A Relativistic Disc Reflection Model for 1H0419-577: Multi-Epoch Spectral Analysis with XMM-Newton and NuSTAR. (arXiv:1811.10932v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Jiang_J/0/1/0/all/0/1">Jiachen Jiang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walton_D/0/1/0/all/0/1">Dominic J. Walton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fabian_A/0/1/0/all/0/1">Andrew C. Fabian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parker_M/0/1/0/all/0/1">Michael L. Parker</a>

We present a detailed analysis of the spectral properties of the Seyfert 1
galaxy 1H0419-577, based on the archival XMM-Newton, NuSTAR and simultaneous
Swift observations taken between 2002-2015. All the observations show a broad
emission line feature at the iron band. We demonstrate that the broad band
spectral variability at different levels can be explained by the combination of
light-bending effects in the vicinity of the central black hole plus a thin
warm absorber. We obtain a black hole spin of a > 0.98 by fitting the
multi-epoch spectra with the relativistic disc reflection model. 1H0419-577 is
accreting at 40% of its Eddington limit and its X-ray band shows the hardest
powerlaw continuum in the highest flux state, which was previously more
commonly seen in AGNs with a low accretion rate (e.g. $L_{rm X} /L_{rm Edd} < 10^{-2}$). The NuSTAR observation shows a cool coronal temperature of $kT=30^{+22}_{-7}$keV in the high flux state.

We present a detailed analysis of the spectral properties of the Seyfert 1
galaxy 1H0419-577, based on the archival XMM-Newton, NuSTAR and simultaneous
Swift observations taken between 2002-2015. All the observations show a broad
emission line feature at the iron band. We demonstrate that the broad band
spectral variability at different levels can be explained by the combination of
light-bending effects in the vicinity of the central black hole plus a thin
warm absorber. We obtain a black hole spin of a > 0.98 by fitting the
multi-epoch spectra with the relativistic disc reflection model. 1H0419-577 is
accreting at 40% of its Eddington limit and its X-ray band shows the hardest
powerlaw continuum in the highest flux state, which was previously more
commonly seen in AGNs with a low accretion rate (e.g. $L_{rm X} /L_{rm Edd} <
10^{-2}$). The NuSTAR observation shows a cool coronal temperature of
$kT=30^{+22}_{-7}$keV in the high flux state.

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