A direct view of the AGN powering IRAS12393+3520

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dc.creatorGuainazzi, M.
dc.creatorDennefeld, M.
dc.creatorPiro, L.
dc.creatorBoller, T.
dc.creatorRafanelli, P.
dc.creatorYamauchi, M.
dc.date2000-01-21
dc.date.accessioned2026-07-07T01:51:49Z
dc.date.available2026-07-07T01:51:49Z
dc.descriptionWe report the first direct X-ray evidence that an AGN is hidden in the center of IRAS12393+3520. An ASCA observation of this target unveiled a bright (0.5-10 keV luminosity 3.9 x 10^42 erg/s) and variable source, with minimum observed doubling/halving time scale comprised in the range 30-75 ks. A model composed by a simple power-law, with photon index ~1.8 and an absorption edge, whose threshold energy is consistent with K-shell photoionization of OVII, provides an adequate fit of the spectrum. This suggests that we are observing the emission from the nuclear region through a warm absorber of N_H a few 10^{21}/cm/cm. If it has internal dust with Galactic gas-to-dust ratio, it could explain the lack of broad Hbeta emission, even in the episodic presence of a broad Halpha emission line. Optical spectra obtained over several years show indeed variations in the strength of this broad Halpha component. A distribution of dusty, optically thick matter on spatial scales a few hundreds parsec, which does not intercept the line of sight towards the nucleus, is probably required to account simultaneously for the relative [OIII] luminosity deficit in comparison to the X-rays. The high IR to X-ray luminosity ratio is most likely due to intense star formation in the circumnuclear region. IRAS12393+3520 might thus exhibit simultaneously nuclear activity and remarkable star formation.
dc.description9 Latex pages, 8 figures, Accepted for publication in Astronomy & Astrophysics
dc.identifierhttps://arxiv.org/abs/astro-ph/0001371
dc.identifierhttp://arxiv.org/abs/astro-ph/0001371
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/425
dc.subjectAstrophysics
dc.titleA direct view of the AGN powering IRAS12393+3520
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