BeppoSAX observations of Narrow-Line Seyfert 1 galaxies

Comastri, A.; Stirpe, G. M.; Vignali, C.; Brandt, W. N.; Leighly, K. M.; Fiore, F.; Guainazzi, M.; Matt, Giorgio; Nicastro, F.; Puchnarewicz, E. M.; Siemiginowska, Aneta

doi:10.1051/0004-6361:20000152

Cited by 40 publications

(77 citation statements)

References 52 publications

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“…It represents 45 ± 3% of the intrinsic source flux in that band after correction for Galactic absorption and less than 1% of the intrinsic source flux above 2 keV. Evidence for ionized accretion discs have been found in particular in narrow line Seyfert 1 galaxies (TON S 180: Comastri et al 1998;Turner et al 1998;Ark 564: Vaughan et al 1999;Gondoin et al 2002). These conclusions are based on either the energy centroid of the observed Fe Kα line or on spectral fits using the PEXRIV ionized disc model of Magdziarz & Zdziarski (1995).…”

Section: Analysis Of the Soft Energy Rangementioning

confidence: 97%

XMM–Newtonobservations of the Seyfert 1 galaxy ESO 141–G55

Gondoin

Orr

Lumb

2003

A&A

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Abstract.We report on an observation of the Seyfert 1 galaxy ESO 141-G55 performed in October 2001 with the EPIC MOS cameras and Reflection Grating Spectrometers (RGS) on board the XMM-Newton observatory. We find the hard (3-10 keV) continuum slope, including reflection, to be somewhat flatter (Γ = 1.72 ± 0.06) than that of a typical broad-line Seyfert 1 galaxy. The spectrum shows a weak emission line at 6.45 ± 0.04 keV with a measured equivalent width of ≈40 eV. A broad spectral feature is observed around 7 keV that can be fitted by an absorption edge at 7.6 ± 0.1 keV. The extrapolation of the primary power law continuum to energies lower than 2 keV indicates the presence of a soft excess component contributing to 45 ± 3% of the overall flux in the 0.3−2.0 keV energy range. This soft-excess cannot be explained solely by enhanced reflection from a highly ionized disk.

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Section: Analysis Of the Soft Energy Rangementioning

confidence: 97%

XMM–Newtonobservations of the Seyfert 1 galaxy ESO 141–G55

Gondoin

Orr

Lumb

2003

A&A

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“…Turner et al 2001;Comastri et al 2001;Romano et al 2002) suggests the particulars of the disk in Mrk 766 may be a characteristic of the NLSy1 class and one that could give us insight into these systems. For example, a high rate of magnetic reconnection events in NLSy1s might naturally explain both their rapid X-ray continuum flux variability and the nature of the Fe line emission, one might then look for a link between high accretion rate and rate of magnetic reconnections.…”

Section: Emission From Materials Close To the Black Holementioning

confidence: 99%

Evidence for orbital motion of material close to the central black hole of Mrk 766

Turner¹,

Miller

George³

et al. 2005

A&A

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Time-resolved X-ray spectroscopy has been obtained for the narrow line Seyfert galaxy Mrk 766 from XMM-Newton observations. We present analysis in the energy-time plane of EPIC pn data in the 4−8 keV band with energy resolution R 50. A component of Fe Kα emission detected in the maps shows a variation of photon energy with time that appears both to be statistically significant and to be consistent with sinusoidal variation. We investigate the interpretation that there exists a component of line emission from matter in a Keplerian orbit around a supermassive black hole. The orbit has a period ∼165 ks and a line-of-sight velocity ∼13 500 km s −1 . This yields a lower limit for the central mass of M > 4.9 × 10 5 M within a radius of 3.6 × 10 13 cm (2.4 AU). The orbit parameters are consistent with higher black hole masses, but the lack of any substantial gravitational redshift of the orbit implies an upper limit to the black hole mass of 4.5 × 10 7 M .

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“…This object is a strong UV and X-ray source (Boller et al 1996 ;Crenshaw et al 1999 ;Comastri et al 2001 ;Ballantyne et al 2001). The near-IR spectrum is dominated by He I j10830 and the H I Paschen lines (Fig.…”

Section: Mrk 335mentioning

confidence: 99%

Infrared FeiiEmission in Narrow‐Line Seyfert 1 Galaxies

Rodríguez-Ardila

Viegas

Pastoriza

et al. 2002

ApJ

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We obtained 0.8È2.4 km spectra at a resolution of 320 km s~1 of four narrow-line Seyfert 1 galaxies in order to study the near-infrared properties of these objects. We focus on the analysis of the Fe II emission in that region and the kinematics of the low-ionization broad lines. We show that the 1 km Fe II lines (j9997, j10501, j10863, and j11126) are the strongest Fe II lines in the observed interval. For the Ðrst time, primary cascade lines of Fe II arising from the decay of upper levels pumped by Lya Ñuores-cence are resolved and identiÐed in active galactic nuclei. Excitation mechanisms leading to the emission of the 1 km Fe II features are discussed. A combination of Lya Ñuorescence and collisional excitation is found to be the main contributor. The Ñux ratio between near-IR Fe II lines varies from object to object, in contrast to what is observed in the optical region. A good correlation between the 1 km and optical Fe II emission is found. This suggests that the upper z4F0 and z4D0 levels from which the bulk of the optical Fe II lines descend are mainly populated by the transitions leading to the 1 km lines. The width and proÐle shape of Fe II j11127, Ca II j8642, and O I j8446 are very similar but signiÐcantly narrower than Pab, giving strong observational support to the hypothesis that the regions where Fe II, Ca II, and O I are produced are cospatial, interrelated kinematically, and most probably located in the outermost portion of the broad-line region.

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BeppoSAX observations of Narrow-Line Seyfert 1 galaxies

Cited by 40 publications

References 52 publications

XMM–Newtonobservations of the Seyfert 1 galaxy ESO 141–G55

XMM–Newtonobservations of the Seyfert 1 galaxy ESO 141–G55

Evidence for orbital motion of material close to the central black hole of Mrk 766

Infrared FeiiEmission in Narrow‐Line Seyfert 1 Galaxies

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