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http://hdl.handle.net/20.500.12386/31224
Title: | Detection of Cosmic Structures using the Bispectrum Phase. II. First Results from Application to Cosmic Reionization Using the Hydrogen Epoch of Reionization Array | Authors: | Nithyanandan Thyagarajan Chris L. Carilli Bojan Nikolic James Kent Andrei Mesinger Nicholas S. Kern BERNARDI, GIANNI Siyanda Matika Zara Abdurashidova James E. Aguirre Paul Alexander Zaki S. Ali Yanga Balfour Adam P. Beardsley Tashalee S. Billings Judd D. Bowman Richard F. Bradley Jacob Burba Steve Carey Carina Cheng David R. DeBoer Matt Dexter Eloy de Lera Acedo Joshua S. Dillon John Ely Aaron Ewall-Wice Nicolas Fagnoni Randall Fritz Steven R. Furlanetto Kingsley Gale-Sides Brian Glendenning Deepthi Gorthi Bradley Greig Jasper Grobbelaar Ziyaad Halday Bryna J. Hazelton Jacqueline N. Hewitt Jack Hickish Daniel C. Jacobs Austin Julius Joshua Kerrigan Piyanat Kittiwisit Saul A. Kohn Matthew Kolopanis Adam Lanman Paul La Plante Telalo Lekalake David Lewis Adrian Liu David MacMahon Lourence Malan Cresshim Malgas Matthys Maree Zachary E. Martinot Eunice Matsetela Mathakane Molewa Miguel F. Morales Tshegofalang Mosiane Abraham R. Neben Aaron R. Parsons Nipanjana Patra Samantha Pieterse Jonathan C. Pober Nima Razavi-Ghods Jon Ringuette James Robnett Kathryn Rosie Peter Sims Craig Smith Angelo Syce Peter K. G. Williams Haoxuan Zheng |
Issue Date: | 2020 | Journal: | PHYSICAL REVIEW D | Number: | 102 | Issue: | 2 | Abstract: | Characterizing the epoch of reionization (EoR) at $z\gtrsim 6$ via the redshifted 21 cm line of neutral Hydrogen (HI) is critical to modern astrophysics and cosmology, and thus a key science goal of many current and planned low-frequency radio telescopes. The primary challenge to detecting this signal is the overwhelmingly bright foreground emission at these frequencies, placing stringent requirements on the knowledge of the instruments and inaccuracies in analyses. Results from these experiments have largely been limited not by thermal sensitivity but by systematics, particularly caused by the inability to calibrate the instrument to high accuracy. The interferometric bispectrum phase is immune to antenna-based calibration and errors therein, and presents an independent alternative to detect the EoR HI fluctuations while largely avoiding calibration systematics. Here, we provide a demonstration of this technique on a subset of data from the Hydrogen Epoch of Reionization Array (HERA) to place approximate constraints on the brightness temperature of the intergalactic medium (IGM). From this limited data, at $z=7.7$ we infer "$1\sigma$" upper limits on the IGM brightness temperature to be $\le 316$ "pseudo" mK at $\kappa_\parallel=0.33$ "pseudo" $h$ Mpc$^{-1}$ (data-limited) and $\le 1000$ "pseudo" mK at $\kappa_\parallel=0.875$ "pseudo" $h$ Mpc$^{-1}$ (noise-limited). The "pseudo" units denote only an approximate and not an exact correspondence to the actual distance scales and brightness temperatures. By propagating models in parallel to the data analysis, we confirm that the dynamic range required to separate the cosmic HI signal from the foregrounds is similar to that in standard approaches, and the power spectrum of the bispectrum phase is still data-limited (at $\gtrsim 10^6$ dynamic range) indicating scope for further improvement in sensitivity as the array build-out continues. | URI: | http://hdl.handle.net/20.500.12386/31224 | URL: | https://journals.aps.org/prd/abstract/10.1103/PhysRevD.102.022002 http://arxiv.org/abs/2005.10275v2 |
ISSN: | 2470-0010 | DOI: | 10.1103/PhysRevD.102.022002 | Bibcode ADS: | 2020PhRvD.102b2002T | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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