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In this investigation we quantify the metallicities of low mass galaxies byconstructing the most comprehensive census to date. We use galaxies from theSDSS and DEEP2 survey and estimate metallicities from their optical emissionlines. We also use two smaller samples from the literature which havemetallicities determined by the direct method using the temperature sensitive[OIII]4363 line. We examine the scatter in the local mass-metallicity (MZ)relation determined from ~20,000 star-forming galaxies in the SDSS and showthat it is larger at lower stellar masses, consistent with the theoreticalscatter in the MZ relation determined from hydrodynamical simulations. Wedetermine a lower limit for the scatter in metallicities of galaxies down tostellar masses of ~10^7 M_solar that is only slightly smaller than the expectedscatter inferred from the SDSS MZ relation and significantly larger than whatis previously established in the literature. The average metallicity ofstar-forming galaxies increases with stellar mass. By examining the scatter inthe SDSS MZ relation, we show that this is mostly due to the lowest metallicitygalaxies. The population of low mass, metal-rich galaxies have properties whichare consistent with previously identified galaxies that may be transitionalobjects between gas-rich dwarf irregulars and gas-poor dwarf spheroidals andellipticals.

The Metallicities of Low Stellar Mass Galaxies and the Scatter in the Mass-Metallicity Relation