Relativistic Reflection Modeling in AGN and Related Variability from PCA: A Brief Review

TL;DR

This review discusses recent advances in modeling relativistic reflection in AGNs and how PCA reveals rapid variability in X-ray emissions, aiding automated spectral analysis.

Contribution

It highlights the effectiveness of PCA in detecting relativistic reflection and understanding rapid X-ray variability in AGNs.

Findings

Relativistic reflection shows negligible fluctuations over observations.

PCA effectively discloses relativistic reflection in AGN X-ray spectra.

Rapid intrinsic variations in accretion flows may cause observed variability.

Abstract

X-ray observations of active galactic nuclei (AGNs) reveal relativistic reflections from the innermost regions of accretion disks, which contain general-relativistic footprints caused by spinning supermassive black holes (SMBH). We anticipate the spin of a SMBH to be stable over the human timeframe, so brightness changes in the high-energy corona above the SMBH should slightly alter relativistic reflection. In this brief review, we discuss the latest developments in modeling relativistic reflection, as well as the rapid small variation in relativistic emission disclosed by the principal component analysis (PCA) of X-ray variability in AGN. PCA studies of X-ray spectra from AGNs have shown that relativistically blurred reflection has negligible fluctuations over the course of observations, which could originate from rapid (intrahour) intrinsic variations in near-horizon accretion flows and photon rings. The PCA technique is an effective way to disclose relativistic reflection from X-ray observations of AGNs, simplifying the complexity of largely variable X-ray data for automated spectral analysis with machine learning algorithms.