Wide-field 12CO (J=2-1) and 13CO (J=2-1) Observations toward the Aquila Rift and Serpens Molecular Cloud Complexes. I. Molecular Clouds and Their Physical Properties

We present the results of wide-field (CO)-C-12 (J = 2-1) and (CO)-C-13 (J = 2-1) observations toward the Aquila Rift and Serpens molecular cloud complexes (25. < l < 33. and1. < b < 6.) at an angular resolution of 3 4 (approximate to 0.25 pc) and at a velocity resolution of 0.079 km s(-1) with velocity coverage of 5 km s(-1) V 35 km s(LSR) -1. We found that the (CO)-C-13 emission better traces the structures seen in the extinction map, and derived the X13CO-factor of this region. Applying SCIMES to the (CO)-C-13 data cube, we identified 61 clouds and derived their mass, radii, and line widths. The line width-radius relation of the identified clouds basically follows those of nearby molecular clouds. The majority of the identified clouds are close to virial equilibrium, although the dispersion is large. By inspecting the (CO)-C-12 channel maps by eye, we found several arcs that are spatially extended to 0 degrees. 2-3 degrees in length. In the longitude-velocity diagrams of (CO)-C-12, we also found two spatially extended components that appear to converge toward Serpens South and the W40 region. The existence of two components with different velocities and arcs suggests that large-scale expanding bubbles and/or flows play a role in the formation and evolution of the Serpens South and W40 cloud.