We measure the power spectrum of HI intensity fluctuations in the extremely faint ( M _ { B } ~ { } \sim~ { } -10.9 ) dwarf galaxy DDO 210 using a visibility based estimator that is well suited in very low signal to noise ratio regimes .
DDO 210 ’ s HI power spectrum is well fit by a power law { P } _ { HI } ( U ) = AU ^ { \alpha } with \alpha = -2.75 \pm 0.45 over the length-scales 80 { pc } to 500 { pc } .
We also find that the power spectrum does not change with an increase in the velocity channel width , indicating that the measured fluctuations correspond mainly to density fluctuations .
However , Kolmogorov turbulence ( with a velocity structure function spectral slope of 2/3 ) can not be ruled out from the present observations .
The value of the slope \alpha is similar to that obtained in the Milkyway .
In contrast to the Milkyway , DDO 210 has three orders of magnitude less HI , no spiral arms , and also no measurable ongoing star formation .
The fact that the power spectrum slope is nonetheless similar in these two galaxies ( and also similar to the values measured for the LMC and SMC ) suggests that there is some universal , star formation independent , phenomenon responsible for producing fine scale structure in the gas .