the extremes of dwarf galaxy evolution. Toward this end, we include the galaxies in the Local Volume Legacy (LVL) survey as a comparison sample. LVL is a volume-limited survey of 258 galaxies within $11$ Mpc, which includes flux observations from the ultraviolet to the far-infrared. The LVL sample is a particularly good comparison sample as its volume limited nature means that a majority of its galaxies have stellar masses below $10^9M_\odot$, similar to our BCD sample [@dale09]. In fact, some of the galaxies in the LVL sample are classified as BCDs, as discussed in Section \[bcd\]. In this analysis, we do not consider the environment of LVL galaxies (or BCDs), and treat each galaxy individually; further work is needed to explore the effects of the environment on star formation processes in dwarf galaxies.

Photometric observations of the BCD sample
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The multi-wavelength photometric observations of our BCD sample come from many sources. Table \[bcdobs\] shows a complete summary of the photometry for each object, and Table \[bcddata\] contains all of the observed fluxes of our BCD sample. We also use gas-phase abundances from spectroscopic observations of the BCDs from sources in the literature [@zhao10; @brinchmann08; @izotov07]. These abundances allow us 