MCSED: A flexible spectral energy distribution fitting code and its application to $z sim 2$ emission-line galaxies. (arXiv:2006.13245v1 [astro-ph.GA])

MCSED: A flexible spectral energy distribution fitting code and its application to $z sim 2$ emission-line galaxies. (arXiv:2006.13245v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Bowman_W/0/1/0/all/0/1">William P. Bowman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zeimann_G/0/1/0/all/0/1">Gregory R. Zeimann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagaraj_G/0/1/0/all/0/1">Gautam Nagaraj</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ciardullo_R/0/1/0/all/0/1">Robin Ciardullo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gronwall_C/0/1/0/all/0/1">Caryl Gronwall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McCarron_A/0/1/0/all/0/1">Adam P. McCarron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weiss_L/0/1/0/all/0/1">Laurel H. Weiss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Molina_M/0/1/0/all/0/1">Mallory Molina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Belles_A/0/1/0/all/0/1">Alexander Belles</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schneider_D/0/1/0/all/0/1">Donald P. Schneider</a>

We present MCSED, a new spectral energy distribution (SED)-fitting code,
which mates flexible stellar evolution calculations with the Markov Chain Monte
Carlo algorithms of the software package emcee. MCSED takes broad,
intermediate, and narrow-band photometry, emission-line fluxes, and/or
absorption line spectral indices, and returns probability distributions and
co-variance plots for all model parameters. MCSED includes a variety of dust
attenuation curves with parameters for varying the UV slopes and bump
strengths, a prescription for continuum and PAH emission from dust, models for
continuum and line emission from ionized gas, options for fixed and variable
stellar metallicity, and a selection of star formation rate (SFR) histories.
The code is well-suited for exploring parameter inter-dependencies in sets of
galaxies with known redshifts, for which there is multi-band photometry and/or
spectroscopy. We apply MCSED to a sample of $sim2000$ $1.90<z<2.35$ galaxies
in the five CANDELS fields, which were selected via their strong [O III]
$lambda5007$ emission, and explore the systematic behavior of their SEDs. We
find the galaxies become redder with stellar mass, due to both increasing
internal attenuation and a greater population of older stars. The slope of the
UV extinction curve also changes with stellar mass, and at least some galaxies
exhibit an extinction excess at 2175 Angstroms. Finally, we demonstrate that
below $Mlesssim10^9,M_{odot}$), the shape of the star-forming galaxy main
sequence is highly dependent on the galaxies’ assumed SFR history, as
calculations which assume a constant SFR produce stellar masses that are
$sim1$ dex smaller than those found using more realistic SFR histories.

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