and reverse-fit to this relationship, and the red line shows their average. Members of our BCD sample are shown as blue points at their measured abundances. The magenta line shows the best-fit L-Z relation from @tremonti04, which agrees well with our fit. \[MZ\]](MZ-crop.eps){width="7.2cm"}

In addition to the complete set of panchromatic SEDs, gas-phase metallicities have been measured for much of the LVL sample. @cook14b compiles metallicity measurements from @marble10, @berg12, and @moustakas10, which come from different metallicity methods calibrations [see @marble10; @mcgaugh91; @pilyuginthuan05; @kobulnickykewley04]. Of the 258 galaxies in LVL, 155 have measured metallicities (about half “direct” and half “strong-line” methods), which are shown in the luminosity-metallicity relationship (L-Z) in Figure \[MZ\]. Also shown in Figure \[MZ\] is the L-Z relation from @tremonti04 for a sample of $\sim$$53,000$ SDSS galaxies brighter than M$_\textrm{B}$=$-$$16$ mag, which agrees well with the L-Z relation from the LVL and BCD samples.

BCDs in LVL {#bcd}
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Some of the galaxies in LVL have been classified as BCDs – in particular Mk 475 is a member of both our BCD sample and of the LVL sample. For brevity, throughout this work we refer to the “BCD sample” and the “LVL sample”, but there exists a 