Stellar, Gas, and Dust Emission of Star Forming Galaxies out to z∼2

While dust is a major player in galaxy evolution, its relationship with gas and stellar radiation in the early universe is still not well understood. Using the near-IR grism data from the 3D-HST Treasury program,  we constructed a vetted sample of 4,351 emission-line galaxies (ELGs) at 1.16<z<1.9. We combined the emission line fluxes with FUV through FIR photometry and ran all of the sources through the spectral energy distribution fitting code MCSED, constraining physical parameters such as star formation rates (SFRs), stellar masses, and dust content of galaxies. We find that the assumption of energy balance between dust attenuation and emission may be unreasonable in many cases. In addition, we demonstrate a strong relation between specific SFR, stellar mass, and dust mass for high-redshift ELGs. Stacking of Hα and Hβ fluxes shows complex trends between nebular extinction and other physical properties like stellar mass. The greater wavelength coverage of the Wide Field Instrument of the Nancy Grace Roman Space Telescope will enable us study large, statistically complete samples of emission-line selected galaxies, constrain their gas-phase metallicities, and better understand the connection between metallicity and dust content over a large range of cosmic time.