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CO observations of the interacting galaxies IC 2163 and NGC 2207 are combinedwith HI, Halpha and 24 microns to study the star formation rate (SFR) surfacedensity as a function of the gas surface density. More than half of the highSFR regions are HI dominated. When compared to other galaxies, theseHI-dominated regions have excess SFRs relative to their molecular gas surfacedensities but normal SFRs relative to their total gas surface densities. TheHI-dominated regions are mostly located in the outer part of NGC 2207, wherethe HI velocity dispersion is high, 40 - 50 km/s. We suggest that thestar-forming clouds in these regions have envelopes at lower densities thannormal, making them predominantly atomic, and cores at higher densities thannormal because of the high turbulent Mach numbers. This is consistent withtheoretical predictions of a flattening in the density probability distributionfunction for compressive, high Mach number turbulence.

High star formation rates in turbulent atomic-dominated gas in the interacting galaxies IC 2163 and NGC 2207