X-ray polarization fluctuations induced by cloud eclipses in active galactic nuclei

TL;DR

This study models X-ray polarization fluctuations caused by cloud eclipses in active galactic nuclei to differentiate between intrinsic variability and obscuration effects, providing a new method for understanding AGN behavior.

Contribution

It introduces detailed Monte Carlo simulations of polarization changes during cloud eclipses in AGN, highlighting their potential to reveal the geometry and emission structure of the source.

Findings

Large polarization angle variations (~50°) occur during eclipses with low residual polarization.

Eclipses significantly alter polarization spectra, especially the polarization angle psi.

Distinctive polarization profiles indicate non-uniform emission regions and can test relativistic disk models.

Abstract

Context: A fraction of active galactic nuclei (AGN) show dramatic X-ray spectral changes on the day-to-week time scales associated with variation in the line of sight of the cold absorber. Aims: We intend to model the polarization fluctuations arising from an obscuration event, thereby offering a method of determining whether flux variations are due to occultation or extreme intrinsic emission variability. Methods: Undertaking 1 - 100 keV polarimetric simulations with the Monte Carlo code STOKES, we simulated the journey of a variety of cold gas clouds in front of an extended primary source. We varied the hydrogen column density nH and size of the absorber, as well as the initial polarization state of the emitting source, to cover a wide range of scenarios. Results: For unpolarized primary fluxes, large (about 50deg) variations of the polarization position angle psi are expected before and after an occultation event, which is associated with very low residual polarization degrees (P lower than 1 per cent). In the case of an emitting disk with intrinsic, position-independent polarization, and for a given range of parameters, X-ray eclipses significantly alter the observed polarization spectra, with most of the variations seen in psi. Finally, non-uniformly polarized emitting regions produce very distinctive polarization variations due to the successive covering and uncovering of different portions of the disk. Plotted against time, variations in P and psi form detectable P~Cygni type profiles that are distinctive signatures of non-axisymmetric emission. Conclusions: Polarization measurements are thus particularly adapted to distinguish between intrinsic intensity fluctuations and external eclipsing events, constrain the geometry of the covering medium, and test the hypothesis of non-uniformly emitting disks predicted by general relativity.