Abstract  Along with gravity, thermal processes, and magnetic field, turbulence is a key factor in ISM evolution and star formation. Characterizing turbulence in astrophysical settings has been challenging, largely due to the incompleteness of dynamic measurements and the coupling between motion and position on the sky. For molecular clouds, in particular, we (Qian et al. 2012, 2015) have developed a new method, namely Core-Velocity-Dispersion (CVD), which is shown to be related to the two dimensional structural function. CVD holds the promise to provide a rare, direct measurement of the turbulence energy dissipating rates in clouds, for which spectroscopic maps of large spatial dynamic range are available. We also obtained energy injection rate from star formation in Taurus (Li et al. 2015). It is surprising that even in such an exclusively low mass star-forming region, the turbulence can be sustained solely by star formation feedback.