Variability and the X-ray/UV ratio of active galactic nuclei

Context. The observed relation between the X-ray radiation from active galactic nuclei, originating in the corona, and the optical/UV radiation from the disk is usually described by the anticorrelation between the UV to X-ray slope α_ox and the UV luminosity. Many factors can affect this relation, including: i) enhanced X-ray emission associated with the jets of radio-loud AGNs, ii) X-ray absorption associated with the UV broad absorption line (BAL) outflows, iii) other X-ray absorption not associated with BALs, iv) intrinsic X-ray weakness, v) UV and X-ray variability, and non-simultaneity of UV and X-ray observations. The separation of these effects provides information about the intrinsic α_ox - L_UV relation and its dispersion, constraining models of disk-corona coupling.
Aims: We use simultaneous UV/X-ray observations to remove the influence of non-simultaneous measurements from the α_ox - L_UV relation.
Methods: We extract simultaneous data from the second XMM-Newton serendipitous source catalogue (XMMSSC) and the XMM-Newton Optical Monitor Serendipitous UV Source Survey catalogue (XMMOMSUSS), and derive the single-epoch α_ox indices. We use ensemble structure functions to analyse multi-epoch data.
Results: We confirm the anticorrelation of α_ox with L_UV, and do not find any evidence of a dependence of α_ox on z. The dispersion in our simultaneous data (σ~0.12) is not significantly smaller than in previous non-simultaneous studies, suggesting that “artificial α_ox variability” introduced by non-simultaneity is not the main cause of dispersion. “Intrinsic α_ox variability”, i.e., the true variability of the X-ray to optical ratio, is instead important, and accounts for ~30% of the total variance, or more. “Inter-source dispersion”, due to intrinsic differences in the average α_ox values from source to source, is also important. The dispersion introduced by variability is mostly caused by the long timescale variations, which are expected to be driven by the optical variations.

Table 1 is only available in electronic form at http://www.aanda.org