Complex resonance absorption structure in the X-ray spectrum of IRAS 13349+2438

Šako, M.; Kahn, S. M.; Behar, E.; Kaastra, J. S.; Brinkman, A. C.; Boller, Th.; Puchnarewicz, E. M.; Starling, R.; Liedahl, D. A.; Clavel, J.; Santos-Lleo, M.

doi:10.1051/0004-6361:20000081

Cited by 177 publications

(206 citation statements)

References 25 publications

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“…Only in the case of Mrk 110 and CTS A08.12 do we see a feature between 15 and 17 Å in absorption that can be associated with the Fe-L UTA (Unresolve Transition Array), which is the characteristic signature of warm absorbers (Sako et al 2001). We tested for the presence of warm absorption related with these sources using PHASE (Krongold et al 2003), but in neither case have we found a satisfactory result that would inprove the model fitting.…”

Section: High-resolution Spectral Featuresmentioning

confidence: 97%

A comprehensive approach to analyzing theXMM-Newtondata of Seyfert 1 galaxies

Cardaci

Santos-Lleó

Hägele

et al. 2011

A&A

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Aims. We seek a comprehensive analysis of all the information provided by the XMM-Newton satellite of the four Seyfert 1 galaxies ESO 359-G19, HE 1143-1810, CTS A08.12, and Mrk 110, including the UV range, to characterize the different components that are emitting and absorbing radiation in the vicinity of the active nucleus. Methods. The continuum emission was studied through the EPIC spectra by taking advantage of the spectral range of these cameras. The high-resolution RGS spectra were analyzed to characterize the absorbing and emission line features that arise in the spectra of the sources. All these data, complemented by information in the UV, are analyzed jointly in order to achieve a consistent characterization of the observed features in each object. Results. The continuum emission of the sources can be characterized either by a combination of a power law and a black body for the weakest objects or by two power law components for the brightest ones. The continuum is not absorbed by neutral or ionized material in the line of sight to any of these sources. In all of them we have identified a narrow Fe-Kα line at 6.4 keV. In ESO 359-G19 we also find an Fexxvi line at about 7 keV. In the soft X-rays band, we identify only one Ovii line in the spectra of HE 1143-1810 and CTS A08.12, and two Ovii-Heα triplets and a narrow Oviii-Lyα emission line in Mrk 110. Conclusions. Not detecting warm material in the line of sight to the low state objects is due to intrinsically weaker or absent absorption in the line of sight and not to a low signal-to-noise ratio in the data. Besides this, the absence of clear emission lines cannot be fully attributed to dilution of those lines by a strong continuum.

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Section: High-resolution Spectral Featuresmentioning

confidence: 97%

A comprehensive approach to analyzing theXMM-Newtondata of Seyfert 1 galaxies

Cardaci

Santos-Lleó

Hägele

et al. 2011

A&A

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“…For iron, which has a best-fit value 2.5σ below the protosolar ratio, some of the stronger lines are notably weaker in the best-fit model, but the main difference is in the absorption due to the unresolved transition array (UTA between 16 and 17.5 Å, Sako et al 2001;Behar et al 2001), because the many absorption lines result in pseudo-continuum absorption. The spacing of 2.68 Å and 3.18 Å between the points of the spline used to fit the continuum in the range 14−18 Å is wider than the UTA, which has a width of about 1.5 Å.…”

Section: Derived Abundancesmentioning

confidence: 99%

Multiwavelength campaign on Mrk 509

Steenbrugge

Kaastra

Detmers

et al. 2011

A&A

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Context. The study of abundances in the nucleus of active galaxies allows us to investigate the evolution of the abundance by comparing local and higher redshift galaxies. However, the methods used so far have substantial drawbacks or rather large uncertainties. Some of the measurements are at odds with the initial mass function derived from the older stellar population of local elliptical galaxies. Aims. We determine accurate and reliable abundances of C, N, Ne, and Fe relative to O from the narrow absorption lines observed in the X-ray spectra of Mrk 509. Methods. We use the stacked 600 ks XMM-Newton RGS and 180 ks Chandra LETGS spectra. Thanks to simultaneous observations with INTEGRAL and the optical monitor on-board XMM-Newton for the RGS observations and HST-COS and Swift for the LETGS observations, we have an individual spectral energy distribution for each dataset. Owing to the excellent quality of the RGS spectrum, the ionisation structure of the absorbing gas is well constrained, allowing for a reliable abundance determination using ions over the whole observed range of ionisation parameters. Results. We find that the relative abundances are consistent with the proto-solar abundance ratios: C/O = 1.19 ± 0.08, N/O = 0.98 ± 0.08, Ne/O = 1.11 ± 0.10, Mg/O = 0.68 ± 0.16, Si/O = 1.3 ± 0.6, Ca/O = 0.89 ± 0.25, and Fe/O = 0.85 ± 0.06, with the exception of S, which is slightly under-abundant, S/O = 0.57 ± 0.14. Our results, and their implications, are discussed and compared to the results obtained using other techniques to derive abundances in galaxies.

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“…Recent XMM-Newton observations of the radio-quiet quasar Mrk 205 might provide the first evidence for a dust-torus in a quasar (Reeves et al 2001). XMM-data of IRAS 13349+2438 suggest column-densities which are consistent with a dusty torus (Sako et al 2001). Observations impose important constraints on the properties of such tori.…”

Section: Introductionmentioning

confidence: 97%

Binary black holes and tori in AGN

Zier

Biermann

2001

A&A

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Abstract.Observations of HST and groundbased data strongly suggest that most galaxies harbour central supermassive black holes and that most galaxies merge with others. Consequently a black hole binary emerges as the two black holes are spiraling into the center towards each other. In our work we are investigating two basic questions of our understanding of the central activity of galaxies and find that both can be answered with "yes": (1) Do the black holes actually merge? (2) And does the effect of the torque of the black hole binary on the surrounding stellar distribution help to explain the presence of the ubiquitous torus of molecular material surrounding apparently all active galactic nuclei? The first question is the topic of the present article, while the second question will be subject of a subsequent paper. Simulating the evolution of a stellar cluster in the potential of such a binary by solving the equations of the restricted three body problem we obtained the following results: provided that the cluster is about as massive as the black hole binary the two black holes coalesce after ∼10 7 yr due to ejection of stars and finally via emission of gravitational radiation. Whether a star is ejected or not crucially depends on its angular momentum. Almost all stars whose angular momentum is twice as large as that of a star circulating around the binary in a distance corresponding to that between the black holes, stay bound to the binary. In a sequence of models where the mass of the secondary black hole increases while M1 is fixed, a bigger fraction of stars is ejected. For a more massive binary also the cluster has to be more massive in order to allow the two black holes to coalesce. The merger then proceeds on smaller time scales. The cluster is depleted in the central region and the final distribution of stars assumes a torus-like structure, peaking at three times the initial distance of the two black holes. The relationship of the bound stars to the obscuring torus in active galactic nuclei will be investigated in a subsequent paper.

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Complex resonance absorption structure in the X-ray spectrum of IRAS 13349+2438

Cited by 177 publications

References 25 publications

A comprehensive approach to analyzing theXMM-Newtondata of Seyfert 1 galaxies

A comprehensive approach to analyzing theXMM-Newtondata of Seyfert 1 galaxies

Multiwavelength campaign on Mrk 509

Binary black holes and tori in AGN

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