Experimental astroparticle physicist developing radio-based detection of ultra-high-energy cosmic rays. Directions: (1) HAWC — high-altitude water Cherenkov detector for gamma-ray and cosmic ray sensing; (2) IceTop surface array at IceCube for cosmic ray composition at the knee; (3) radio detection of cosmic-ray-induced air showers (Askaryan emission) as a technique for large-scale UHE cosmic ray sensing. Enrico Fermi Institute member.
Wang's BOBA group directly images young, self-luminous exoplanets by suppressing host-star glare with coronagraphy, extreme adaptive optics, and long-baseline optical interferometry (e.g. Keck/KPIC, VLTI), combined with physics-based computational signal-processing and machine-learning algorithms to extract faint planetary signals. He led early JWST direct-imaging detections of exoplanets and studies their orbits, formation, and atmospheres via high- and low-resolution spectroscopy. This is offered as an astronomy pivot on the filter: the enabling technology is increasingly complex opto-mechanical and computational instrumentation pushing spatial and spectral resolution, rather than a quantum sensor per se.
Warren uses large near-infrared sky surveys (e.g. UKIDSS/VISTA) to discover and characterise high-redshift quasars, cool brown dwarfs and other rare populations, and works on wide-field survey design and statistics.
Webster works on the Epoch of Reionisation with the Murchison Widefield Array, where the science goal — detecting the redshifted 21-cm signal from the first stars — is a five-orders-of-magnitude foreground-subtraction and instrumental-calibration problem rather than an astrophysics problem. Her group's contributions are in foreground modelling, ionospheric and beam calibration, and the statistical detection of a signal buried far below the systematics floor; she also works on quasar accretion physics. Positioned against the established body of NV-ensemble quantum sensing work — DEER, nanoscale NMR and T1 relaxometry protocols operating at pT/sqrt(Hz) field sensitivity — the methodological parallel is exact: like a pT/sqrt(Hz) NV ensemble measurement, a 21-cm detection lives or dies on the control of correlated systematics rather than on raw sensitivity. Borderline inclusion under the astronomy criterion, kept because the array and its calibration are the central object of study.
Astrochemist studying the evolution of prebiotic molecules during star and planet formation, combining laboratory molecular spectroscopy and instrument development with radio and far-IR astronomical observations and astrochemical modeling.
Studies the evolution of galaxies and galaxy groups (gas content, Magellanic-type spirals, radio AGN, intergalactic medium) primarily through radio observations.
Studies molecular gas and the interstellar medium in galaxies using radio and millimeter interferometry (e.g., ALMA, CARMA).
Wurm's group builds and exploits large liquid-scintillator neutrino detectors, principally JUNO (reactor neutrinos, mass ordering) plus low-energy solar and geo-neutrino physics; work spans scintillator chemistry and optical purity, photosensor characterization, and reconstruction. Relative to the established NV-ensemble quantum-sensing playbook (DEER, nanoscale NMR, T1 relaxometry at pT/sqrt(Hz) ensemble sensitivity), included as a detector-instrumentation pivot -- the transferable content is ultra-low-noise photon counting and calibration at scale, not spin physics.
Wyatt studies the structure, composition and dynamical evolution of circumstellar debris discs (using ALMA, Herschel and JWST imaging) as tracers of hidden planetary systems, linking dust production, planetesimal collisions and planet-disc interactions to the broader picture of planet formation.
Studies how planet-formation chemistry shapes the composition and habitability of young planets, using molecular line observations (e.g., ALMA) combined with numerical simulations.