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The spatial range for feedback from star formation varies from molecularcloud disruption on parsec scales to supershells and disk blowout on kiloparsecscales. The relative amounts of energy and momentum given to these scales isimportant for understanding the termination of star formation in any one regionand the origin of interstellar turbulence and disk stability in galaxies as awhole. Here we measure for eleven THINGS galaxies the excess kinetic energy,velocity dispersion and surface density of HI gas associated with regions ofexcess star formation, where the excess is determined from the differencebetween the observed local value and the azimuthal average. We find smalldecreases in the excess kinetic energy and velocity dispersion in regions ofexcess star formation rate density, suggesting that most of the feedback energydoes not go into local HI motion. Most likely it disrupts molecular clouds anddissipates rapidly at high gas density. Some could also be distributed overlarger regions, filling in spaces between the peaks of star formation andcontributing to other energy sources from self-gravity and spiral arm shocks.

A Search for correlations between turbulence and star formation in THINGS galaxies