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

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.

arXiv comment11 pages, 8 figures. Accepted for publication in Proceedings of the Astronomical Society of Australia (PASA)

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Cited by in corpus (17)

• Data Analysis for Precision 21 cm Cosmology
• First Season MWA EoR Power Spectrum Results at Redshift 7
• Improving the Epoch of Reionization Power Spectrum Results from Murchison Widefield Array Season 1 Observations
• Low frequency observations of linearly polarized structures in the interstellar medium near the south Galactic pole
• Mapmaking for Precision 21 cm Cosmology
• The effect of baseline layouts on the EoR foreground wedge: a semi-analytical approach
• Extracting the 21 cm EoR signal using MWA drift scan data
• Fundamental uncertainty levels of 21cm power spectra from a delay analysis
• Beamforming Errors in Murchison Widefield Array Phased Array Antennas and their effects on Epoch of Reionization Science
• Observing the Reionization : Effect of Calibration and Position Errors on Realistic Observation Conditions
• Methods of Error Estimation for Delay Power Spectra in $21\text{cm}$ Cosmology
• The Impact of Tandem Redundant/Sky-Based Calibration in MWA Phase II Data Analysis
• Study of Redshifted HI from the Epoch of Reionization with Drift scan
• Unlocking Sensitivity for Visibility-based Estimators of the 21 cm Reionization Power Spectrum
• The Tracking Tapered Gridded Estimator (TTGE) for the power spectrum from drift scan observations
• Measuring the global 21-cm signal with the MWA-II: improved characterisation of lunar-reflected radio frequency interference
• Detecting 21 cm EoR Signal using Drift Scans: Correlation of Time-ordered Visibilities