Evolution of W(Hβ) (top), W(Hα) (center), and W(Brγ) (bottom) with age for our instantaneous burst (left) and continuous star formation (right) models, demonstrating the effects of varying the IMF. The models shown here adopt the z = 0.014 v _rot = 0 (solid lines) and v _rot = 0.4 v _crit (dashed lines) evolutionary tracks of Ekström et al. (2012) and IMFs with a 0.5  M _☉–100  M _☉ mass range exponent of α = 1.3 (red), α = 2.3 (Kroupa, green), and α = 3.3 (blue).