  We present Very Large Array (VLA) radio interferometry observations of the
1720 MHz OH masers in the Galactic Center (GC). Most 1720 MHz OH masers arise
in regions where the supernova remnant Sgr A East is interacting with the
interstellar medium. The majority of the newly found 1720 MHz OH masers are
located to the northeast, independently indicating and confirming an area of
shock interaction with the +50 km/s molecular cloud (M-0.02-0.07) on the far
side of Sgr A East. The previously known bright masers in the southeast are
suggested to be the result of the interaction between two supernova remnants,
instead of between Sgr A East and the surrounding molecular clouds as generally
found elsewhere in the Galaxy. Together with masers north of the circumnuclear
disk (CND) they outline an interaction on the near side of Sgr A East. In
contrast to the interaction between the +50 km/s cloud and Sgr A East, OH
absorption data do not support a direct interaction between the CND material
and Sgr A East. We also present three new high-negative velocity masers,
supporting a previous single detection. The location and velocities of the
high-negative and high-positive velocity masers are consistent with being near
the tangent points of, and physically located in the CND. We argue that the
high velocity masers in the CND are pumped by dissipation between density
clumps in the CND instead of a shock generated by the supernova remnant. That
is, the CND masers are not coupled to the supernova remnant and are sustained
independently.
