Simulated predictions for H i at z = 3.35 with the Ooty Wide Field Array (OWFA) – II. Foreground avoidance. Issue 4 (29th October 2020)

• Record Type: Journal Article
• Authors: Chatterjee, Suman; Bharadwaj, Somnath; Marthi, Visweshwar Ram
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 500:Issue 4(2021)
• Page Start: 4398
• Page End: 4413
• Publication Date: 2020-10-29
• Subjects: techniques: interferometric -- diffuse radiation -- large-scale structure of Universe -- cosmology: observations; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa3348
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Considering the upcoming OWFA, we use simulations of the foregrounds and the z = 3.35 H i 21-cm intensity mapping signal to identify the ( k ⊥, k ∥ ) modes where the expected 21-cm power spectrum P ( k ⊥, k ∥ ) is substantially larger than the predicted foreground contribution. Only these uncontaminated k modes are used for measuring P ( k ⊥, k ∥ ) in the "Foreground Avoidance" technique. Though the foregrounds are largely localized within a wedge. we find that the small leakage beyond the wedge surpasses the 21-cm signal across a significant part of the ( k ⊥, k ∥ ) plane. The extent of foreground leakage is extremely sensitive to the frequency window function used to estimate P ( k ⊥, k ∥ ). It is possible to reduce the leakage by making the window function narrower; however, this comes at the expense of losing a larger fraction of the 21-cm signal. It is necessary to balance these competing effects to identify an optimal window function. Considering a broad class of cosine window functions, we identify a six term window function as optimal for 21-cm power spectrum estimation with OWFA. Considering only the k modes where the expected 21-cm power spectrum exceeds the predicted foregrounds by a factor of 100 or larger, a $5\, \sigma$ detection of the binned power spectrum is possible in the k -ranges $0.18 \le k \le 0.3 \, {\rm Mpc}^{-1}$ and $0.18 \le k \le 0.8 \, {\rm Mpc}^{-1}$ with 1000–2000 and 10 4 h of observation, respectively.