The Galactic Center (GC) displays a fascinating array of phenomena.
Among the most fascinating is a complex NE of Sgr A which includes the
Radio Arc, an associated molecular cloud, and the remarkable Quintuplet
stellar cluster.  Recently these structures have been linked together
with evidence of a strong magnetic field to provide a self-consistent
explanation of the observed phenomena.  New mid-infrared images of the
GC Region with MSX at ~20um highlight another morphological feature,
present but not prominent in the 20cm and 6 cm radio images.  This
feature is a closed circular ring or bubble about 500" in diameter,
bisected by the southern portion of the non-thermal filaments of the
Radio Arc and coinciding with G0.18-0.04, the "Sickle".  The mid-IR ring
also appears slightly brightened where it is crossed by the non-thermal
filaments. There is no obvious molecular gas associated with the ring
structure, except perhaps where it passes through the Sickle.
How can such a large-scale structure maintain its integrity and its
spherical symmetry in the turbulent, sheared Galactic center region?
What is the physical state and composition of the mid-IR ring?
Could it be a strong and large-scale shock generated by powerful winds
emanating from the many WR and OB stars of the Quintuplet?
We propose full-range spectral scans with SWS. A number of dust features
as well as molecular rotational lines and atomic fine-structure lines are
available and offer potential diagnostics.   We concentrate primarily
on the dust features (e.g. SiII, FeII), but also seek to detect or set
limits on molecular line emission (notably H2 and OH).