2014A&A...567A..78L

We intend to derive statistical properties of stochastic gas motion inside the dense, low-mass star-forming molecular cores that are traced by NH₃(1,1) and (2,2) emission lines. We use the spatial two-point autocorrelation (ACF) and structure functions calculated from maps of the radial velocity fields. The observed ammonia cores are characterized by complex intrinsic motions of stochastic nature. The measured kinetic temperature ranges between 8.8K and 15.1K. From NH₃ excitation temperatures of 3.5-7.3K, we determine H₂ densities with typical values of n_H2~(1-6)x10⁴cm^–3. The ammonia abundance, X=[NH₃]/[H₂], varies from 2x10^–8 to 1.5x10^–7. We find oscillating ACFs, which eventually decay to zero with increasing lags on scales of 0.04≲l≲0.5pc. The current paradigm supposes that the star-formation process is controlled by the interplay between gravitation and turbulence with the latter preventing molecular cores from a rapid collapse due to their own gravity. Thus, oscillating ACFs may indicate a damping of the developed turbulent flows surrounding the dense but less turbulent core, a transition to dominating gravitational forces and, hence, to gravitational collapse.