  We developed methods for mapping spatial variations of the spatial power
spectrum (SPS) and structure function (SF) slopes, with a goal of connecting
neutral hydrogen (HI) statistical properties with the turbulent drivers. The
new methods were applied on the HI observations of the Small and Large
Magellanic Clouds (SMC and LMC). In the case of the SMC, we find highly uniform
turbulent properties of HI, with no evidence for local enhancements of
turbulence due to stellar feedback. Such properties could be caused by a
significant turbulent driving on large-scales. Alternatively, a significant
line-of-sight depth of the SMC could be masking out localized regions with a
steeper SPS slope caused by stellar feedback. In contrast to the SMC, the LMC
HI shows a large diversity in terms of its turbulent properties. Across most of
the LMC, the small-scale SPS slope is steeper than the large-scale slope due to
the presence of the HI disk. On small spatial scales, we find several areas of
localized steepening of the SPS slope around major HII regions, with the 30
Doradus region being the most prominent. This is in agreement with predictions
from numerical simulations which suggest steepening of the SPS slope due to
stellar feedback eroding and destroying interstellar clouds. We also find
localized steepening of the large-scale SPS slope in the outskirts of the LMC.
This is likely caused by the flaring of the HI disk, or alternatively
ram-pressure stripping of the LMC disk due to the interactions with the
surrounding halo gas.
