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Building on our previous spectroscopic and photometric analysis of theisolated Local Group dwarf irregular (dIrr) galaxy WLM, we present a comparisonof the metallicities of its RGB stars with respect to the well studied LocalGroup dwarf spheroidal galaxies (dSphs) and Magellanic Clouds. We calculate amean metallicity of [Fe/H]$ = -1.28 \pm 0.02$, and intrinsic spread inmetallicity of $\sigma = 0.38 \pm 0.04$ dex, similar to the mean and spreadobserved in the massive dSph Fornax and the Small Magellanic Cloud. Thus,despite its isolated environment the global metallicity still followsexpectations for WLM's mass and its global chemical evolution is similar toother nearby luminous dwarf galaxies (gas-rich or gas-poor). The data also showa radial gradient in [Fe/H] of $\rm{d[Fe/H]/dr_{c}} = -0.04 \pm 0.04$ dex$\rm{r_{c}^{-1}}$, which is flatter than that seen in the unbiased andspatially extended surveys of dSphs. Comparison of the spatial distribution of[Fe/H] in WLM, the Magellanic Clouds, and a sample of Local Group dSphs, showsan apparent dichotomy in the sense that the dIrrs have statistically flatterradial [Fe/H] gradients than the low angular momentum dSphs. The correlationbetween angular momentum and radial metallicity gradient is further supportedwhen considering the Local Group dEs. This chemodynamic relationship offers anew and useful constraint for environment driven dwarf galaxy evolution modelsin the Local Group.

The Comparative Chemical Evolution of an Isolated Dwarf Galaxy: A VLT and Keck Spectroscopic Survey of WLM