  We introduce a novel model to spectroscopically constrain the mid-infrared
(MIR) extinction/attenuation curve from 3--17 um, using Polycyclic Aromatic
Hydrocarbon (PAH) emission drawn from an AKARI-Spitzer extragalactic
cross-archival dataset. Currently proposed MIR extinction curves vary
significantly in their slopes toward the near-infrared, and the variation of
the strengths and shapes of the 9.7 um and 18 um silicate absorption features
make MIR spectral modeling and interpretation challenging, particularly for
heavily obscured galaxies. By adopting the basic premise that PAH bands have
relatively consistent intrinsic ratios within dusty starbursting galaxies, we
can, for the first time, empirically determine the overall shape of the MIR
attenuation curve by measuring the differential attenuation at specific PAH
wavelengths. Our attenuation model shows PAH emission in most (U)LIRGs is
unambiguously subjected to attenuation, and we find strong evidence that PAH
bands undergo differential attenuation as obscuration increases. Compared to
pre-existing results, the MIR attenuation curve derived from the model favors
relatively gray continuum absorption from 3-8 $\mu$m and silicate features with
intermediate strength at 9.7 um but with stronger than typical 18 um opacity.
