dwarf galaxies more significantly [e.g., @cook14b; @mcquinn10a; @weisz11].

Galaxy stellar masses are most commonly determined by converting observed luminosities to masses [e.g., @bell01; @McGaughSchombert14]. Often a color (e.g., B$-$V), is used to determine the mass-to-light ratio, but these estimates become less reliable for galaxies which deviate from mean scaling relations (e.g., if they are currently experiencing a starburst). In order to more uniformly determine stellar masses across our sample of BCDs and LVL galaxies, a full multi-wavelength SED-fit is necessary.

Our SED fits can be also used to make crude estimates of the SFR and star formation histories (SFHs) for BCDs and LVL galaxies, which describe the amount of star formation they experienced throughout their lifetimes. Different observational indicators are sensitive to star formation of different ages, and the SED fits incorporate all of the multi-wavelength information into a single best fitting SFH. While the broadband photometry can never produce as accurate and well-constrained a SFH as resolved stellar photometry [e.g., @tolstoy09; @mcquinn10a; @mcquinn15a], it can still be useful in comparing BCDs with typical LVL galaxies. In particular, the stellar masses and SFRs from the SED fits allow us to quantify how extreme the BCDs are compared with typical LVL 