The M33 Metallicity Project: Resolving the Abundance Gradient Discrepancies in M33

We present a new determination of the metallicity gradient in M33, based on Keck LRIS measurements of oxygen abundances using the temperature-sensitive emission line [O iii] k4363 in 61 H ii regions. These data approximately triple the sample of direct oxygen abundances in M33. We find a central abundance of 12þ log (O/H) 1⁄4 8:36 0:04 and a slope of 0:027 0:012 dex kpc , in agreement with infrared measurements of the neon abundance gradient but much shallower than most previous oxygen gradient measurements. There is substantial intrinsic scatter of 0.11 dex in the metallicity at any given radius in M33, which imposes a fundamental limit on the accuracy of gradient measurements that rely on small samples of objects. We also show that the ionization state of neon does not follow the ionization state of oxygen as is commonly assumed, suggesting that neon abundance measurements from optical emission lines require careful treatment of the ionization corrections. Subject headingg s: galaxies: abundances — galaxies: individual (M33) — galaxies: spiral — H ii regions — ISM: abundances — ISM: evolution Online material: machine-readable table