shapes of these panchromatic SEDs encode much of the information about the star formation history, stellar populations, and dust in the BCD sample. The SEDs of each LVL galaxy are not reproduced here, but are shown and discussed extensively in @cook14b.

Fitting SEDs {#cigale}
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We fit our SEDs with CIGALE [Code Investigating Galaxy Emission, @noll09]. CIGALE fits SEDs from UV to far infrared in order to account for dust absorption and re-emission in a self-consistent manner. It creates a grid of synthetic SEDs based on theoretical models to account for all of the relevant line and continuum emission and absorption from stars, gas, and dust. This grid of models is then compared with observed SEDs in order to determine the most likely values and uncertainties for various physical parameters. In the following sub-sections we describe the models that CIGALE uses to generate SEDs, our verifications of the appropriateness of the models, and the consistency checks we employ to understand the reliability of the fit results.

Input Models {#input_models}
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CIGALE uses theoretical models to parametrize the flux emitted and absorbed by the stars, gas, and dust in model galaxies, and produces a grid of model spectra which are then 