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\documentstyle[12pt,aasms4]{article}
\def\solar{$_{\mathord\odot}$}
\def\kms{km sec$^{-1}$}
\def\11{NH$_3$(1,1)}
\def\22{NH$_3$(2,2)}
\def\33{NH$_3$(3,3)}

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\title{\center The Dynamics of Molecular Material Within 15 Parsecs of the
Galactic Center}
\author{Alison L. Coil}
\affil{Astronomy Department\\
University of California at Berkeley \\
Berkeley, CA 94720 \\
e-mail: acoil@astro.berkeley.edu \\}
\author{Paul T.P. Ho}
\affil{Harvard-Smithsonian Center for Astrophysics \\
60 Garden St. MS-78\\
Cambridge, MA 02138\\
e-mail: pho@cfa.harvard.edu \\}

\begin{abstract}

\ \ \ \ \ We report the results of a 5-field mosaic of the central 15pc
of the Galaxy in the (1,1) and (2,2) lines of NH$_3$.  Two narrow
filaments or streamers are seen running parallel to the Galactic
plane.  The southern streamer appears to carry
gas directly toward the nuclear region from the 20 \kms cloud.  
The eastern streamer, which
we will denote the molecular ridge, appears to be the denser part of
the 50 \kms cloud which lies immediately east of the Sgr A East
complex and extends in the south towards the 20 \kms cloud.  This
ridge of gas carries the kinematical signatures of interactions
with Sgr A East as well as a SNR which lies south of the Galactic
center.  The bulk motion of the gas, the enhanced line widths, and the
heating of the molecular material all suggest an active evolutionary
phase for the gas immediately adjacent to the nucleus.

\end{abstract}