ERRATUM: “WHAT NEXT-GENERATION 21 cm POWER SPECTRUM MEASUREMENTS CAN TEACH US ABOUT THE EPOCH OF REIONIZATION” (2014, ApJ, 782, 66)

Pober, Jonathan C.; Liu, Adrian; Dillon, Joshua S.; Aguirre, James E.; Bowman, Judd D.; Bradley, Richard F.; Carilli, C. L.; DeBoer, David R.; Hewitt, Jacqueline N.; Jacobs, Daniel C.; McQuinn, Matthew; Morales, M. F.; Parsons, Aaron; Tegmark, Max; Werthimer, Dan

doi:10.1088/0004-637x/788/1/96

Cited by 70 publications

(148 citation statements)

References 2 publications

Supporting

Mentioning

142

Contrasting

Order By: Relevance

“…We also see evidence in Figure 8 for non-negligible amounts of spillover of foreground emission (or suprahorizon emission) beyond the baseline's geometric horizon, which has also been observed by other 21 cm experiments (e.g. Pober et al 2013b;Beardsley et al 2016). Supra-horizon emission can come naturally from intrinsic spectral structure of the foregrounds.…”

Section: Antenna Cross Couplingssupporting

confidence: 81%

“…Cross multiplying a visibility with itself in Equation 2 to form a delay spectrum will result in an overall bias in power due to the noise present in the data. To avoid this, we take visibility spectra adjacent to each other in LST separated by 10.7 seconds and apply a phasing term to align their phase centers before cross multiplication (Pober et al 2013a). This means the two visibilities to leading order measure the same cosmological mode on the sky but have uncorrelated noise realizations, such that they do not produce a noise bias upon cross correlation.…”

Section: Delay Spectramentioning

confidence: 99%

“…As such, many of the current upper limits on the 21 cm power spectrum have been limited by instrumental systematics. Current and future experiments like the Hydrogen Epoch of Reionization Array (HERA; DeBoer et al 2017) and the Square Kilometer Array (SKA; Koopmans et al 2015) are nominally forecasted to provide high significance characterizations of the 21 cm signal and place constraints on IGM properties and the sources driving reionization (Pober et al 2014;Liu & Parsons 2016;Kern et al 2017). However, these forecasts neglect the impact of systematic contamination, which can significantly hamper an experiment's overall sensitivity and parameter constraining ability.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Mitigating Internal Instrument Coupling for 21 cm Cosmology. II. A Method Demonstration with the Hydrogen Epoch of Reionization Array

Kern¹,

Parsons²,

Dillon³

et al. 2020

ApJ

Self Cite

View full text Add to dashboard Cite

2 Kern et al.We present a study of internal reflection and cross coupling systematics in Phase 1 of the Hydrogen Epoch of Reionization Array (HERA). In a companion paper, we outlined the mathematical formalism for such systematics and presented algorithms for modeling and removing them from the data. In this work, we apply these techniques to data from HERA's first observing season as a method demonstration. The data show evidence for systematics that, without removal, would hinder a detection of the 21 cm power spectrum for the targeted EoR line-of-sight modes in the range 0.2 < k < 0.5 h −1 Mpc. After systematic removal, we find we can recover these modes in the power spectrum down to the integrated noise-floor of a nightly observation, achieving a dynamic range in the EoR window of 10 −6 in power (mK 2 units) with respect to the bright galactic foreground signal. In the absence of other systematics and assuming the systematic suppression demonstrated here continues to lower noise levels, our results suggest that fully-integrated HERA Phase I may have the capacity to set competitive upper limits on the 21 cm power spectrum. For future observing seasons, HERA will have upgraded analog and digital hardware to better control these systematics in the field.

show abstract

Section: Antenna Cross Couplingssupporting

confidence: 81%

Section: Delay Spectramentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Mitigating Internal Instrument Coupling for 21 cm Cosmology. II. A Method Demonstration with the Hydrogen Epoch of Reionization Array

Kern¹,

Parsons²,

Dillon³

et al. 2020

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…Nevertheless, the path towards detecting the 21 cm signal from the Cosmic Dawn and EoR has seen tremendous progress over the past decade, as first generation radio interferometric experiments such as the Donald C. Backer Precision Array for Probing the Epoch of Reionization (PAPER; Parsons et al 2014;Jacobs et al 2015;Ali et al 2015), the Murchison Widefield Array (MWA; Dillon et al 2014;Beardsley et al 2016;Ewall-Wice et al 2016), the Low Frequency Array (LOFAR; Patil et al 2017), and the Giant Metre Wave Radio Telescope (GMRT; Paciga et al 2013) have placed increasingly competitive limits on the 21 cm power spectrum, while single-dish experiments may have made a first detection of the global signal (Bowman et al 2018). Going forward, second generation interferometric experiments like the Hydrogen Epoch of Reionization Array (HERA; DeBoer et al 2017) and the Square Kilometer Array (SKA; Koopmans et al 2015) are expected to have the raw sensitivity needed to not only detect the 21 cm signal but provide a power spectrum characterization across a wide range of redshifts, leading to drastic improvements in our understanding of astrophysical and cosmological parameters that govern large scale structure and star formation at these epochs (Pober et al 2014;Ewall-Wice et al 2016;Kern et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Mitigating Internal Instrument Coupling for 21 cm Cosmology. I. Temporal and Spectral Modeling in Simulations

Kern

Parsons

Dillon

et al. 2019

ApJ

Self Cite

View full text Add to dashboard Cite

We study the behavior of internal signal chain reflections and antenna cross coupling as systematics for 21 cm cosmological surveys. We outline the mathematics for how these systematics appear in interferometric visibilities and describe their phenomenology. We then describe techniques for modeling and removing these systematics without attenuating the 21 cm signal in the data. This has critical implications for low-frequency radio surveys aiming to characterize the 21 cm signal from the Epoch of Reionization and Cosmic Dawn, as systematics can cause bright foreground emission to contaminate the EoR window and prohibit a robust detection. We also quantify the signal loss properties of the systematic modeling algorithms, and show that our techniques demonstrate resistance against EoR signal loss. In a companion paper, we demonstrate these methods on data from the Hydrogen Epoch of Reionization Array as a proof-of-concept.

show abstract

“…Phase II achieves lower noise levels by a factor of ∼ 2 to 5 (in mK 2 ) compared with Phase I over a wide range of scales. Comparisons with other facilities such as HERA, the Low-Frequency Array (LOFAR), and the Precision Array for Probing the Epoch of Reionization Figure 4) and the appendix of Pober et al (2014).…”

Section: Compact Configurationmentioning

confidence: 99%

Science with the Murchison Widefield Array: Phase I results and Phase II opportunities

Beardsley

Johnston‐Hollitt

Trott

et al. 2019

Publ. Astron. Soc. Aust.

View full text Add to dashboard Cite

The Murchison Widefield Array (MWA) is an open access telescope dedicated to studying the low frequency (80-300 MHz) southern sky. Since beginning operations in mid 2013, the MWA has opened a new observational window in the southern hemisphere enabling many science areas. The driving science objectives of the original design were to observe 21 cm radiation from the Epoch of Reionisation (EoR), explore the radio time domain, perform Galactic and extragalactic surveys, and monitor solar, heliospheric, and ionospheric phenomena. All together 60+ programs recorded 20,000 hours producing 146 papers to date. In 2016 the telescope underwent a major upgrade resulting in alternating compact and extended configurations. Other upgrades, including digital back-ends and a rapid-response triggering system, have been developed since the original array was commissioned. In this paper we review the major results from the prior operation of the MWA, and then discuss the new science paths enabled by the improved capabilities. We group these science opportunities by the four original science themes, but also include ideas for directions outside these categories.

show abstract

ERRATUM: “WHAT NEXT-GENERATION 21 cm POWER SPECTRUM MEASUREMENTS CAN TEACH US ABOUT THE EPOCH OF REIONIZATION” (2014, ApJ, 782, 66)

Cited by 70 publications

References 2 publications

Mitigating Internal Instrument Coupling for 21 cm Cosmology. II. A Method Demonstration with the Hydrogen Epoch of Reionization Array

Mitigating Internal Instrument Coupling for 21 cm Cosmology. II. A Method Demonstration with the Hydrogen Epoch of Reionization Array

Mitigating Internal Instrument Coupling for 21 cm Cosmology. I. Temporal and Spectral Modeling in Simulations

Science with the Murchison Widefield Array: Phase I results and Phase II opportunities

Contact Info

Product

Resources

About