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ABSTRACT  We explore the use of simple star formation rate (SFR) indicators (such as may be used in high‐redshift galaxy surveys) in the local Universe using [O  ii ], H and  u ‐band luminosities from the deeper 275 deg 2  Stripe 82 subsample of the Sloan Digital Sky Survey (SDSS) coupled with UV data from the  Galaxy Evolution EXplorer  ( GALEX ) satellite. We examine the consistency of such methods using the star formation rate density as a function of stellar mass in this local volume, and quantify the accuracy of corrections for dust and metallicity on the various indicators. Rest‐frame  u ‐band promises to be a particularly good SFR estimator for high‐redshift studies since it does not require a particularly large or sensitive extinction correction, yet yields results broadly consistent with more observationally expensive methods. We suggest that the [O  ii ]‐derived SFR, commonly used at higher redshifts , can be used to reliably estimate SFRs for ensembles of galaxies, but for high‐mass galaxies , a larger correction than is typically used is required to compensate for the effects of metallicity dependence and dust extinction. We provide a new empirical mass‐dependent correction for the [O  ii ]‐SFR.

The local star formation rate density: assessing calibrations using [O ii ], H and UV luminosities