Correlation and time delays of the X-ray and optical emission of the Seyfert Galaxy NGC3783

TL;DR

This study analyzes simultaneous X-ray and optical observations of NGC3783, revealing correlated variability with delays suggesting reprocessing near the broad line region, but also indicating additional long-term optical variability sources.

Contribution

It provides the first detailed power spectrum analysis of both X-ray and optical variability in NGC3783, highlighting the complexity of optical variability origins.

Findings

Optical bands lag X-ray fluctuations by 3-9 days.

X-ray variability shows a power-law spectrum with a bend at ~2.9 days.

Optical variability amplitude increases over longer time-scales, exceeding X-ray variability.

Abstract

We present simultaneous X-ray and optical B and V band light curves of the Seyfert Galaxy NGC3783 spanning 2 years. The flux in all bands is highly variable and the fluctuations are significantly correlated. As shown before by Stirpe et al. the optical bands vary simultaneously, with a delay of less than 1.5 days but both B and V bands lag the X-ray fluctuations by 3-9 days. This delay points at optical variability produced by X-ray reprocessing and the value of the lag places the reprocessor close to the broad line region. A power spectrum analysis of the light curve, however, shows that the X-ray variability has a power law shape bending to a steeper slope at a time-scale ~2.9 days while the variability amplitude in the optical bands continues to grow towards the longest time-scale covered, ~ 300 days. We show that the power spectra together with the small value of the time delay is inconsistent with a picture where all the optical variability is produced by X-ray reprocessing, though the small amplitude, rapid optical fluctuations might be produced in this way. We detect larger variability amplitudes on long time-scales in the optical bands than in the X-rays. This behaviour adds to similar results recently obtained for at least three other AGN and indicates a separate source of long term optical variability, possibly accretion rate or thermal fluctuations in the optically emitting accretion disc.