A detailed analysis on the cloud structure and dynamics in Aquila Rift
  We present maps in several molecular emission lines of a 1 square-degree
region covering the W40 and Serpens South molecular clouds belonging to the
Aquila Rift complex. The observations were made with the 45 m telescope at the
Nobeyama Radio Observatory. We found that the $^{12}$CO and $^{13}$CO emission
lines consist of several velocity components with different spatial
distributions. The component that forms the main cloud of W40 and Serpens
South, which we call the "main component", has a velocity of $V_{\rm LSR}\simeq
7$ km s$^{-1}$. There is another significant component at $V_{\rm LSR}\simeq
40$ km s$^{-1}$, which we call the "40 km s$^{-1}$ component". The latter
component is mainly distributed around two young clusters: W40 and Serpens
South. Moreover, the two components look spatially anti-correlated. Such
spatial configuration suggests that the star formation in W40 and Serpens South
was induced by the collision of the two components. We also discuss a
possibility that the 40 km s$^{-1}$ component consists of gas swept up by
superbubbles created by SNRs and stellar winds from the Scorpius-Centaurus
Association.
