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XMM-Newton Observation of Fe Kalpha emission from a BAL QSO: Mrk 231

T. J. Turner·S. B. Kraemer
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Abstract

We present results from a 20 ksec XMM observation of Mrk 231. EPIC data reveal strong line emission due to Fe Ka, which has rarely been detected in this class. The line energy is consistent with an origin in neutral Fe and the width equivalent to a velocity dispersion ~ 18,000 km/s, thus the line may be attributed to transmission and/or reflection from a distribution of emitting clouds. If, instead, the line originates in the accretion disk then the line strength and flat X-ray continuum support some contribution from reflection, although the data disfavor a model where the hard X-ray band is purely reflected X-rays from a disk. Line parameters are similar to those obtained for the BAL QSO, H1413+117.

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T. J. Turner, S. B. Kraemer. 2003-08-14. XMM-Newton Observation of Fe Kalpha emission from a BAL QSO: Mrk 231. https://doi.org/10.1086/379100

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