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Polycyclic aromatic hydrocarbon (PAH) emission has long been proposed to be apotential star formation rate indicator, as it arises from thephotodissociation region bordering the Str\"omgren sphere of young, massivestars. We apply a recently developed technique of mid-infrared spectraldecomposition to obtain a uniform set of PAH measurements from Spitzerlow-resolution spectra of a large sample of star-forming galaxies spanning awide range in stellar mass ($M_\star \approx 10^6-10^{11.4}\,M_{\odot}$) andstar formation rate ($\sim 0.1- 2000\,M_{\odot}\rm\,yr^{-1}$). High-resolutionspectra are also analyzed to measure [Ne II] 12.8 $\mu$m and [Ne III] 15.6$\mu$m, which effectively trace the Lyman continuum. We present a new relationbetween PAH luminosity and star formation rate based on the [Ne II] and [NeIII] lines. Calibrations are given for the integrated $5-15$ $\mu$m PAHemission, the individual features at 6.2, 7.7, 8.6, and 11.3 $\mu$m, as well asseveral mid-infrared bandpasses sensitive to PAH. We confirm that PAH emissionis suppressed in low-mass, dwarf galaxies, and we discuss the possible physicalorigin of this effect.

A New Calibration of Star Formation Rate in Galaxies Based on Polycyclic Aromatic Hydrocarbon Emission