SIMBAD references

2012MNRAS.426.2522P - Mon. Not. R. Astron. Soc., 426, 2522-2565 (2012/November-1)

A Suzaku survey of Fe K lines in Seyfert 1 active galactic nuclei.

PATRICK A.R., REEVES J.N., PORQUET D., MARKOWITZ A.G., BRAITO V. and LOBBAN A.P.

Abstract (from CDS):

We construct full broad-band models in an analysis of Suzaku observations of nearby Seyfert 1 active galactic nuclei (AGN) (z ≤ 0.2) with exposures >50ks and with greater than 30000 counts in order to study their iron line profiles. This results in a sample of 46 objects and 84 observations. After a full modelling of the broad-band Suzaku and Swift-Burst Alert Telescope data (0.6–100keV), we find complex warm absorption is present in 59 per cent of the objects in this sample which has a significant bearing upon the derived FeK region parameters. Meanwhile 35 per cent of the 46 objects require some degree of high column density partial coverer in order to fully model the hard X-ray spectrum. We also find that a large number of the objects in the sample (22 per cent) require high velocity, high ionization outflows in the FeK region resulting from FeXXV and FeXXVI. A further four AGN feature highly ionized FeK absorbers consistent with zero outflow velocity, making a total of 14/46 (30 per cent) AGN in this sample showing evidence for statistically significant absorption in the FeK region.

Narrow FeKα emission from distant material at 6.4keV is found to be almost ubiquitous in these AGN. Examining the 6–7keV FeK region we note that narrow emission lines originating from FeXXV at 6.63–6.70keV and from FeXXVI at 6.97keV are present in 52 and 39 per cent of objects, respectively.

Our results suggest statistically significant relativistic FeKα emission is detected in 23 of 46 objects (50 per cent) at >99.5 per cent confidence, measuring an average emissivity index of q = 2.4±0.1 and equivalent width \mo (\mi EW\mo)\mn 96=±\mn 10eV using the RELLINE model. When parametrized with a Gaussian we find an average line energy of 6.32±0.04keV, σwidth= 0.470±0.05keV and \mi EW==\mn 97=±\mn 19eV. Where we can place constraints upon the black hole spin parameter a, we do not require a maximally spinning black hole in all cases.

Alexander von Humboldt Fellow.


Abstract Copyright: © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS

Journal keyword(s): black hole physics - galaxies: active - galaxies: Seyfert - X-rays: galaxies

VizieR on-line data: <Available at CDS (J/MNRAS/426/2522): table1.dat table3.dat table4.dat tableb1.dat>

Simbad objects: 47

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2019.11.17-04:48:44

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