The optical to X-ray spectrum of the broad-line ultrasoft AGN RE J2248-511

Details The optical to X-ray spectrum of the broad-line ultrasoft AGN RE J2248-511 The optical to X-ray spectrum of the broad-line ultrasoft AGN RE J2248-511

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004adspr..34.2588s&link_type=abstract

Advances in Space Research, Volume 34, Issue 12, p. 2588-2593.

Computer Science

1

Scientific paper

We present a series of monitoring observations of the ultrasoft broad-line Seyfert galaxy RE J2248-511 with XMM-Newton. Previous X-ray observations showed a transition from a very soft state to a harder state five years later. We find that the ultrasoft X-ray excess has re-emerged, yet there is no change in the hard power-law. Reflection models with a reflection fraction of ⩾15, and Comptonisation models with two components of different temperatures and optical depths (kT1 = 83 keV, T1 = 30 eV, τ1 = 0.8; KT2 = 3.5 keV, T2 = 60 eV, τ2 = 2.8) can be fit to the spectrum, but cannot be constrained. The best representation of the spectrum is a model consisting of two blackbodies (kT1 = 0.09 ± 0.01 keV, kT2 = 0.21 ± 0.03 keV) plus a power-law (Γ = 1.8 ± 0.08). We also present simultaneous optical and infrared data showing that the optical spectral slope also changes dramatically on timescales of years. If the optical to X-ray flux comes primarily from a Comptonised accretion disk we obtain estimates for the black hole mass ˜108M˙&sun;, accretion rate ˜0.8M˙Edd and inclination cos(i) ⩾ 0.8 of the disk.

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