Left panel: column density vs. Fe Kα EW for the obscured sources with pn+MOS+Chandra joint fit (black) and pn only fit (gray). The red (green) shaded areas show the expected Fe Kα EW as a function of N_H as computed in the torus model of Ikeda et al. 2009 (Murphy & Yaqoob 2009). Cyan points represent the observed N_H and EW for a sample of local Seyfert galaxies observed with Suzaku (Fukazawa et al. 2011). Right panel: scattered fraction vs. column density for the obscured sources with pn+MOS+Chandra joint fit (black) and pn only fit (gray).