from SDSS Data Release 12 [DR12, @dr12], where available. The SEDs shown in Figure \[allsed\] demonstrate the amount and quality of the photometric observations of this sample. Most of the BCDs have UV fluxes, and many have complete Spitzer FIR coverage as well. When compared with the average SEDs of the low-mass late-type (non-BCD) LVL galaxies [e.g., Figure 5 of @cook14b, and shown in our Figure \[allsed\]], the BCDs show much flatter (bluer) SEDs at UV/optical wavelengths. This is consistent with the presence of substantial recent star formation activity. The three most massive galaxies in our sample (Mk 324, Mk 328, Mk 475, Mk 900) have noticeably redder optical SEDs, and also have smooth elliptical isophotes in their outskirts. These three galaxies are classified as BCD type “nE” by @gildepaz03, and will be referred to as “BCD/E” on subsequent plots.

Across the sample of BCDs, the UV slope shows significant variations from the steep rise of Mk 67 to the flat slope of Mk 36. The UV slope is sensitive to both the internal absorption from dust as well as the current star formation. The IR observations are necessary to disentangle the effects of dust and star formation.

The detailed 