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In order to test a recent hypothesis that the dispersion in theSchmidt-Kennicutt law arises from variations in the evolutionary stage of starforming molecular clouds, we compared molecular gas and recent star formationin an early-phase merger galaxy pair, Taffy I (UGC\ 12915/UGC\ 12914, VV\ 254)which went through a direct collision 20 Myr ago and whose star forming regionsare expected to have similar ages. Narrow-band Pa-alpha image is obtained usingthe ANIR near-infrared camera on the mini-TAO 1m telescope. The image enablesus to derive accurate star formation rates within the galaxy directly. Thetotal star formation rate, 22.2 M_sun/yr, was found to be much higher thanprevious estimates. Ages of individual star forming blobs estimated fromequivalent widths indicate that most star forming regions are ~7 Myr old,except for a giant HII region at the bridge which is much younger. Comparisonbetween star formation rates and molecular gas masses for the regions with thesame age exhibits a surprisingly tight correlation, a slope of unity, and starformation efficiencies comparable to those of starburst galaxies. These resultssuggest that Taffy I has just evolved into a starburst system after thecollision, and the star forming sites are at a similar stage in their evolutionfrom natal molecular clouds except for the bridge region. The tightSchmidt-Kennicutt law supports the scenario that dispersion in the starformation law is in large part due to differences in evolutionary stage of starforming regions.

The Schmidt-Kennicutt Law of Matched-Age Star Forming Regions; Pa-alpha Observations of the Early-Phase Interacting Galaxy Taffy I