Study of Complex Absorption and Reflection in a Unique Intermediate Polar Paloma. (arXiv:2206.08635v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Dutta_A/0/1/0/all/0/1">Anirban Dutta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rana_V/0/1/0/all/0/1">Vikram Rana</a>
We present the broadband (0.3-40.0 keV) X-ray analysis of a unique
intermediate polar Paloma using simultaneous data from XMM-Newton and NuSTAR
observatories. The X-ray power spectra show strong modulations over orbital
period compared to spin period. The orbit folded lightcurves show single broad
hump like structure with strong dips for soft to medium X-rays (0.3-10.0 keV).
The energy dependent dips at $phi sim 0.16$ and $0.5$ arise due to complex
intrinsic absorber, strong enough to have effect well around 15 keV. The
absorber could potentially be contributed from accretion curtain/ accretion
stream and absorbing material produced by stream-disc/stream-magnetosphere
interactions. We notice significant variation of the absorber with orbital
phase, with maximum absorption during orbital phase 0.1-0.22. The absorber
requires more than one partial covering absorber component, specifying the
necessity to use distribution of column densities for spectral modelling of the
source. Isobaric cooling flow component is utilized to model the emission from
the multi-temperature post-shock region, giving shock temperature of
$31.7_{-3.5}^{+3.3}$keV, which corresponds to white dwarf mass of
$0.74_{-0.05}^{+0.04};M_{odot}$. We have used both the neutral absorber and
the warm absorber models, which statistically give similarly good fit, but with
different physical implications. Among the Fe K$_{alpha}$ line complex, the
neutral line is the weakest. We probed the Compton reflection, and found
minimal statistical contribution in the spectral fitting, suggesting presence
of weak reflection in Paloma.
We present the broadband (0.3-40.0 keV) X-ray analysis of a unique
intermediate polar Paloma using simultaneous data from XMM-Newton and NuSTAR
observatories. The X-ray power spectra show strong modulations over orbital
period compared to spin period. The orbit folded lightcurves show single broad
hump like structure with strong dips for soft to medium X-rays (0.3-10.0 keV).
The energy dependent dips at $phi sim 0.16$ and $0.5$ arise due to complex
intrinsic absorber, strong enough to have effect well around 15 keV. The
absorber could potentially be contributed from accretion curtain/ accretion
stream and absorbing material produced by stream-disc/stream-magnetosphere
interactions. We notice significant variation of the absorber with orbital
phase, with maximum absorption during orbital phase 0.1-0.22. The absorber
requires more than one partial covering absorber component, specifying the
necessity to use distribution of column densities for spectral modelling of the
source. Isobaric cooling flow component is utilized to model the emission from
the multi-temperature post-shock region, giving shock temperature of
$31.7_{-3.5}^{+3.3}$keV, which corresponds to white dwarf mass of
$0.74_{-0.05}^{+0.04};M_{odot}$. We have used both the neutral absorber and
the warm absorber models, which statistically give similarly good fit, but with
different physical implications. Among the Fe K$_{alpha}$ line complex, the
neutral line is the weakest. We probed the Compton reflection, and found
minimal statistical contribution in the spectral fitting, suggesting presence
of weak reflection in Paloma.
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