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We present a recalibration of the luminosity-metallicity relation forgas-rich, star-forming dwarfs to magnitudes as faint as M$_R$ ~ -13. We use theDopita et al. (2013) metallicity calibrations to calibrate the relation for allof the data in this analysis. In metallicity-luminosity space we find twosub-populations within a sample of high-confidence SDSS DR8 star-forminggalaxies; 52% are metal-rich giants and 48% are metal-medium galaxies.Metal-rich dwarfs classified as tidal dwarf galaxy (TDG) candidates in theliterature are typically of metallicity 12 + log(O/H) = 8.70 $\pm$ 0.05, whileSDSS dwarfs fainter than M$_R$ = -16 have a mean metallicity of 12 + log(O/H) =8.28 $\pm$ 0.10, regardless of their luminosity, indicating that there is anapproximate floor to the metallicity of low luminosity galaxies. Ourhydrodynamical simulations predict that TDGs should have metallicities elevatedabove the normal luminosity-metallicity relation. Metallicity can therefore bea useful diagnostic for identifying TDG candidate populations in the absence oftidal tails. At magnitudes brighter than M$_R$ ~ -16 our sample of 53star-forming galaxies in 9 HI gas-rich groups is consistent with the normalrelation defined by the SDSS sample. At fainter magnitudes there is an increasein dispersion in metallicity of our sample, suggestive of a wide range of HIcontent and environment. In our sample we identify three (16% of dwarfs) strongTDG candidates (12 + log(O/H) > 8.6), and four (21%) very metal poor dwarfs (12+ log(O/H) < 8.0), which are likely gas-rich dwarfs with recently ignited starformation.

Choirs HI Galaxy Groups: The metallicity of dwarf galaxies