I am a NASA Einstein Postdoctoral Fellow at the University of Chicago who develops cutting-edge instrumentation and data analysis techniques to make sensitive measurements of cosmic history. Currently I am working on SPT-SLIM, a pathfinder mm-wave line intensity mapping experiment with the potentail for a first detection of the CO power spectrum. This has new sepctrometer technology which will allow line intensity mapping telescopes to be scaled to the sensitivity needed for cosmological surveys to probe the Hubble tension, inflation, neutrino properties, and search for new light particles.
As a graduate student at UC Berkeley I worked on the South Pole Telescope (SPT), a 10-meter microwave telescope at Amundsen-Scott South Pole Station in Antarctica. During grad school I built and commissioned SPT-3G, the most recent camera on the SPT. SPT-3G makes precision measurements of the Cosmic Microwave Background, the oldest light in the universe. For my thesis, I developed novel analysis techniques to measure the polarization of the CMB to search for the signature of gravitational waves imprinted during inflation.
Previous to grad school, I worked on a variety of projects pursuing my interest in high-energy astrophysics. These included doing site characterization and instrumentation for the Greenland Neutrino Observatory, an in-ice radio detector for astrophysical ultra-high energy neutrinos, and studying cosmic ray acceleration in supernova remnants with the Fermi LAT and VERITAS.
In Fall 2025, I will hold a joint appointment as a Fermilab Lederman Fellow and as a University of Chicago KICP Fellow.
My first project of grad school was developing a cryogenically robust, low-thermal conductance, low-inductance way to connect cryogenic readout. I developed a system using ultrasonic soldering.
This is the focal plane of the SPT-3G camera on the South Pole Telescope. All of the years that I deployed to the south pole during the summer austral season, I was part of the receiver assembly team.
Here is one SPT-3G readout electronics module. On top is an LC filter assembly which connects to the detectors and set their readout channel bias frequency. The broadside coupled NbTi stripline attached to it will connect to the SQUIDs.
Show above is the figure from On-sky performance of the SPT-3G frequency-domain multiplexed readout showcasing my analysis of crosstalk in the SPT-3G receiver. We found that our crosstalk was tolerable for our science goals, and at predicted levels from our electronics design.
Recently, I've been focusing on making low-noise maps with SPT-3G data, using noise-reduction techniques to optimize for large angular scales.
Gravitational waves from inflation imprint a distinct signature in CMB polarization. The current focus of my work is to make a precision measurement of the B-mode polarization power of the CMB using SPT-3G data. However, this is a difficult measurement to make due to the tiny size of the signal, foreground contamination, atmospheric contamination, and lensed B-modes.
I am very passionate about diverse outreach. Most recently a fellow grad student and I developed a 3 week program about noise and averaging using SPT-3G Centauras A data (seen above) which we taught multiple summers to Bay Area high school students from underrepresented backgrounds. In addition, I enjoy combining the arts and science and have worked with the Runways Lab Theater on incorporating accurate physics and astronomy in many of their performances over the last 7 years.
This is my most recent "project," my dog Frango! Outside of science, I like to take him for hikes in Berkeley and hang out at the dog park.