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Metal poor dwarf galaxies in the local universe, such as those found in theRESOLVE galaxy survey, often produce high [O III]/H\b{eta} ratios close to thestar forming demarcation lines of the diagnostic BPT diagram. Modeling theemission from these galaxies at lower metallicities generally underpredictsthis line ratio, which is typically attributed to a deficit of photons >35 eV.We show that applying a model that includes empirical abundances scaled withmetallicity strongly influences the thermal balance in HII regions andpreserves the [O III]/H\b{eta} offset even in the presence of a harderradiation field generated by interacting binaries. Additional heatingmechanisms are more successful in addressing the offset. In accordance with thehigh sSFR typical of dwarf galaxies in the sample, we demonstrate that cosmicray heating serves as one mechanism capable of aligning spectral synthesispredictions with observations. We also show that incorporating a range ofphysical conditions in our modeling can create even better agreement betweenmodel calculations and observed emission line ratios. Together these resultsemphasize that both the hardness of the incident continuum and the variety ofphysical conditions present in nebular gas clouds must be accurately accountedfor prior to drawing conclusions from emission line diagnostic diagrams.

Addressing the [O III]/H\b{eta} Offset of Dwarf Galaxies in the RESOLVE Survey