The MOSDEF Survey: The Dependence of H$\alpha$-to-UV SFR Ratios on SFR
  and Size at $z\sim2$
  We perform an aperture-matched analysis of dust-corrected H$\alpha$ and UV
SFRs using 303 star-forming galaxies with spectroscopic redshifts
$1.36<z_\text{spec}<2.66$ from the MOSFIRE Deep Evolution Field (MOSDEF)
survey. By combining H$\alpha$ and H$\beta$ emission line measurements with
multi-waveband resolved CANDELS/3D-HST imaging, we directly compare
dust-corrected H$\alpha$ and UV SFRs, inferred assuming a fixed attenuation
curve shape and constant SFHs, within the spectroscopic aperture. Previous
studies have found that H$\alpha$ and UV SFRs inferred with these assumptions
generally agree for typical star-forming galaxies, but become increasingly
discrepant for galaxies with higher SFRs ($\gtrsim$100 M$_\odot$ yr$^{-1}$),
with H$\alpha$-to-UV SFR ratios being larger for these galaxies. Our analysis
shows that this trend persists even after carefully accounting for the
apertures over which H$\alpha$ and UV-based SFRs (and the nebular and stellar
continuum reddening) are derived. Furthermore, our results imply that H$\alpha$
SFRs may be higher in the centers of large galaxies (i.e., where there is
coverage by the spectroscopic aperture) compared to their outskirts, which
could be indicative of inside-out galaxy growth. Overall, we suggest that the
persistent difference between nebular and stellar continuum reddening and high
H$\alpha$-to-UV SFR ratios at the centers of large galaxies may be indicative
of a patchier distribution of dust in galaxies with high SFRs.
