Notes. Col. (1): Object name; Col. (2): Dust sublimation radius computed with equation 3 for the sources with a R_Fe Kα measurement; Col. (3): Fe Kα radius estimated from υ_FWHM; Col. (4): deconvolved full width at half maximum velocity; Col. (5) Size of the Fe Kα reprocessor computed in Sect. 4.2 with 1-σ errors or 2-σ limits; Col. (6) spatial extent of Fe Kα emitting region obtained from imaging analysis, where values denote largest bin with a 3-σ detection and with errors correspond to 25% of bin width, while upper limits are calculated for 25 (4″ for Cen A and 2MASXJ23444), below which the effects of pileup severely limit any estimate for this sample (see Sect. 5); Col. (7) F_Fe Kα–F_2−10 keV slope and 1-σ errors; Col. (8) variability probability P_var for continuum light curve; Col. (9) variability probability P_var for Fe Kα line light curve; Cols. (10–12): 50% percentile of the distributions of normalized excess variance, , calculated through the Monte Carlo method described in Sect. 4.1.2, for the continuum and Fe Kα line light curves, as well as the ratio between them, for all AGN in the sample. Error bars represent the ∼1σ uncertainties due to different realizations of the observational Poisson noise in the light curves. Negative values can occur when the Poisson noise uncertainty is larger than the intrinsic variance in Eq. (5). Column (13): normalized excess variance of the simulated continuum light curve and ∼1σ uncertainties (see Sect. 4.2); Col. (14): maximum light curve timespan in years. Asymmetric upper and lower errors are calculated separately following Sect. 1.73 of Lyons (1991).