Probing X-ray Timing and Spectral Variability in the Blazar PKS 2155-304 Over a Decade of XMM-Newton Observations

TL;DR

This study analyzes a decade of XMM-Newton X-ray observations of the blazar PKS 2155-304, revealing its variability patterns, spectral properties, and flux states to better understand the jet-driven mechanisms behind its rapid flux changes.

Contribution

It provides a comprehensive long-term spectral and timing analysis of PKS 2155-304, highlighting flux bimodality and spectral breaks with implications for jet physics.

Findings

Moderate intra-day variability observed in most light curves.

Presence of two distinct flux states in several observations.

Spectral fits favor broken power-law models indicating spectral breaks.

Abstract

Blazars, a class of active galactic nuclei (AGN) powered by supermassive black holes, are known for their remarkable variability across multiple timescales and wavelengths. Despite significant advancements in our understanding of AGN central engines, thanks to both ground- and space-based telescopes, the details of the mechanisms driving this variability remain elusive. The primary objective of this study is to constrain the X-ray variability properties of the TeV blazar PKS 2155-304. We conducted a comprehensive X-ray spectral and timing analysis, focusing on both long-term and intra-day variability (IDV), using data from 22 epochs of {\it XMM-Newton} observations collected over 15 years (2000 to 2014). For the timing analysis, we estimated the fractional variability, variability amplitude, minimum variability timescales, flux distribution, and power spectral density. In the spectral analysis, we fitted the X-ray spectra using power-law, log-parabola, and broken power-law models to determine the best-fitting parameters. We observed moderate IDV in the majority of the light curves. Seven out of the 22 observations showed a clear bimodal flux distribution, indicating the presence of two distinct flux states. Our analysis revealed a variable power spectral slope. Most hardness ratio plots did not show significant variation with flux, except for two observations, where the hardness ratio changed considerably with flux. The fitted X-ray spectra favored the broken power law model for the majority of observations, indicating break in the spectral profiles. The findings of this work shed light on the IDV of blazars, providing insights into the non-thermal jet processes that drive the observed flux variations.