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tokens: that will be found by next-generation space-based grism surveys, such as those planned for Euclid and WFIRST (Maciaszek et al. 2014 ; Gong et al. 2016 ). Section 2 briefly describes our galaxy sample and the archival photometry and spectrophotometry available for analysis. Section 3 lists the parameters used for modeling the galaxies’ UV through near-IR SEDs and introduces our new SED fitting code, MCSED . Section 4 explores the basic properties of the Bowman et al. ( 2019 ) sample, the systematics of the data set, and the effect that various assumptions have on the results. Section 5 extends our analysis to the mid- and far-IR and tests the ability of MCSED to explore the balance between the sight-line attenuation of the UV stellar continua by dust and its isotropic reradiation at longer wavelengths. Finally, in Section 6 , our results are placed in the context of other work at these redshifts and within the framework of simulations. Throughout this paper, we assume a ΛCDM cosmology, with Ω Λ = 0.7, Ω M = 0.3, and H 0 = 70 km s −1 Mpc −1 (Bennett et al. 2013 ). 2. The Sample At present, the largest samples of z ≳ 2 galaxies have been constructed from broadband photometry and color selection via the use of photometric redshifts (e.g., Reddy et al. 2012 ; Bouwens et al. 2015 ; Ono et al. 2018 ). However, in the near future, space missions such as Euclid/NISP (Maciaszek et al. 2014 ) and WFIRST (Gong et al. 2016 ) will detect millions of emission-line galaxies via near-IR slitless grism spectroscopy. Since the selection criteria for these galaxies will differ substantially from those identified using broadband photometric techniques, we can expect the distribution of the galaxies’ physical properties to differ as well. To prepare for this era, we can study the objects found by the pathfinding 3D-HST survey, a 625 arcmin 2 set of two-orbit observations taken with the Wide Field Camera 3 (WFC3) and the G141 grism on the HST (GO programs 11600, 12177, and 12328; Momcheva et al. 2016 ; Weiner AGHAST Team 2014 ). This data set consists of R ∼ 130 near-IR (1.08 μ m λ 1.68 μ m) slitless spectroscopy within the deep CANDELS fields of AEGIS, COSMOS, UDS, GOODS-N, and GOODS-S (Giavalisco et al. 2004 ; Davis et al. 2007 ; Lawrence et al. 2007 ; Scoville et al. 2007 ). Tens of thousands of objects are detectable on these frames, but of special interest are galaxies in the redshift range 1.90 z 2.35. In this window, the emission lines of [O ii ] λ 3727, [Ne iii ] λ 3869, H β , and the distinctively shaped [O iii ] blended doublet λλ 4959, 5007 are simultaneously present in the bandpass. This set of observable emission lines, which includes two different ionization states of oxygen, not only enables the determination of unambiguous redshifts but also allows for the direct detection of galaxies over an extremely wide range of metallicities and ionization parameters. Bowman et al. ( 2019 ) recently created a sample of 1952 such oELGs by vetting the list of 1.90