SiO Emission from the Galactic Center Molecular Clouds

摘要

The characteristics (size and H2 densities) of the SiO emission in the GC are completely different from those observed in the Galactic disk, where the SiO emission arises from much smaller regions with larger H_2, densities. We discuss briefly the implications of the SiO emission in the molecular clouds of the GC. We conclude that the particular chemistry in these clouds is probably related to large-scale fast shocks occurring in the Galactic center region.