the BCD sample. The SEDs for the complete LVL sample are presented in @cook14b. These SEDs include *GALEX* FUV and NUV images [@lee11], ground-based optical UBVRI images [@cook14a], NIR JHK images from 2MASS [Two Micron All Sky Survey @dale09], and Spitzer IR images [@dale09]. This observational dataset is used to determine the multi-wavelength SEDs from $1500$Å$-24\mu$m for galaxies in the LVL sample. Constructing SEDs with self-consistent UV, optical, NIR, and FIR fluxes is a complex process, and care was taken to measure the galaxies within a common aperture across all wavelengths [@cook14b]. In all, fluxes are reported in 14 band-passes between *GALEX* FUV and Spitzer $24\mu$m for all of the 258 LVL galaxies. As noted by @cook14b, there are 47 upper limits on non-detections in the IR observations, 13 upper limits in the UV observations, and 1 upper limit in the optical data. In total, 3551 fluxes are used in the LVL SEDs. @cook14b present the LVL SEDs and derive physical properties from them, including their star formation rates, stellar masses, and internal extinction

![Different symbols show the L-Z relation for all of the LVL galaxies with measured gas-phase metallicities (various methods). The solid blue lines show the best forward-fit 