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The star formation rate (SFR) is a fundamental property of galaxies and it iscrucial to understand the build-up of their stellar content, their chemicalevolution, and energetic feedback. The SFR of galaxies is typically obtained byobserving the emission by young stellar populations directly in theultraviolet, the optical nebular line emission from gas ionized by newly-formedmassive stars, the reprocessed emission by dust in the infrared range, or bycombining observations at different wavelengths and fitting the full spectralenergy distributions of galaxies. In this brief review we describe theassumptions, advantages and limitations of different SFR indicators, and wediscuss the most promising SFR indicators for high-redshift studies.

Panchromatic star formation rate indicators and their uncertainties