Speaker
Description
Pulsar timing array experiments (PTAs) aim to detect ultra-low-frequency (∼1–100 nHz) gravitational waves (GWs) by monitoring an ensemble of millisecond pulsars (MSPs) distributed across the Galaxy. The intrinsic wander of the rotation rate of the constituent pulsars, variations in dispersion measure (DM), scatter-broadening, and instrumental noise of radio telescopes often correlate with the slowly varying GW signature in the data and act as sources of chromatic and achromatic noise. Consequently, the detection and characterization of GWs heavily rely on accurate noise modeling, which may require custom approaches for each pulsar. In this presentation, I will discuss the recent efforts of single-pulsar noise analysis by the Indian Pulsar Timing Array experiment. In this study, we focus on modeling white noise, achromatic red noise, dispersion measure variations, and scattering variations. We employ Bayesian model selection techniques to determine the most appropriate noise models for each pulsar.
| Track type | Gravitational waves |
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