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HI spatial power spectra (PS) were determined for a sample of 24 nearby dwarfirregular galaxies selected from the LITTLE THINGS (Local Irregulars That TraceLuminosity Extremes - The HI Nearby Galaxy Survey) sample. The two-dimensional(2D) power spectral indices asymptotically become a constant for each galaxywhen a significant part of the line profile is integrated. For narrow channelmaps, the PS become shallower as the channel width decreases, and thisshallowing trend continues to our single channel maps. This implies that eventhe highest velocity resolution of 1.8 km/s is not smaller than the thermaldispersion of the coolest, widespread HI component. The one-dimensional PS ofazimuthal profiles at different radii suggest that the shallower PS fornarrower channel width is mainly contributed by the inner disks, whichindicates that the inner disks have proportionally more cooler HI than theouter disks. Galaxies with lower luminosity (M_B > -14.5 mag) and starformation rate (SFR, log(SFR (M\odot/yr)) < -2.1) tend to have steeper PS,which implies that the HI line-of-sight depths can be comparable with theradial length scales in low mass galaxies. A lack of a correlation between theinertial-range spectral indices and SFR surface density implies that eithernon-stellar power sources are playing a fundamental role in driving theinterstellar medium (ISM) turbulent structure, or the nonlinear development ofturbulent structures has little to do with the driving sources.

HI Power Spectra and the Turbulent ISM of Dwarf Irregular Galaxies