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We systematically analyzed the high-quality Suzaku data of 88 Seyfertgalaxies. We obtained a clear relation between the absorption column densityand the equivalent width of the 6.4 keV line above 10$^{23}$ cm$^{-2}$,suggesting a wide-ranging column density of $10^{23-24.5}$ cm$^{-2}$ with asimilar solid and a Fe abundance of 0.7--1.3 solar for Seyfert 2 galaxies. TheEW of the 6.4 keV line for Seyfert 1 galaxies are typically 40--120 eV,suggesting the existence of Compton-thick matter like the torus with a columndensity of $>10^{23}$ cm$^{-2}$ and a solid angle of $(0.15-0.4)*4pi$, and nodifference of neutral matter is visible between Seyfert 1 and 2 galaxies. Anabsorber with a lower column density of $10^{21-23}$ cm$^{-2}$ for Compton-thinSeyfert 2 galaxies is suggested to be not a torus but an interstellar medium.These constraints can be understood by the fact that the 6.4 keV line intensityratio against the 10--50 keV flux is almost identical within a range of 2--3 inmany Seyfert galaxies. Interestingly, objects exist with a low EW, 10--30 eV,of the 6.4 keV line, suggesting that those torus subtends only a small solidangle of $<0.2*4pi$. Ionized Fe-K$\alpha$ emission or absorption lines aredetected from several percents of AGNs. Considering the ionization state andequivalent width, emitters and absorbers of ionized Fe-K lines can be explainedby the same origin, and highly ionized matter is located at the broad lineregion. The rapid increase in EW of the ionized Fe-K emission lines at$N_{H}>10^{23}$ cm$^{-2}$ is found, like that of the cold material. It is foundthat these features seem to change for brighter objects with more than several$10^{44}$ erg/s such that the Fe-K line features become weak. We discuss thisfeature, together with the torus structure.

Fe-K line probing of material around the AGN central engine with Suzaku