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We have obtained velocity-resolved spectra of the H_2 v=1-0 S(1) (lambda =2.1218 micron) emission line at 2 arcsec angular resolution (or 0.08 pc spatialresolution) in four regions within the central 10 pc of the Galaxy where thesupernova-like remnant Sgr A East is colliding with molecular clouds. Toinvestigate the kinematic, physical, and positional relationships between theimportant gaseous components in the center, we compared the H_2 data cube withpreviously published NH_3 data. The projected interaction-boundary of Sgr AEast is determined to be an ellipse with its center offset 1.5 pc from Sgr A*and dimensions of 10.8 pc X 7.6 pc. This H_2 boundary is larger than thesynchrotron emission shell but consistent with the dust ring which is believedto trace the shock front of Sgr A East. Since Sgr A East is driving shocks intoits nearby molecular clouds, we can determine their positional relationshipsusing the shock directions as indicators. As a result, we suggest a revisedmodel for the three-dimensional structure of the central 10 pc. The actualcontact between Sgr A East and all of the surrounding molecular material,including the circum-nuclear disk and the southern streamer, makes thehypothesis of infall into the nucleus and feeding of Sgr A* very likely.

Three-Dimensional Observations of H_2 Emission around Sgr A East - I. Structure in the Central 10 Parsecs of Our Galaxy