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The statistical study of the Epoch of Reionisation (EoR) involves computing the power spectrum (variance) of the signal as a function of spatial wavenumber (k, measured in inverse megaparsec). The angular scales are obtained by Fourier Transform of radio astronomy images, or equivalently, we may directly use the visibilities (raw data) measured by an interferometer. The line-of-sight scales are computed by obtaining data in individual frequency channels, mapping those channels to cosmological distances, and then taking the Fourier Transform across frequency. This procedure assumes that the information within the observation volume (field-of-view times depth) is statistically equivalent. However, the 21cm cosmological signal of the EoR evolves with redshift, and taking Fourier Transforms over large redshift ranges dilutes and biases the signal.
In Trott (2016, MNRAS 1310, http://adsabs.harvard.edu/doi/10.1093/mnras/stw1310), we proposed using wavelets to perform wide bandwidth analysis, but with localised properties. This project takes those initial explorations and applies the methods to existing Murchison Widefield Array data. We aim to study the impact of foreground contamination in the wavelet space, and refine our wavelet methods based on optimising signal relative to noise and contamination.
This project may be part of the ARC Centre of Excellence for All-Sky Astrophysics in 3D (ASTRO-3D) EoR program, with potential for scholarship funding.

Simulated EoR power spectrum using a wavelet basis (left) versus the traditional Fourier basis (right). From Trott (2016).

Simulated EoR power spectrum using a wavelet basis (left) versus the traditional Fourier basis (right). From Trott (2016).

Co-Supervisor

Dr Steven Murray

Research Associate (CAASTRO)

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