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We compile a sample of 89 Seyfert galaxies with both [OIV] 25.89 um lineluminosities observed by Spitzer IRS and X-ray spectra observed by XMM EPIC.Using [OIV] emission as proxy of AGN intrinsic luminosity, we find thatalthough type 2 AGNs have higher line equivalent width, the narrow Fe Kalphaline in Compton-Thin and Compton-Thick Seyfert 2 galaxies are 2.9 +0.8 -0.6 and5.6 +1.9 -1.4 times weaker in terms of luminosity than Seyfert 1 galaxiesrespectively. This indicates different correction factors need to be appliedfor various types of AGNs before the narrow Fe Kalpha line luminosity couldserve as intrinsic AGN luminosity indicator. We also find Seyfert 1 galaxies inour sample have on average marginally larger line width and higher linecentroid energy, suggesting contamination from highly ionized Fe line orbroader line emission from much smaller radius, but this effect is too weak toexplain the large difference in narrow Fe Kalpha line luminosity between type 1and type 2 AGNs. This is the first observational evidence showing the narrow FeKalpha line emission in AGNs is anisotropic. The observed difference isconsistent with theoretical calculations assuming a smoothly distributedobscuring torus, and could provide independent constraints on the clumpiness ofthe torus.

The Difference in Narrow Fe K\alpha Line Emission Between Seyfert 1 and Seyfert 2 Galaxies