2016ApJ...820L..23S

We present the first direct comparison between Balmer line and panchromatic spectral energy distribution (SED)-based star formation rates (SFRs) for z ∼ 2 galaxies. For this comparison, we used 17 star-forming galaxies selected from the MOSFIRE Deep Evolution Field (MOSDEF) survey, with 3 σ detections for Hα and at least two IR bands (Spitzer/MIPS 24 µm and Herschel/PACS 100 and 160 µm, and in some cases Herschel/SPIRE 250, 350, and 500 µm). The galaxies have total IR (8-1000 µm) luminosities of ∼ 10^11.4 - 10¹²⁴ L_☉ and SFRs of ∼ 30 - 250 M_☉/yr. We fit the UV-to-far-IR SEDs with flexible stellar population synthesis (FSPS) models–which include both stellar and dust emission–and compare the inferred SFRs with the SFR(Hα, Hβ) values corrected for dust attenuation using Balmer decrements. The two SFRs agree with a scatter of 0.17 dex. Our results imply that the Balmer decrement accurately predicts the obscuration of the nebular lines and can be used to robustly calculate SFRs for star-forming galaxies at z ∼ 2 with SFRs up to ∼200 M_☉/yr. We also use our data to assess SFR indicators based on modeling the UV-to-mid-IR SEDs or by adding SFR(UV) and SFR(IR), for which the latter is based on the mid-IR only or on the full IR SED. All these SFRs show a poorer agreement with SFR(Hα, Hβ) and in some cases large systematic biases are observed. Finally, we show that the SFR and dust attenuation derived from the UV-to-near-IR SED alone are unbiased when assuming a delayed exponentially declining star formation history.