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Fig. 4


Top panel: values of the Fe Kα EW versus the geometrical covering factor of the torus (fobs) obtained by fitting MIR spectra with the clumpy torus model. The black filled diamonds are the corrected values (obtained using the model of Ikeda et al. 2009, see Eqs. (4) and (5)), while the empty red ones are the uncorrected values multiplied by an arbitrary constant factor for comparison. The data were rebinned to have six values per bin, and the uncertainties on the Fe Kα EW were calculated using the standard error of the mean. The dotted line represents the best fit to the non-binned data obtained by applying Eq. (10), and it has a slope of . The red dashed line represents the expected EWfobs trend for the set of parameters chosen for the renormalisation, calculated using the model of Ikeda et al. (2009). The intercept of the expected trend was obtained by fitting the data with the slope fixed to the expected value (Bexp ≃ 0.4). Bottom panel: 2–10 keV luminosities versus covering factor of the torus for our sample. The dashed line represents the best fit to the data (Eq. (11).

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