The following document lists the file abstract/DLEVINE_BUBBLE.abs
from catalogue VI/111.
A plain copy of the file
(without headers/trailers) may be downloaded.
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).