Characterising Magellanic Stream Turbulent HI

The injection and transport of energy in the interstellar medium (ISM) directly affects structure and motions. In both netural and ionised gas, a hierarchy of structure is present down to very small scales [1, 2]. Two-dimensional spatial power spectrum (SPS) analyses can be used to investigate the hierarchical nature of turbulent ISM gas by showing the power distributed as a function of spatial scale. Furthermore, important three-dimensional statistical properties can be inferred from the two-dimensional spatial power spectra [4]. We present some results of a statistical analysis applied to a higher resolution (∼7 arcmin) ATCA and Parkes H i data set of the Magellanic Stream, which shows a damped range of velocity fluctuations with a steep velocity index. This analysis suggests the presence of some process which acts on the Stream ISM to restrict the normal range of velocity fluctuations.