Research Page
I measure how galaxies build up their stellar mass and how that stellar mass is distributed through a galaxy cluster. Dense spectroscopic surveys of nearby clusters supply the member catalogs, and SED fitting converts galaxy light into stellar masses and star-formation rates. From there I recover the three-dimensional structure of a cluster from what we observe in projection, extend the measurements from the optical into the infrared and the radio, and compare the results with cosmological simulations such as IllustrisTNG.
Selected Publications
A redshift survey of the nearby galaxy cluster Abell 2199: No upturn of the faint-end slope of galaxy luminosity function
Weak-Lensing Analysis of the Galaxy Cluster Abell 85: Constraints on the Merger Scenarios of Its Southern Subcluster
Projects
Each card links to a project page with more detail.
PEEL
Projection-to-Enclosed Estimator by Layers: an analytical deprojection model that recovers 3D stellar mass profiles and stellar mass fractions of galaxy clusters from projected data. Paper in preparation.
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HI Mapping on A2029
Predicting the cold-gas (HI) content of Abell 2029 members from optical/UV data, in support of a MeerKAT HI survey proposal.
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SPHEREx
Extensive multi-band SED fitting analysis using SPHEREx IR data.
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