and related galaxies. Some are canonical BCDs (e.g., I Zw 18), while some have smooth outer isophotes (similar to a dE) with a strong central starburst (e.g., Mk 900). Some have offset starbursts (e.g., Mk 36, Mk 750), dual starburst regions (UM 461, Mk 600), cometary shapes (Mk 5), or large numbers of active star formation sites (e.g., UM 439, UM 462, UM 323). Our sample is faint ($\langle$M$_\textrm{B} \rangle$=$-16$ mag), blue ($0$$<$B$-$V$<$$0.5$), metal deficient ($\langle 12+$log$($O$/$H$) \rangle
$$\sim$$8$), and less than 50 Mpc away [see Table 1 in @janowiecki14 for more details]. Our BCD sample is not comprehensive, but instead is representative and its members span the range of parameter space that BCDs typically occupy. Samples of BCDs have been defined in various ways, beginning from their identification as extragalactic HII regions [@sargentsearle70], continuing through the definitions of @tm81 and @gildepaz03. All of these samples commonly include dwarf galaxies which are compact (or merely small) and intensely forming stars. However, conclusions about the evolution of BCDs can depend strongly on sample selection [see also Section 5 of @janowiecki14]. Rather than creating or adopting a definition of BCDs, we instead select a sample of BCDs and BCD-like galaxies to study 