Abstract We surveyed spatial profiles of the Fe K $\alpha $ lines in the Galactic center diffuse X-rays (GCDX), including the transient region from the GCDX to the Galactic ridge X-ray emission (GRXE), with the Suzaku satellite. We resolved Fe K $\alpha $ line complex into three lines of Fe I, Fe XXV, and Fe XXVI K $\alpha $ , and obtained their spatial intensity profiles with a resolution of $\sim\ $ 0 $^\circ\!\!\!.$ 1. We compared the Fe XXV K $\alpha $ profile with a stellar mass distribution (SMD) model made from near infrared observations. The intensity profile of Fe XXV K $\alpha $ was nicely fitted with the SMD model in the GRXE region, while that in the GCDX region showed a 3.8 $\ \pm\ $ 0.3 (0 $^\circ\!\!\!.$ 2 $<$$\vert l\vert$$<$ 1 $^\circ\!\!\!.$ 5) or 19 $\ \pm\ $ 6 ( $\vert l\vert$$<$ 0 $^\circ\!\!\!.$ 2) times excess over the best-fit SMD model in the GRXE region. Thus, Fe XXV K $\alpha $ in the GCDX is hardly explained by the same origin of the GRXE. In the case of a point-source origin, a new population with the extremely strong Fe XXV K $\alpha $ line is required. An alternative possibility is that the majority of the GCDX is truly diffuse optically thin thermal plasma.