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 EW − fobs 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).
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.