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We present the first direct comparison between Balmer line and panchromaticSED-based SFRs for z~2 galaxies. For this comparison we used 17 star-forminggalaxies selected from the MOSFIRE Deep Evolution Field (MOSDEF) survey, with$3\sigma$ detections for H$\alpha$ and at least two IR bands (Spitzer/MIPS24$\mu$m and Herschel/PACS 100 and 160$\mu$m, and in some cases Herschel/SPIRE250, 350, and 500$\mu$m). The galaxies have total IR (8-1000$\mu$m)luminosities of $\sim10^{11.4}-10^{12.4}\,\textrm{L}_\odot$ and star-formationrates (SFRs) of $\sim30-250\,\textrm{M}_\odot\,\mathrm{yr^{-1}}$. We fit theUV-to-far-IR SEDs with flexible stellar population synthesis (FSPS) models -which include both stellar and dust emission - and compare the inferred SFRswith the SFR(H$\alpha$,H$\beta$) values corrected for dust attenuation usingBalmer decrements. The two SFRs agree with a scatter of 0.17 dex. Our resultsimply that the Balmer decrement accurately predicts the obscuration of thenebular lines and can be used to robustly calculate SFRs for star-forminggalaxies at z~2 with SFRs up to $\sim200\,\textrm{M}_\odot\,\mathrm{yr^{-1}}$.We also use our data to assess SFR indicators based on modeling theUV-to-mid-IR SEDs or by adding SFR(UV) and SFR(IR), for which the latter isbased on the mid-IR only or on the full IR SED. All these SFRs show a pooreragreement with SFR(H$\alpha$,H$\beta$) and in some cases large systematicbiases are observed. Finally, we show that the SFR and dust attenuation derivedfrom the UV-to-near-IR SED alone are unbiased when assuming a delayedexponentially declining star-formation history.

The MOSDEF Survey: The strong agreement between H-alpha and UV-to-FIR star formation rates for z~2 star-forming galaxies