Our parent sample is star-forming galaxies with optical drift-scan spectrophotometry from Moustakas & Kennicutt (2006, J/ApJS/164/81) and Moustakas+ (2010, J/ApJS/190/233) that also have Sloan Digital Sky Survey III optical imaging (SDSS-III; Aihara+ 2011ApJS..193...29A). All of the galaxies in the sample have imaging at ultraviolet, optical, near-infrared, and mid-infrared wavelengths, taken from GALEX, the Swift UV/Optical Monitor Telescope, the Sloan Digital Sky Survey III (SDSS-III), the Two Micron All Sky Survey (2MASS), the Spitzer Space Telescope, and/or the Wide-field Infrared Space Explorer (WISE). Radio-continuum flux densities at 1.4GHz and 150MHz were determined using multiple sets of archival data. Our principal source of 1.4GHz flux densities is the NRAO VLA Sky Survey (NVSS, Condon+, 1998, VIII/65). Our principal source of 150MHz flux densities is the TIFR GMRT Sky Survey (TGSS), which has an angular resolution of ~25". We used the first alternative data release of the TGSS (TGSS ADR1; Intema+ 2017, J/A+A/598/A78). (1 data file).@en

We present calibrations for star formation rate (SFR) indicators in the ultraviolet, mid-infrared, and radiocontinuumbands, including one of the first direct calibrations of 150 MHz as an SFR indicator. Our calibrationsutilize 66 nearby star-forming galaxies with Balmer-decrement-corrected Hα luminosities, which span five ordersof magnitude in SFR and have absolute magnitudes of -24 < Mr < -12. Most of our photometry andspectrophotometry are measured from the same region of each galaxy, and our spectrophotometry has beenvalidated with SDSS photometry, so our random and systematic errors are small relative to the intrinsic scatter seenin SFR indicator calibrations. We find that the Wide-field Infrared Space Explorer W4 (22.8 μm), Spitzer 24 μm,and 1.4 GHz bands have tight correlations with the Balmer-decrement-corrected Hα luminosity, with a scatter ofonly 0.2 dex. Our calibrations are comparable to those from the prior literature for L∗ galaxies, but for dwarfgalaxies, our calibrations can give SFRs that are far greater than those derived from most previous literature.

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