Long-term optical variability of PKS 2155-304

TL;DR

This study analyzes the long-term optical variability of the blazar PKS 2155-304 over timescales from 20 days to over 10 years, using multiple methods to characterize its red noise behavior and power spectral density.

Contribution

It introduces a new method, the Multiple Fragments Variance Function (MFVF), for analyzing variability and compares it with existing techniques, providing more accurate PSD parameter estimates.

Findings

The PSD follows a broken power-law with a slope of about 1.8.

A break in the PSD occurs at a timescale of approximately 2.7 years.

The MFVF method yields the most reliable parameter estimates.

Abstract

Aims: The optical variability of the blazar PKS 2155-304 is investigated to characterise the red noise behaviour at largely different time scales from 20 days to O(>10 yrs). Methods: The long-term optical light curve of PKS 2155-304 is assembled from archival data as well as from so-far unpublished observations mostly carried out with the ROTSE-III and the ASAS robotic telescopes. A forward folding technique is used to determine the best-fit parameters for a model of a power law with a break in the power spectral density function (PSD). The best-fit parameters are estimated using a maximum-likelihood method with simulated light curves in conjunction with the Lomb Scargle Periodogram (LSP) and the first-order Structure Function (SF). In addition, a new approach based upon the so-called Multiple Fragments Variance Function (MFVF) is introduced and compared to the other methods. Simulated light curves have been used to confirm the reliability of these methods as well as to estimate the uncertainties of the best-fit parameters. Results: The light curve is consistent with the assumed broken power-law PSD. All three methods agree within the estimated uncertainties with the MFVF providing the most accurate results. The red-noise behaviour of the PSD in frequency f follows a power law with f^-{\beta}, {\beta}=1.8 +0.1/-0.2 and a break towards f^0 at frequencies lower than f_min=(2.7 +2.2/-1.6 yrs)^-1.