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We present the ASCA and Suzaku studies of the TeV source HESS J1837--069,which has not been identified in other wave-lengths. We confirm the presence oftwo X-ray sources in the Suzaku XIS image, AX J1838.0--0655 and AXJ1837.3--0652, near both ends of the elongated TeV emission region. The XISspectra of the two sources are reproduced by an absorbed power-law model, whoseparameters are all consistent with those determined by the ASCA data. Recently,70.5 ms X-ray pulsation has been detected with RXTE in the sky region includingHESS J1837--069 (2008, ApJ, 681, 515). Using the ASCA GIS data which has bothtiming and imaging capabilities, we identified the pulsation source as AXJ1838.0--0655. The pulse periods determined by ASCA and Suzaku, and thatreported with RXTE indicate steady spin-down at $\dot{P} = 4.917(4) \times10^{-14}$ s s$^{-1}$. These results suggest that AX J1838.0--0655 is anintrinsically stable source, and presumably a pulsar wind nebula (PWN). Wediscuss the possibility that AX J1838.0--0655 is associated with HESSJ1837--069 and the VHE gamma-ray emission is originated from the PWN.

X-ray studies of HESS J1837--069 with Suzaku and ASCA: a VHE gamma-ray source originated from the pulsar wind nebula