<i>XMM-NEWTON</i>OBSERVATIONS OF SDSS J143030.22 – 001115.1: AN UNUSUALLY FLAT-SPECTRUM ACTIVE GALACTIC NUCLEUS

Mathur, S.; Golowacz, E. C.; Williams, R.; Pogge, Richard W.; Fields, Dale L.; Grupe, D.

doi:10.1088/0004-6256/138/6/1655

Cited by 2 publications

(1 citation statement)

References 32 publications

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“…Unusually flat spectral slopes have been often found to be due to a partially-covering ionised absorber (see, e.g., Piconcelli et al 2004;Mathur et al 2009;Svoboda et al 2012). As the next step, we therefore employed a partially-covering ionised absorption to model the absorption features in the spectra.…”

Section: Modelling the Complex Absorptionmentioning

confidence: 99%

An X-ray variable absorber within the broad line region in Fairall 51

Svoboda

Guainazzi

Longinotti

et al. 2015

A&A

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Context. Fairall 51 is a polar-scattered Seyfert 1 galaxy, a type of active galaxy believed to represent a bridge between unobscured type-1 and obscured type-2 objects. Fairall 51 has shown complex and variable X-ray absorption, but little is known about its origin. Aims. In our research, we observed Fairall 51 with the X-ray satellite Suzaku in order to constrain a characteristic time scale of its variability. Methods. We performed timing and spectral analysis of four observations separated by 1.5, 2, and 5.5 day intervals. Results. We found that the 0.5-50 keV broadband X-ray spectra are dominated by a primary power-law emission (with the photon index ∼2). This emission is affected by at least three absorbers with different ionisations (log ξ ≈ 1-4). The spectrum is shaped further by a reprocessed emission, possibly coming from two regions, the accretion disc and a more distant scattering region. The accretion disc emission is smeared by the relativistic effects, from which we measured the spin of the black hole as a ≈ 0.8 ± 0.2. We found that most of the spectral variability can be attributed to the least ionised absorber whose column density changed by a factor of two between the first (highest-flux) and the last (lowest-flux) observation. Conclusions. A week-long scale of the variability indicates that the absorber is located at the distance ≈0.05 pc from the centre, i.e., in the broad line region.

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Section: Modelling the Complex Absorptionmentioning

confidence: 99%

An X-ray variable absorber within the broad line region in Fairall 51

Svoboda

Guainazzi

Longinotti

et al. 2015

A&A

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XMM-NEWTONOBSERVATIONS OF THE RADIO-LOUD BROAD ABSORPTION LINE QUASAR FBQS J131213.5+231958

Mathur

Dai

2010

The Astronomical Journal

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We present XMM-Newton observations of the broad absorption line (BAL) quasar FBQS J131213.5+231958. The X-ray spectrum of the source can be well described by an absorbed power-law model in which the absorber is either ionized or only partially covers the continuum source. This can explain the apparent lack of absorption observed in the Chandra spectrum with low signal-to-noise ratio. While the power-law slope of the spectrum is similar to that of non-BAL radio-loud quasars, the Eddington luminosity ratio is likely to be significantly higher than the mean. This shows that in high-mass black holes (BHs), high Eddington accretion may not result in as steep of a spectrum as in lower-mass BHs. This provides important constraints for accretion disk models. It also provides support to the idea that BAL quasars, at least their radio-loud subclass, represent an early evolutionary stage of quasars.

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XMM-NEWTONOBSERVATIONS OF SDSS J143030.22 – 001115.1: AN UNUSUALLY FLAT-SPECTRUM ACTIVE GALACTIC NUCLEUS

Cited by 2 publications

References 32 publications

An X-ray variable absorber within the broad line region in Fairall 51

An X-ray variable absorber within the broad line region in Fairall 51

XMM-NEWTONOBSERVATIONS OF THE RADIO-LOUD BROAD ABSORPTION LINE QUASAR FBQS J131213.5+231958

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