to consider the chemical evolution of the BCDs and put them in context of galaxy scaling relations.

In the UV, we use far-ultraviolet (FUV) and near-ultraviolet (NUV) observations from the *Galaxy Evolution Explorer* . Most of our galaxies were observed through our Cycle 3 program (GI3-089), but six are from archival images. *GALEX* acquires images in FUV ($1344-1786$Å) with a $4.3''$ FWHM PSF, and in NUV ($1771-2831$Å) with a $5.3''$ FWHM PSF. The images are processed and calibrated with the standard pipeline and were downloaded from the archive. The fluxes are measured in large apertures on the calibrated images. These UV images are especially sensitive to recent star formation, and provide a critical measurement of the presence and impact of young stars in the BCDs.

Some of our optical photometry comes from @sudarsky95 and @norton97, which contain complete details of their reduction and calibration. In brief, the UBVRI optical CCD observations were carried out at the Kitt Peak National Observatory[^1] (KPNO) 0.9m telescope in November/December 1989 and April 1990. The images were calibrated with observations of Landolt standards, and total fluxes were measured. NIR JHK photometry was also obtained at KPNO with IR arrays [@salzerelston92]. Table \[bcdobs\] shows which photometric 