Characterizing the Variable X-ray and UV-Optical Flux Behavior of Blazars

TL;DR

This study analyzes the variability of blazars in X-ray and UV-optical bands using Swift data, revealing how their flux changes over time and informing observation strategies for future studies.

Contribution

It provides a detailed characterization of blazar variability in X-ray and UV-optical wavelengths, highlighting differences in amplitude and suggesting optimal observation timing.

Findings

X-ray variability is 3-8 times larger than UV-optical variability.

No significant redshift dependence in variability amplitude.

Brightening episodes last at least 2-3 months with flickering.

Abstract

The variability of blazars in the X-ray and optical regions informs both the physics of their emitting region and places demands on the observer if a program requires that the object be bright or faint. The extensive simultaneous X-ray and optical observation by Swift provides the best insight into the variable nature of these objects. This program uses \textit{Swift} data for 19 X-ray-bright blazars, generally at $z > 0.1$, to determine their variability properties. The analysis is based on structure functions and provides insight into the nature of the variability and how it depends on time, luminosity, and redshift. We also consider strategies for observing blazars at or above average brightness, given a time delay between planning an observation and obtaining the data. This is critical to observations with orbiting X-ray telescopes, current or future. The variability in the soft X-ray band is typically three to eight times larger than at UV-optical wavelengths, at fixed time differences (i.e., 30 or 100 days). There is almost no difference in the amplitude of variation (X-ray or UV-optical) as a function of redshift (time delay of 30 days) and a modest positive correlation with luminosity. In the X-ray band, blazars that become brighter than normal typically remain bright for at least 2-3 months, although with significant flickering. One can avoid observing objects that are significantly below the average X-ray flux by scheduling the observation when the $F_X > 0.9 F_{X,avg}$, which requires monitoring observations near the time of the scheduling activity.