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The MOSDEF Survey: An Improved Voronoi Binning Technique on Spatially Resolved Stellar Populations at z~2 | | Tara Fetherolf
; Naveen Reddy
; Alice Shapley
; Mariska Kriek
; Brian Siana
; Alison Coil
; Bahram Mobasher
; William Freeman
; Ryan Sanders
; Sedona Price
; Irene Shivaei
; Mojegan Azadi
; Laura de Groot
; Gene Leung
; Tom Zick
; | | Date: |
8 Sep 2020 | | Abstract: | We use a sample of 350 star-forming galaxies at $1.25<z<2.66$ from the
MOSFIRE Deep Evolution Field survey to demonstrate an improved Voronoi binning
technique that we use to study the properties of resolved stellar populations
in $zsim2$ galaxies. Stellar population and dust maps are constructed from the
high-resolution CANDELS/3D-HST multi-band imaging. Rather than constructing the
layout of resolved elements (i.e., Voronoi bins) from the S/N distribution of
the $H_{160}$-band alone, we introduce a modified Voronoi binning method that
additionally incorporates the S/N distribution of several resolved filters. The
SED-derived resolved E(B-V)$_{ ext{stars}}$, stellar population ages, SFRs,
and stellar masses that are inferred from the Voronoi bins constructed from
multiple filters are generally consistent with the properties inferred from the
integrated photometry within the uncertainties, with the exception of the
inferred E(B-V)$_{ ext{stars}}$ from our $zsim1.5$ sample due to their UV
slopes being unconstrained by the resolved photometry. The results from our
multi-filter Voronoi binning technique are compared to those derived from a
"traditional" single-filter Voronoi binning approach. We find that
single-filter binning produces inferred E(B-V)$_{ ext{stars}}$ that are
systematically redder by 0.02 mag on average, but could differ by up to 0.20
mag, and could be attributed to poorly constrained resolved photometry covering
the UV slope. Overall, we advocate that our methodology produces more reliable
SED-derived parameters due to the best-fit resolved SEDs being better
constrained at all resolved wavelengths--particularly those covering the UV
slope. | | Source: | arXiv, 2009.03926 | | Services: | Forum | Review | PDF | Favorites | |
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