Catalogue of ionized emission line spectra in obscured AGN

Guainazzi, M.; Barbarisi, I.; Bianchi, S.; Osuna, P.; Salgado, J.

doi:10.1016/j.asr.2007.07.006

Cited by 2 publications

(2 citation statements)

References 20 publications

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“…photoionization), suggest that the emitting gas in Fairall 9 could be probably part of a nuclear wind driven out by radiation pressure. This same evidence is found in numerous other Seyfert galaxies, both absorbed (Guainazzi et al 2008) and unabsorbed (Bianchi et al 2009). It is commonly interpreted as a biconical outflow, launched from the innermost region of the AGN and spatially colocated with the optical ionization cones frequently seen in O iii emission in type II Seyfert galaxies (Ogle et al 2000; Bianchi, Guainazzi & Chiaberge 2006).…”

Section: Summary and Discussionsupporting

confidence: 84%

An XMM-Newton view of the ‘bare’ nucleus of Fairall 9★

Emmanoulopoulos

Papadakis

McHardy

et al. 2011

Monthly Notices of the Royal Astronomical Society

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We present the spectral results from a 130-ks observation, obtained from the X-ray Multi-Mirror Mission-Newton (XMM-Newton) observatory, of the type I Seyfert galaxy Fairall 9. An X-ray hardness ratio analysis of the light curves reveals a 'softer-when-brighter' behaviour which is typical of radio-quiet type I Seyfert galaxies. Moreover, we analyse the high spectral resolution data of the reflection grating spectrometer and we do not find any significant evidence supporting the presence of warm absorber in the low X-ray energy part of the source's spectrum. This means that the central nucleus of Fairall 9 is 'clean' and thus its X-ray spectral properties probe directly the physical conditions of the central engine. The overall X-ray spectrum in the 0.5-10 keV energy range, derived from the EPIC data, can be modelled by a relativistically blurred disc reflection model. This spectral model yields for Fairall 9 an intermediate black hole best-fitting spin parameter of α = 0.39 +0.48 −0.30 .

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Section: Summary and Discussionsupporting

confidence: 84%

An XMM-Newton view of the ‘bare’ nucleus of Fairall 9★

Emmanoulopoulos

Papadakis

McHardy

et al. 2011

Monthly Notices of the Royal Astronomical Society

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“…We therefore conclude that the NLR in NGC 5548 is compact in size, is in the form of clouds with a small covering factor or a narrow stream, has a cone-like geometry and is located between 1 and 15 pc from the central source, which is much smaller than the observed extended emission cones in Seyfert 2 galaxies (Kinkhabwala et al 2002;Guainazzi et al 2008). One reason for this compactness could be that in Seyfert 2 galaxies, we can not observe the high density, high emissivity NLR gas that we observe here, since the torus blocks our view.…”

Section: Discussionmentioning

confidence: 85%

X-ray narrow line region variability as a geometry probe

Detmers¹,

Kaastra

McHardy

2009

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We study the long time scale variability of the gas responsible for the X-ray narrow emission lines in the Seyfert 1 galaxy NGC 5548, in order to constrain the location and geometry of the emitting gas. Using X-ray spectra taken with the Chandra−LETGS and HETGS instruments and with XMM−Newton RGS and combining them with long-term monitoring observations of the Rossi X-ray Timing Explorer (RXTE), we perform a correlation analysis in order to try to constrain the time scale on which the narrow line emitting gas responds to variations of the continuum flux. With the inclusion of the 2007 Chandra−LETGS observation we have an additional observation at an historically low flux level. We conclude that the NLR in NGC 5548 is in the form of an ionization cone, compact in size, and located between 1 and 15 pc from the central source, depending on the exact geometry of the NLR.

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Catalogue of ionized emission line spectra in obscured AGN

Cited by 2 publications

References 20 publications

An XMM-Newton view of the ‘bare’ nucleus of Fairall 9★

An XMM-Newton view of the ‘bare’ nucleus of Fairall 9★

X-ray narrow line region variability as a geometry probe

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