  We present results of a multi-band Spectral Energy Distribution (SED) and
nebular emission line analysis of a sample of 1147 spectroscopically identified
dusty star-forming galaxies at 0.49 < z < 2.24 from Herschel/SPIRE and HST/WFC3
grism observations in the five CANDELS fields: AEGIS, GOODS-N, GOODS-S, COSMOS,
and UDS. We use the spectroscopic redshifts measured from nebular lines to
construct the SEDs of galaxies from the optical to the infrared using HST and
Herschel photometry. We further utilize the 3D-HST grism Ha line flux
measurements to measure the nebular star-formation rates after correcting for
attenuation. We compare this with direct observations of the SFR measurements
in the far-infrared from Herschel. Observation of the infrared excess (IRX) in
this sample as a function of the UV spectral slope reveals that these DSFGs
deviate toward bluer colors, thus sitting well above the expected relation for
normal star-forming galaxies. The high-z dusty galaxies have a stellar mass
distribution that is skewed towards larger masses, with $M_{med} = 2.6 \times
10^{10} M_{\odot}$. However this population has star-formation rates consistent
with the most massive tail of the main sequence, showing that these are both
the most massive and the most star-forming galaxies during the peak epoch of
formation.
