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Additional info for Encyclopedia of Astronomy and Astrophysics, Volumes 1-4
E. rBLR ≈ 1015−17 cm), and scale with luminosity approximately as rBLR ∝ L1/2 , consistent with the simplest theory. Different lines in a given AGN respond with different time delays, usually in the sense that higher-ionization lines respond faster than lower-ionization lines; this indicates that the BLR has a radially stratified ionization structure and that the maximum variability response of different lines occurs at different radii. The range of time responses is such that the outer edge of the BLR is at least 10 times larger than the inner edge.
Furthermore, the low frequencies involved make it relatively easy to correlate signals from individual radio receivers separated by large distances and thus attain higher angular resolution through interferometry. Copyright © Nature Publishing Group 2001 Brunel Road, Houndmills, Basingstoke, Hampshire, RG21 6XS, UK Registered No. 785998 and Institute of Physics Publishing 2001 Dirac House, Temple Back, Bristol, BS1 6BE, UK 5 Active Galaxies: Observations 3 N V λ1240 Fλ (10−16 ergs s−1 cm−2 Å−1) in the spatial resolution they can obtain, typically down to milliarcsecond (mas) levels.
It remains to be investigated how these models apply to much brighter and to much fainter AGN. The AGN that are the subject of this article are those in which the central optical, UV, and x-ray source is Figure 1. Variations of the continuum flux at different energies during a 10 d intensive monitoring of the AGN NGC 4151. The light curves are shifted vertically for convenience and a 10 % change is indicated by the bar. (From R A Edelson et al 1996 Astrophys. J. 470 364) viewed directly and where the variations are not amplified by relativistic effects (see ACTIVE GALAXIES: OVERVIEW; UNIFIED MODEL).