The MOSDEF Survey: Dissecting the star-formation rate vs. stellar mass relation using H$\alpha$ and H$\beta$ emission lines at z ~ 2

Abstract

We present results on the star-formation rate (SFR) versus stellar mass ($M_{\ast }$) relation (i.e., the "main sequence") among star-forming galaxies at 1.37$\le$$z$$\le$2.61 using the MOSFIRE Deep Evolution Field (MOSDEF) survey. Based on a sample of 261 galaxies with H$\alpha$ and H$\beta$ spectroscopy, we have estimated robust dust-corrected instantaneous SFRs over a large range in $M_{\ast }$ ($\sim 10^{9.5}-10^{11.5}{M}_{\odot }$). We find a correlation between log(SFR(H$\alpha$)) and log($M_{\ast }$) with a slope of 0.65$\pm$0.08 (0.58$\pm$0.10) at 1.4<z<2.6 (2.1<z<2.6). We find that different assumptions for the dust correction, such as using the color-excess of the stellar continuum to correct the nebular lines, sample selection biases against red star-forming galaxies, and not accounting for Balmer absorption can yield steeper slopes of the log(SFR)-log($M_{\ast }$) relation. Our sample is immune from these biases as it is rest-frame optically selected, H$\alpha$ and H$\beta$ are corrected for Balmer absorption, and the H$\alpha$ luminosity is dust-corrected using the nebular color-excess computed from the Balmer decrement. The scatter of the log(SFR(H$\alpha$))-log($M_{\ast }$) relation, after accounting for the measurement uncertainties, is 0.31 dex at 2.1<z<2.6, which is 0.05 dex larger than the scatter in log(SFR(UV))-log($M_{\ast }$). Based on comparisons to a simulated SFR-$M_{\ast }$ relation with some intrinsic scatter, we argue that in the absence of direct measurements of galaxy-to-galaxy variations in the attenuation/extinction curves and the IMF, one cannot use the difference in the scatter of the SFR(H$\alpha$)- and SFR(UV)-$M_{\ast }$ relations to constrain the stochasticity of star formation in high-redshift galaxies.

13 pages, 8 figures, 2 tables, ApJ accepted version

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