The Tracking Tapered Gridded Estimator (TTGE) for the power spectrum from drift scan observations

Abstract

Intensity mapping with the redshifted 21-cm line is an emerging tool in cosmology. Drift scan observations, where the antennas are fixed to the ground and the telescope's pointing center (PC) changes continuously on the sky due to earth's rotation, provide broad sky coverage and sustained instrumental stability needed for 21-cm intensity mapping. Here we present the Tracking Tapered Grided Estimator (TTGE) to quantify the power spectrum of the sky signal estimated directly from the visibilities measured in drift scan radio interferometric observations. The TTGE uses the data from the different PC to estimate the power spectrum of the signal from a small angular region located around a fixed tracking center (TC). The size of this angular region is decided by a suitably chosen tapering window function which serves to reduce the foreground contamination from bright sources located at large angles from the TC. It is possible to cover the angular footprint of the drift scan observations using multiple TC, and combine the estimated power spectra to increase the signal to noise ratio. Here we have validated the TTGE using simulations of $154\mathrm{MHz}$ MWA drift scan observations. We show that the TTGE can recover the input model angular power spectrum $C_{\ell }$ within $20\%$ accuracy over the $\ell$ range $40<\ell <700$.

arXiv commentAccepted for publication in MNRAS

References in corpus (89)

• HEALPix -- a Framework for High Resolution Discretization, and Fast Analysis of Data Distributed on the Sphere
• LOFAR: The LOw-Frequency ARray
• Cosmology at Low Frequencies: The 21 cm Transition and the High-Redshift Universe
• The Murchison Widefield Array: the Square Kilometre Array Precursor at low radio frequencies
• 21-cm cosmology
• Hydrogen Epoch of Reionization Array (HERA)
• Reionization and Cosmology with 21 cm Fluctuations
• Cosmological Parameter Estimation Using 21 cm Radiation from the Epoch of Reionization
• The Precision Array for Probing the Epoch of Reionization: 8 Station Results
• Bright Source Subtraction Requirements For Redshifted 21 cm Measurements
• What Next-Generation 21 cm Power Spectrum Measurements Can Teach Us About the Epoch of Reionization
• Reionization and the Cosmic Dawn with the Square Kilometre Array
• A simulation calibrated limit on the HI power spectrum from the GMRT Epoch of Reionization experiment
• A Per-Baseline, Delay-Spectrum Technique for Accessing the 21cm Cosmic Reionization Signature
• Improved upper limits on the 21-cm signal power spectrum of neutral hydrogen at $\mathbf{z}\approx 9.1$ from LOFAR
• Multifrequency analysis of 21 cm fluctuations from the Era of Reionization
• Upper limits on the 21-cm Epoch of Reionization power spectrum from one night with LOFAR
• The Epoch of Reionization Window: I. Mathematical Formalism
• Foreground simulations for the LOFAR - Epoch of Reionization Experiment
• PAPER-64 Constraints on Reionization: The 21cm Power Spectrum at z=8.4
• Imaging the Epoch of Reionization: limitations from foreground confusion and imaging algorithms
• Deep multi-redshift limits on Epoch of Reionisation 21cm Power Spectra from Four Seasons of Murchison Widefield Array Observations
• Radio Foregrounds for the 21cm Tomography of the Neutral Intergalactic Medium at High Redshifts
• The Epoch of Reionization Window: II. Statistical Methods for Foreground Wedge Reduction
• The impact of point source subtraction residuals on 21 cm Epoch of Reionization estimation
• First Results from HERA Phase I: Upper Limits on the Epoch of Reionization 21 cm Power Spectrum
• Overcoming real-world obstacles in 21 cm power spectrum estimation: A method demonstration and results from early Murchison Widefield Array data
• All-Sky Interferometry with Spherical Harmonic Transit Telescopes
• Foregrounds for observations of the cosmological 21 cm line: I. First Westerbork measurements of Galactic emission at 150 MHz in a low latitude field
• The GMRT-EoR Experiment: A new upper limit on the neutral hydrogen power spectrum at z~8.6
• Foreground Contamination in Interferometric Measurements of the Redshifted 21 cm Power Spectrum
• Opening the 21cm EoR Window: Measurements of Foreground Isolation with PAPER
• Foreground Removal using FastICA: A Showcase of LOFAR-EoR
• Coaxing Cosmic 21cm Fluctuations from the Polarized Sky using m-mode Analysis
• A study of fundamental limitations to statistical detection of redshifted HI from the epoch of reionization
• On using visibility correlations to probe the HI distribution from the dark ages to the present epoch I: Formalism and the expected signal
• Foregrounds in Wide-Field Redshifted 21 cm Power Spectra
• Initial deep LOFAR observations of Epoch of Reionization windows: I. The North Celestial Pole
• A simplified, lossless re-analysis of PAPER-64
• Improving the Epoch of Reionization Power Spectrum Results from Murchison Widefield Array Season 1 Observations
• Power Spectrum Sensitivity and the Design of Epoch of Reionization Observatories
• Statistical 21-cm Signal Separation via Gaussian Process Regression Analysis
• Empirical Covariance Modeling for 21 cm Power Spectrum Estimation: A Method Demonstration and New Limits from Early Murchison Widefield Array 128-Tile Data
• Foregrounds for redshifted 21 cm studies of reionization: GMRT 153 MHz observations
• The multi-frequency angular power spectrum of the epoch of reionization 21 cm signal
• Characterizing Foreground for redshifted 21-cm radiation: 150 MHz GMRT observations
• The first power spectrum limit on the 21-cm signal of neutral hydrogen during the Cosmic Dawn at z=20-25 from LOFAR
• How well can we measure and understand foregrounds with 21 cm experiments?
• HI Fluctuations at Large Redshifts: I--Visibility correlation
• Studying Galactic interstellar turbulence through fluctuations in synchrotron emission: First LOFAR Galactic foreground detection
• First Season MWA Phase II EoR Power Spectrum Results at Redshift 7
• The Importance of Wide-field Foreground Removal for 21 cm Cosmology: A Demonstration With Early MWA Epoch of Reionization Observations
• Tight Constraints on the Excess Radio Background at $z=9.1$ from LOFAR
• The Radio Sky at Meter Wavelengths: m-Mode Analysis Imaging with the Owens Valley Long Wavelength Array
• The GMRT EoR Experiment: Limits on Polarized Sky Brightness at 150 MHz
• Improved foreground removal in GMRT 610 MHz observations towards redshifted 21-cm tomography
• The Murchison Widefield Array 21 cm Power Spectrum Analysis Methodology
• Characterizing Signal Loss in the 21 cm Reionization Power Spectrum: A Revised Study of PAPER-64
• Visibility based angular power spectrum estimation in low frequency radio interferometric observations
• Towards simulating and quantifying the light-cone EoR 21-cm signal
• Spherical Harmonic Analyses of Intensity Mapping Power Spectra
• GMRT observation towards detecting the Post-reionization 21-cm signal
• The visibility based Tapered Gridded Estimator (TGE) for the redshifted 21-cm power spectrum
• Source counts and confusion at 72-231 MHz in the MWA GLEAM survey
• Optimized Beam Sculpting with Generalized Fringe-Rate Filters
• Software Holography: Interferometric Data Analysis for the Challenges of Next Generation Observatories
• Detailed study of ELAIS N1 field with the uGMRT -- II. Source Properties and Spectral Variation Of Foreground Power Spectrum from 300-500 MHz Observations
• Polarization leakage in epoch of reionization windows: III. Wide-field effects of narrow-field arrays
• Tapering the sky response for angular power spectrum estimation from low-frequency radio-interferometric data
• Demonstrating the Tapered Gridded Estimator (TGE) for the Cosmological HI 21-cm Power Spectrum using $150\mathrm{MHz}$ GMRT observations
• Foreground modelling via Gaussian process regression: an application to HERA data
• Prospects for detecting the 326.5 MHz redshifted 21 cm HI signal with the Ooty Radio Telescope (ORT)
• Predictions for measuring the 21-cm multi-frequency angular power spectrum using SKA-Low
• The angular power spectrum measurement of the Galactic synchrotron emission in two fields of the TGSS survey
• Detecting Cosmic Reionization using Bi-Spectrum Phase
• A Tapered Gridded Estimator (TGE) for the Multi-Frequency Angular Power Spectrum (MAPS) and the Cosmological HI 21-cm Power Spectrum
• All sky angular power spectrum: I. Estimating brightness temperature fluctuations using TGSS 150 MHz survey
• Detection of Cosmic Structures using the Bispectrum Phase. II. First Results from Application to Cosmic Reionization Using the Hydrogen Epoch of Reionization Array
• Detailed study of the ELAIS N1 field with the uGMRT - I. Characterizing the 325 MHz foreground for redshifted 21 cm observations
• Exploring the evolution of Reionisation using a wavelet transform and the light cone effect
• Extracting the 21 cm EoR signal using MWA drift scan data
• Characterizing EoR foregrounds: A study of the Lockman Hole Region at 325 MHz
• Comparison of observing modes for statistical estimation of the 21cm signal from the Epoch of Reionisation
• A study of Kepler supernova remnant: angular power spectrum estimation from radio frequency data
• An Image-based Tapered Gridded Estimator (ITGE) for the angular power spectrum
• Study of Redshifted HI from the Epoch of Reionization with Drift scan
• An analytical method to simulate the HI 21-cm visibility signal for intensity mapping experiments
• Simulated Predictions for HI at $z=3.35$ with the Ooty Wide Field Array (OWFA) -- II: Foreground Avoidance
• Detecting 21 cm EoR Signal using Drift Scans: Correlation of Time-ordered Visibilities

Cited by in corpus (2)

• Towards $21$-cm intensity mapping at $z=2.28$ with uGMRT using the tapered gridded estimator III: Foreground removal
• The Tracking Tapered Gridded Estimator for the 21-cm power spectrum from MWA drift scan observations I: Validation and preliminary results