Fisher Matrix Based Predictions for Measuring the z = 3.35 Binned 21-cm Power Spectrum using the Ooty Wide Field Array (OWFA)

Abstract

We use the Fisher matrix formalism to predict the prospects of measuring the redshifted 21-cm power spectrum in different $k$-bins using observations with the upcoming Ooty Wide Field Array (OWFA) which will operate at $326.5\mathrm{MHZ}$. This corresponds to neutral hydrogen (HI) at $z=3.35$, and a measurement of the 21-cm power spectrum provides an unique method to probe the large-scale structures at this redshift. Our analysis indicates that a $5\sigma$ detection of the binned power spectrum is possible in the $k$ range $0.05\le k\le 0.3{\mathrm{Mpc}}^{-1}$ with $1,000$ hours of observation. We find that the Signal-to-Noise ratio ($\mathrm{SNR}$) peaks in the $k$ range $0.1-0.2{\mathrm{Mpc}}^{-1}$ where a $10\sigma$ detection is possible with $2,000$ hours of observations. Our analysis also indicates that it is not very advantageous to observe much beyond $1,000$ hours in a single field of view as the $\mathrm{SNR}$ increases rather slowly beyond this in many of the small $k$-bins. The entire analysis reported here assumes that the foregrounds have been completely removed.

To appear in the Special Section of the JAA on the Ooty Wide Field Array

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Cited by in corpus (4)

• The Ooty Wide Field Array
• Modelling redshift-space distortion in the post-reionization $\mathrm{HI}$ 21-cm power spectrum
• Redshift space distortions of the {\rm HI} 21-cm intensity mapping signal due to the internal motions within galaxies
• An analytical method to simulate the HI 21-cm visibility signal for intensity mapping experiments