  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 spatial
resolution) in four regions within the central 10 pc of the Galaxy where the
supernova-like remnant Sgr A East is colliding with molecular clouds. To
investigate the kinematic, physical, and positional relationships between the
important gaseous components in the center, we compared the H_2 data cube with
previously published NH_3 data. The projected interaction-boundary of Sgr A
East 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 the
synchrotron emission shell but consistent with the dust ring which is believed
to trace the shock front of Sgr A East. Since Sgr A East is driving shocks into
its nearby molecular clouds, we can determine their positional relationships
using the shock directions as indicators. As a result, we suggest a revised
model for the three-dimensional structure of the central 10 pc. The actual
contact between Sgr A East and all of the surrounding molecular material,
including the circum-nuclear disk and the southern streamer, makes the
hypothesis of infall into the nucleus and feeding of Sgr A* very likely.
