The Chemistry and Kinematics of Two Molecular Clouds near Sagittarius A*
  We have analysed the chemical and kinematic properties of the 20 and 50 km
s$^{-1}$ molecular clouds in the Central Molecular Zone of the Milky Way
Galaxy, as well as those of the molecular ridge bridging these two clouds. Our
work has utilized 37 molecular transitions in the 0.65, 3 and 7-mm wavebands,
from the Mopra and NANTEN2 telescopes. The 0.65-mm NANTEN2 data highlights a
dense condensation of emission within the western part of the 20 km s$^{-1}$
cloud, visible in only four other transitions, which are 3-mm H$^{13}$CN
(1--0), H$^{13}$CO$^{+}$ (1--0), HNC (1--0) and N$_{2}$H$^{+}$ (1--0),
suggesting that the condensation is moderately optically thick and cold. We
find that while the relative chemical abundances between both clouds are alike
in many transitions, suggesting little variation in the chemistry between both
clouds; the 20 km s$^{-1}$, cold cloud is brighter than the 50 km s$^{-1}$
cloud in shock and high density tracers. The spatial distribution of enhanced
emission is widespread in the 20 km s$^{-1}$ cloud, as shown via line ratio
maps. The position velocity diagrams across both clouds indicate that the gas
is well mixed. We show that the molecular ridge is most likely part of the 20
km s$^{-1}$ cloud and that both of them may possibly extend to include the 50
km s$^{-1}$ cloud, as part of one larger cloud. Furthermore, we expect that the
20 km s$^{-1}$ cloud is being tidally sheared as a result of the gravitational
potential from Sgr A*.
