I am the A.I. for New Messengers Postdoctoral Fellow at Vanderbilt University, USA, a position jointly offered by the Department of Physics and Astronomy and the Data Science Institute at Vanderbilt University. I obtained my PhD in Physics from The University of Western Australia in 2023, where I worked on developing deep learning models for rapid detection and sky localization of gravitational wave sources. My current research focuses on applying large language models for gravitational wave data analysis and inference from both individual and populations of sources.
I grew up in West Bengal, India, where I completed my Bachelors and Masters in Physics from Presidency University, Kolkata. During my Masters, I worked on the impact of self-interacting dark matter on cosmological large-scale structure formation. I am passionate about science communication and public outreach, having delivered several public talks and participated in science talk shows and podcasts. In addition to my interests in astronomy and physics, I enjoy reading, creative writing, films, and traveling.
PhD in Physics, 2023
The University of Western Australia
Masters in Physics, 2018
Presidency University, Kolkata
Bachelors in Physics, 2016
Presidency University, Kolkata
Responsibilities include:
Responsibilities include:
Responsibilities included:
For a full list of talks, please check CV.
We extend the work in Chatterjee & Jani, 2024 and demonstrate that AWaRe can be used to estimate gravitational wave reconstruction uncertainties. We further show that the uncertainties capture waveform systematics the model has not been trained on, including intermediate mass black holes and eccentricity.
We have developed a deep learning model, AWaRe, that is capable of producing accurate reconstructions of gravitational wave signals from real LIGO data. We demonstrate that the model is robust against complex waveform systematics like precession and the presence of higher multipoles.
We have developed a deep learning model, called GW-SkyLocator, to obtain the posterior distribution of the sky location of gravitational wave sources. This method is applicable for all three categories of compact binary coalescences - binary black holes, binary neutron stars and neutron star-black hole binaries.