PhD candidate at the University of Alberta
I study how stars, stellar clusters, and the ISM evolve across cosmic time using JWST, HST, and VLA data within PHANGS, and I developed Neloura, a platform for astronomical image visualization, cataloging, SED inspection, and interactive source finding designed for the next generation of datasets such as SKA.
I am currently focused on multi-wavelength diagnostics that connect dust physics, stellar clusters, and the ISM across nearby galaxies, combining infrared, optical, ultraviolet, millimeter, and radio observations with advanced visualization tools to uncover how stellar clusters evolve and how feedback, dust, and environment shape their emission.
Student governance roles that keep my research accountable to people first.
Recent lead-author work using multi-wavelength data from JWST, HST, ALMA, and AstroSat, with each entry noting the analysis or tools I led.
My research with JWST has defined a new framework for tracing how stellar clusters evolve from their dusty, embedded birth to their exposed and evolved stages across nearby galaxies. I led the first systematic censuses of compact mid-infrared sources using JWST imaging, identifying and characterizing tens of thousands of stellar clusters spanning the full evolutionary sequence—from deeply embedded stellar clusters to red-supergiant and AGB-dominated populations.
Read on arXiv →
Using AstroSat/UVIT, I calibrated over 150 maps of 31 nearby galaxies at ~1.4″ (25–160 pc) resolution, providing the sharpest wide-field UV images across 9 filters from 1480 Å to 2790 Å. Combined with MUSE Hα and ALMA CO(2–1) data, these maps reveal that the FUV/Hα ratio varies by nearly two dex, decreasing in high-pressure centers and bars—evidence that clusters clear their natal gas more rapidly in dense environments. After correcting for attenuation and controlling for stellar mass and metallicity, FUV/Hα increases with stellar population age, tracing cluster emergence as H II regions fade. We also identified extended ultraviolet disks—faint, outer-disk structures marking recent star formation beyond the optical radius.
Read the paper → Data→
My research asks how long massive clusters remain hidden in their dusty, embedded phase before emerging as feedback-dominated systems. I find that such regions are rare in nearby galaxies, implying a short lifetime of only a few million years. Combining mid-infrared and optical diagnostics, I show that 21 µm emission robustly traces nascent (< 5 Myr) clusters and correlates tightly with Hα emission over five orders of magnitude
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Using single-dish and interferometric observations spanning three frequency bands from 0.16 to 4.8 GHz—including GLEAM/MWA (166 MHz) as the low-frequency SKA precursor, and ATCA and Parkes data—I combined multi-band radio maps with de-reddened Hα emission to produce the spatially resolved thermal and non-thermal component maps of the Magellanic Clouds. Whereas previous studies have established that cosmic-ray electrons steepen their synchrotron spectra as they propagate, and that magnetic-field strength correlates with the star formation rate, my study goes further. Using resolved radio continuum maps of these metal-poor galaxies, I demonstrate for the first time across ISM phases that non-thermal (cosmic-ray + magnetic-field) energy dominates the ISM under equipartition, and that magnetic-field amplification and cosmic-ray feedback are tightly coupled to the star formation rate even in low-metallicity regimes.
Read on MNRAS →