XMM-Newton observations of the Lockman Hole V: time variability of the brightest AGN

TL;DR

This study analyzes long-term X-ray flux and spectral variability in the brightest AGN in the Lockman Hole, revealing that most AGN vary in flux over years, with spectral variability more common in type-2 AGN, indicating complex multi-component variability.

Contribution

First comprehensive analysis of long-term flux and spectral variability in a large sample of bright AGN, highlighting the need for multiple variable components to explain observed X-ray changes.

Findings

Approximately 50% of AGN show significant flux variability.

Over 80% of sources with good light curves vary in flux over long timescales.

Spectral variability occurs in about 40% of sources, more in type-2 AGN.

Abstract

This paper presents the results of a study of X-ray spectral and flux variability on time scales from months to years, of the 123 brightest objects (including 46 type-1 AGN and 28 type-2 AGN) detected with XMM-Newton in the Lockman Hole field. We detected flux variability with a significance >3sigma in ~50% of the objects, including 68+-11% and 48+-15% among our samples of type-1 and type-2 AGN. However we found that the fraction of sources with best quality light curves that exhibit flux variability on the time scales sampled by our data is >80%, i.e the great majority of the AGN population may actually vary in flux on long time scales. The mean relative intrinsic amplitude of flux variability was found to be ~0.15 although with a large dispersion in measured values, from ~0.1 to ~0.65. The flux variability properties of our samples of AGN do not significantly depend on the redshift or X-ray luminosity of the objects and seem to be similar for the two AGN types. Using a broad band X-ray colour we found that the fraction of sources showing spectral variability with a significance >3sigma is ~40% i.e. less common than flux variability. Spectral variability was found to be more common in type-2 AGN than in type-1 AGN with a significance >99%. This result is consistent with the fact that part of the soft emission in type-2 AGN comes from scattered radiation, and this component is expected to be much less variable than the hard component. The observed flux and spectral variability properties of our objects cannot be explained as being produced by variability of one spectral component alone, for example changes in the continuum shape associated with changes in the mass accretion rate, or variability in the amount of X-ray absorption. At least two spectral components must vary in order to explain the X-ray variability of our objects.