The abundance of H in planetary building blocks is of fundamental importance for constraining the evolution of the terrestrial planets. It is commonly assumed that chondrites are the principal sources of Earth's H; however, recent studies have suggested that primitive achondrites and achondrites may retain a small complement of H. There are few constraints on the H budgets of primitive achondrites, which represent the transition from unmelted to melted planetesimals, but prior work suggests that bulk parent body H contents are several orders of magnitude lower than typical chondritic values. Therefore, to provide further constraints on H retention during the transition from unmelted to melted planetesimals, we have measured the H contents of olivine, orthopyroxene, clinopyroxene, and plagioclase from a suite of acapulcoite-lodranite clan meteorites. Acapulcoitelodranite clan meteorites represent the "prototypical" primitive achondrite parent body and have bulk major element compositions more akin to the Earth than previously studied primitive achondrites (e.g., the ureilites). We find that the H2O contents of olivine (-5-12 mu g/g H2O), orthopyroxene (-3-10 mu g/g H2O), and clinopyroxene (-5-8 mu g/g H2O) are broadly similar, while plagioclase (-2.5-5 mu g/g H2O) tends to be offset to lower values. Using a simple, single -stage batch -melting model, we calculate a preferred maximum acapulcoitelodranite parent body H2O content of 38 mu g/g, which is similar to other estimates for primitive achondritic and achondritic parent bodies. Furthermore, assuming chondrite-like precursor materials, our data are consistent with efficient loss of H prior to or during the onset of melting of early -formed planetesimals. This requires that Earth's H -budget was dominated by building blocks that underwent minimal thermal processing.
