2018MNRAS.479..615M -
Mon. Not. R. Astron. Soc., 479, 615-634 (2018/September-1)
A high-density relativistic reflection origin for the soft and hard X-ray excess emission from Mrk 1044.
MALLICK L., ALSTON W.N., PARKER M.L., FABIAN A.C., PINTO C., DEWANGAN G.C., MARKOWITZ A., GANDHI P., KEMBHAVI A.K. and MISRA R.
Abstract (from CDS):
We present the first results from a detailed spectral-timing analysis of a long (∼130 ks) XMM-Newton observation and quasi-simultaneous NuSTAR and Swift observations of the highly accreting narrow-line Seyfert 1 galaxy Mrk 1044. The broad-band (0.3-50 keV) spectrum reveals the presence of a strong soft X-ray excess emission below ∼1.5 keV, iron Kα emission complex at ∼6-7 keV and a 'Compton hump' at ∼15-30 keV. We find that the relativistic reflection from a high-density accretion disc with a broken power-law emissivity profile can simultaneously explain the soft X-ray excess, highly ionized broad iron line and the Compton hump. At low frequencies ([2 - 6] x 10–5 Hz), the power-law continuum-dominated 1.5-5 keV band lags behind the reflection-dominated 0.3-1 keV band, which is explained with a combination of propagation fluctuation and Comptonization processes, while at higher frequencies ([1 - 2] x 10–4Hz), we detect a soft lag which is interpreted as a signature of X-ray reverberation from the accretion disc. The fractional root-mean-squared variability of the source decreases with energy and is well described by two variable components: a less variable relativistic disc reflection and a more variable direct coronal emission. Our combined spectral-timing analyses suggest that the observed broad-band X-ray variability of Mrk 1044 is mainly driven by variations in the location or geometry of the optically thin, hot corona.
Abstract Copyright:
© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
Journal keyword(s):
accretion, accretion discs - black hole physics - relativistic processes - galaxies: active - galaxies: Seyfert
Simbad objects:
12
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