Banting Postdoctoral Fellow at the university of Toronto
Welcome to my page! I am a Banting postdoctoral fellow at the University of Toronto with a joint affiliation at the University of Massachusetts, Amherst. I completed my PhD at Texas A&M University, where I worked with Casey Papovich on searching for the most massive galaxies in the distant Universe. Prior to my PhD, I was a Clark Scholar at Texas Christian University and an intern at the Space Telescope Science Institute, where I worked with Kat Barger and Andrew Fox on the distances and chemical abundances of the Magellanic Stream's Leading Arm, respectively.I was born and raised in the beautiful West African country of Ghana. Beyond academia, I've been involved with organizing outreach events and programs including TEDxTCU, TAMU Physics Festival, Astronomy on Tap, Bryan, and more recently, LUMA. Additionally, I strive to give back to my community through mentoring via platforms such as GLASS, CUWiP and Project iSWEST.
My current research involves using novel methods and near-infrared instrumentation to 1) detect massive quiescent galaxies at z > 3 and 2) improve their selection efficiency in existing ground-based datasets as well as surveys with JWST/NIRCam.
CV available upon request.
The feniks survey
When did the first quiescent galaxies appear? How did the most massive galaxies in the early Universe form? These are the questions we hope to answer with the Flamingos-2 Extragalactic Near-IR K-split Survey. The survey employs novel medium band K filters to reduce contamination from low redshift interlopers and increase our photometric redshift accuracy by factors of 4 and 7, respectively. Learn more at feniks.tamu.edu.
color selection of galaxies in the jwst era
Despite its utility in separating star-forming and quiescent galaxies in large photometric datasets, the UVJ diagram is fraught with problems at z > 3. We introduce an alternative: the synthetic ugi diagram, which mitigates these limitations by 1) reducing the contamination in quiescent samples from 65% to 30% at z = 5, and 2) eliminating the need for extrapolation to determine rest-frame colors.
The magellanic system
The Magellanic Stream and its Leading Arm are the largest and most massive gaseous structures in the Galactic halo. As such, they provide useful constraints for dynamical models of the Magellanic Clouds and an opportunity to study gas inflows around the Milky Way in detail. Using H𝜶 data from WHAM and HST/COS spectra, we determined the distance and chemical abundance of the Leading Arm.
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Department of Astronomy and Astrophysics
50 St George St, Toronto ON
M5S 3H4, Canada