We have obtained velocity-resolved spectra of the H _ { 2 } ~ { } 1 - 0 ~ { } S ( 1 ) ~ { } ( \lambda = 2.1218 \micron ) emission line at 2 \arcsec angular resolution ( or \sim 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 \sim 1.5 pc from Sgr A* and dimensions of 10.8 pc \times 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 .