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. We
combine 3D-HST emission line fluxes with far-UV through far-IR photometry in a
sample of 669 emission-line galaxies (ELGs) between 1.2 < z < 1.9 and use the
MCSED spectral energy distribution fitting code to constrain the galaxies'
physical parameters, such as their star formation rates (SFRs), stellar masses,
and dust masses. We find that the assumption of energy balance between dust
attenuation and emission is likely unreasonable in many cases. We highlight a
relationship between the mass-specific star formation rate (sSFR), stellar
mass, and dust mass, although its exact form is still unclear. Finally, a
stacking of H$\alpha$ and H$\beta$ fluxes shows that nebular attenuation
increases with stellar mass and SFR for IR-bright ELGs.
