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We present a Chandra X-ray observation of G12.82-0.02, a shell-like radiosupernova remnant coincident with the TeV gamma-ray source HESS J1813-178. Weresolve the X-ray emission from the co-located ASCA source into a compactobject surrounded by structured diffuse emission that fills the interior of theradio shell. The morphology of the diffuse emission strongly resembles that ofa pulsar wind nebula. The spectrum of the compact source is well-characterizedby a power-law with index approx. 1.3, typical of young and energeticrotation-powered pulsars. For a distance of 4.5 kpc, consistent with the X-rayabsorption, the 2-10 keV X-ray luminosity of the putative pulsar and nebula isL(PSR) = 3.2E33 erg/s and L(PWN) = 1.4E34 erg/s, respectively. Both the fluxratio of L(PWN)/L(PSR) = 4.3 and the total luminosity of this system imply apulsar spin-down power greater then 1E37 erg/s, on a par with the top ten mostenergetic young pulsars in the Galaxy. We associate the putative pulsar withthe radio remnant and the TeV source and discuss the origin of the gamma-rayemission.Comment: 3 Pages, 3 Figures. Latex, aipproc.cls. To be published in "The  Proceedings of the First International GLAST Symposium" (Held Febuary 5-8,  2007, Stanford Univ., USA), AIP, Eds. S. Ritz, P.F. Michelson, and C. Meegan.  Updated coordinate

Discovery of a Pulsar Candidate Associated with the TeV Gamma-ray Source HESS J1813-178