Cloud–cloud collision in the Galactic center 50 km s−1 molecular cloud

Abstract

Abstract We performed a search of star-forming sites influenced by external factors, such as SNRs, H ii regions, and cloud–cloud collisions (CCCs), to understand the star-forming activity in the Galactic center region using the NRO Galactic Center Survey in SiO v = 0, J = 2–1, H13CO+J = 1–0, and CS J = 1–0 emission lines obtained with the Nobeyama 45 m telescope. We found a half-shell-like feature (HSF) with a high integrated line intensity ratio of ∫TB(SiO v = 0, J = 2–1)dv/∫TB(H13CO+J = 1–0)dv ∼ 6–8 in the 50 km s−1 molecular cloud; the HSF is a most conspicuous molecular cloud in the region and harbors an active star-forming site where several compact H ii regions can be seen. The high ratio in the HSF indicates that the cloud contains huge shocked molecular gas. The HSF can be also seen as a half-shell feature in the position–velocity diagram. A hypothesis explaining the chemical and kinetic properties of the HSF is that the feature originates from a CCC. We analyzed the CS J = 1–0 emission line data obtained with the Nobeyama Millimeter Array to reveal the relation between the HSF and the molecular cloud cores in the cloud. We made a cumulative core mass function (CMF) of the molecular cloud cores within the HSF. The CMF in the CCC region is not truncated at least up to ∼2500 M⊙, although the CMF of the non-CCC region reaches the upper limit of ∼1500 M⊙. Most massive molecular cores with Mgas > 750 M⊙ are located only around the ridge of the HSF and adjoin the compact H ii region. These may be a sign of massive star formation induced by CCCs in the Galactic center region.