Comparison of observing modes for statistical estimation of the 21cm signal from the Epoch of Reionisation

TL;DR

This paper compares different observing modes for 21cm signal detection from the Epoch of Reionisation, analyzing their noise characteristics and effectiveness using a new framework applied to MWA data.

Contribution

It introduces a general framework for estimating power spectrum uncertainties across various observing modes and applies it to MWA data, highlighting the advantages of zenith drift scans.

Findings

Zenith drift scans can slightly reduce uncertainty compared to tracked scans.

The framework accounts for beam shape, antenna distribution, and mode coherence.

Application to MWA data demonstrates practical benefits of alternative observing modes.

Abstract

(Abridged) Noise considerations for experiments that aim to statistically estimate the 21 cm signal from high redshift neutral hydrogen during the Epoch of Reionisation (EoR) using interferometric data are typically computed assuming a tracked observation, where the telescope pointing centre and instrument phase centre are the same over the observation. Current low frequency interferometers use aperture arrays of fixed dipoles, which are steered electronically on the sky, and have different properties to mechanically-steered single apertures, such as reduced sensitivity away from zenith, and discrete pointing positions on the sky. Use of two additional observing modes is encouraged: (1) zenith drift, where the pointing centre remains fixed at the zenith, and the phase centre tracks the sky, and (2) drift+shift, where the telescope uses discrete pointing centres, and the sky drifts during each pointing. The coherence of measurements in these modes dictates the optimal reduction in thermal noise by combination of coherent modes, and the reduction in cosmic variance by combination of incoherent modes (views of different patches of the sky). The balance between these noise components provides one measure for the utility of these three modes for measuring a statistical EoR signature. We provide a general framework for estimating the uncertainty in the power spectrum for a given observing mode, telescope beam shape, and antenna distribution. We apply this framework to the Murchison Widefield Array (MWA) using an analysis of the 2D and 1D power spectra for 900 hours of observing. We demonstrate that zenith drift scans can yield marginally lower uncertainty in the signal power compared with tracked scans for the MWA EoR experiment.