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Using the WKB method, we show that the peak location ($r_{\rm peak}$) of thepotential, which determines the quasinormal mode frequency of the Kerr blackhole, obeys an accurate empirical relation as a function of the specificangular momentum $a$ and the gravitational mass $M$. If the quasinormal modewith $a/M \sim 1$ is observed by gravitational wave detectors, we can confirmthe black-hole space-time around the event horizon, $r_{\rm peak}=r_++O(\sqrt{1-q})$ where $r_+$ is the event horizon radius. While if thequasinormal mode is different from that of general relativity, we are forced toseek the true theory of gravity and/or face to the existence of the nakedsingularity.

How close can we approach the event horizon of the Kerr black hole from the detection of the gravitational quasinormal modes?