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We present MCSED, a new spectral energy distribution (SED)-fitting code,which mates flexible stellar evolution calculations with the Markov Chain MonteCarlo algorithms of the software package emcee. MCSED takes broad,intermediate, and narrow-band photometry, emission-line fluxes, and/orabsorption line spectral indices, and returns probability distributions andco-variance plots for all model parameters. MCSED includes a variety of dustattenuation curves with parameters for varying the UV slopes and bumpstrengths, a prescription for continuum and PAH emission from dust, models forcontinuum and line emission from ionized gas, options for fixed and variablestellar metallicity, and a selection of star formation rate (SFR) histories.The code is well-suited for exploring parameter inter-dependencies in sets ofgalaxies with known redshifts, for which there is multi-band photometry and/orspectroscopy. We apply MCSED to a sample of $\sim2000$ $1.90<z<2.35$ galaxiesin the five CANDELS fields, which were selected via their strong [O III]$\lambda5007$ emission, and explore the systematic behavior of their SEDs. Wefind the galaxies become redder with stellar mass, due to both increasinginternal attenuation and a greater population of older stars. The slope of theUV extinction curve also changes with stellar mass, and at least some galaxiesexhibit an extinction excess at 2175 Angstroms. Finally, we demonstrate thatbelow $M\lesssim10^9\,M_{\odot}$), the shape of the star-forming galaxy mainsequence is highly dependent on the galaxies' assumed SFR history, ascalculations which assume a constant SFR produce stellar masses that are$\sim1$ dex smaller than those found using more realistic SFR histories.

MCSED: A flexible spectral energy distribution fitting code and its application to $z \sim 2$ emission-line galaxies