Abstract
Emission line diagnostics provide a powerful tool for extracting fundamental global properties of galaxies. In this paper, we review the common optical emission‐line diagnostics for star‐formation and discuss our recent progress in this area. We focus on our recent results using H‐alpha and [OII] as star formation rate (SFR) indicators for local and high‐z samples. In local samples, correction of the SFR(H‐alpha) for extinction using the Balmer decrement and a classical reddening curve reduces the scatter and discrepancy between SFR(H‐alpha) and reddening‐insensitive SFR estimates. Using a combination of stellar population synthesis and photoionization models, we investigate the cause of the systematic discrepancy between SFRs derived from [OII] and those derived from H‐alpha. There are two significant effects which produce strong disagreement between SFR([OII]) and SFR(H‐alpha): reddening and metallicity. Such a disagreement can appear as a function of redshift, contaminating cosmic star formation histor...
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