Customized noise modelling for pulsar timing

This project focuses on developing and applying customized chromatic noise models for pulsar timing datasets. Chromatic noise is radio frequency-dependent timing variability which can arise from a variety of astrophysical effects, including interstellar medium (ISM) propagation, scattering, and solar activity. Standard noise models often assume simplified or uniform chromatic behavior across the pulsar array, potentially biasing gravitational wave background (GWB) searches and other signal recovery efforts.

To address this, the project introduces pulsar-specific chromatic noise models that account for individual pulsars’ unique ISM environments and observational characteristics. Using a combination of Bayesian inference techniques and pulsar timing software (e.g., enterprise), we implement radio frequency-dependent Gaussian process modeled tailored to each pulsar. These models aim to better isolate GWB signatures by improving the modeling of chromatic noise.

This work contributes to the broader effort of refining PTA sensitivity and enhancing the robustness of low-frequency gravitational wave detection. It also lays groundwork for future analyses of chromatic systematics in PTA datasets and their implications for pulsar astrophysics and gravitational wave astronomy.