the narrow lines emitters, are evidences against a connection between the warm absorber and the narrow line region in this source.
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U2 - 10.1051/0004-6361/201321416
DO - 10.1051/0004-6361/201321416
M3 - Article
AN - SCOPUS:84881253986
SN - 0004-6361
VL - 556
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A94
ER -