Spatial variations of turbulent properties of neutral hydrogen gas in
  the Small Magellanic Cloud using structure function analysis
  We investigate spatial variations of turbulent properties in the Small
Magellanic Cloud (SMC) by using neutral hydrogen HI observations. With the goal
of testing the importance of stellar feedback on HI turbulence, we define
central and outer SMC regions based on the star formation rate (SFR) surface
density, as well as the HI integrated intensity. We use the structure function
and the Velocity Channel Analysis (VCA) to calculate the power-law index
(gamma) for both underlying density and velocity fields in these regions. In
all cases, our results show essentially no difference in gamma between the
central and outer regions. This suggests that HI turbulent properties are
surprisingly homogeneous across the SMC when probed at a resolution of 30 pc.
Contrary to recent suggestions from numerical simulations, we do not find a
significant change in gamma due to stellar feedback as traced by the SFR
surface density. This could be due to the stellar feedback being widespread
over the whole of the SMC, but more likely due to a large-scale gravitational
driving of turbulence. We show that the lack of difference between central and
outer SMC regions can not be explained by the high optical depth HI.
