Fig. 5
Comparisons of our PAH- and TIR-derived star formation rates and the FUV+22μm star formation rates of Davis et al. (2014), the latter for CO-detected galaxies only. Solid red lines show the best-fit linear relations with nul intercepts, while the labels list the best-fit slopes, fixed intercepts, and intrinsic scatters around the best-fit relations.
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