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We investigate the use of the [O II] $\lambda3727$ emission line as a starformation rate (SFR) estimator using Sloan Digital Sky Spectra for nearly100,000 star-forming galaxies and 5,500 galaxies with narrow-line activegalactic nuclei. Consistent with previous work, we find that the [OII]/H$\alpha$ ratio in star-forming galaxies depends strongly on gas-phasemetallicity. Using metallicities derived from the [N II] $\lambda 6584$/[O II]$\lambda 3727$ method, we refine a metallicity-dependent SFR estimator based on[O II] that is calibrated within a scatter of 0.056 dex against the morecommonly used SFR indicator based on H$\alpha$ emission. The scatter increasesto only 0.12 dex if the metallicity is estimated using the stellarmass-metallicity relation. With the aim of extending the [O II]-based SFRestimator to active galaxies, we calculate radiation pressure-dominatedphotoionization models to constrain the amount of [O II] emission arising fromthe narrow-line region. We use the sample of active galaxies to demonstratethat the SFRs derived from [O II], after accounting for nonstellarcontamination, are consistent with independent SFR diagnostics estimated fromthe stellar continuum of the host galaxies.

Recalibration of [O II] $\lambda 3727$ as a Star Formation Rate Estimator for Active and Inactive Galaxies