Characterizing Signal Loss in the 21 cm Reionization Power Spectrum: A Revised Study of PAPER-64
The Epoch of Reionization (EoR) is an uncharted era in our universe's history during which the birth of the first stars and galaxies led to the ionization of neutral hydrogen in the intergalactic medium. There are many experiments investigating the EoR by tracing the 21 cm line of neutral hydro...
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Published in | The Astrophysical journal Vol. 868; no. 1; pp. 26 - 46 |
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Main Authors | , , , , , , , , , , , , , , , , , , , , |
Format | Journal Article |
Language | English |
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Philadelphia
The American Astronomical Society
20.11.2018
IOP Publishing |
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Abstract | The Epoch of Reionization (EoR) is an uncharted era in our universe's history during which the birth of the first stars and galaxies led to the ionization of neutral hydrogen in the intergalactic medium. There are many experiments investigating the EoR by tracing the 21 cm line of neutral hydrogen. Because this signal is very faint and difficult to isolate, it is crucial to develop analysis techniques that maximize sensitivity and suppress contaminants in data. It is also imperative to understand the trade-offs between different analysis methods and their effects on power spectrum estimates. Specifically, with a statistical power spectrum detection in HERA's foreseeable future, it has become increasingly important to understand how certain analysis choices can lead to the loss of the EoR signal. In this paper, we focus on signal loss associated with power spectrum estimation. We describe the origin of this loss using both toy models and data taken by the 64-element configuration of the Donald C. Backer Precision Array for Probing the Epoch of Reionization (PAPER). In particular, we highlight how detailed investigations of signal loss have led to a revised, higher 21 cm power spectrum upper limit from PAPER-64. Additionally, we summarize errors associated with power spectrum error estimation that were previously unaccounted for. We focus on a subset of PAPER-64 data in this paper; revised power spectrum limits from the PAPER experiment are presented in a forthcoming paper by Kolopanis et al. and supersede results from previously published PAPER analyses. |
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AbstractList | The Epoch of Reionization (EoR) is an uncharted era in our universe's history during which the birth of the first stars and galaxies led to the ionization of neutral hydrogen in the intergalactic medium. There are many experiments investigating the EoR by tracing the 21 cm line of neutral hydrogen. Because this signal is very faint and difficult to isolate, it is crucial to develop analysis techniques that maximize sensitivity and suppress contaminants in data. It is also imperative to understand the trade-offs between different analysis methods and their effects on power spectrum estimates. Specifically, with a statistical power spectrum detection in HERA's foreseeable future, it has become increasingly important to understand how certain analysis choices can lead to the loss of the EoR signal. In this paper, we focus on signal loss associated with power spectrum estimation. We describe the origin of this loss using both toy models and data taken by the 64-element configuration of the Donald C. Backer Precision Array for Probing the Epoch of Reionization (PAPER). In particular, we highlight how detailed investigations of signal loss have led to a revised, higher 21 cm power spectrum upper limit from PAPER-64. Additionally, we summarize errors associated with power spectrum error estimation that were previously unaccounted for. We focus on a subset of PAPER-64 data in this paper; revised power spectrum limits from the PAPER experiment are presented in a forthcoming paper by Kolopanis et al. and supersede results from previously published PAPER analyses. Abstract The Epoch of Reionization (EoR) is an uncharted era in our universe’s history during which the birth of the first stars and galaxies led to the ionization of neutral hydrogen in the intergalactic medium. There are many experiments investigating the EoR by tracing the 21 cm line of neutral hydrogen. Because this signal is very faint and difficult to isolate, it is crucial to develop analysis techniques that maximize sensitivity and suppress contaminants in data. It is also imperative to understand the trade-offs between different analysis methods and their effects on power spectrum estimates. Specifically, with a statistical power spectrum detection in HERA’s foreseeable future, it has become increasingly important to understand how certain analysis choices can lead to the loss of the EoR signal. In this paper, we focus on signal loss associated with power spectrum estimation. We describe the origin of this loss using both toy models and data taken by the 64-element configuration of the Donald C. Backer Precision Array for Probing the Epoch of Reionization (PAPER). In particular, we highlight how detailed investigations of signal loss have led to a revised, higher 21 cm power spectrum upper limit from PAPER-64. Additionally, we summarize errors associated with power spectrum error estimation that were previously unaccounted for. We focus on a subset of PAPER-64 data in this paper; revised power spectrum limits from the PAPER experiment are presented in a forthcoming paper by Kolopanis et al. and supersede results from previously published PAPER analyses. |
Author | Aguirre, James E. Nunhokee, Chuneeta D. Carilli, Chris L. Pober, Jonathan C. Ali, Zaki S. Bernardi, Gianni MacMahon, David H. E. DeBoer, David R. Moore, David F. Dexter, Matthew R. Kolopanis, Matthew Liu, Adrian Klima, Pat Jacobs, Daniel C. Cheng, Carina Bradley, Richard F. Walbrugh, William P. Kohn, Saul A. Parsons, Aaron R. Dillon, Joshua S. Walker, Andre |
Author_xml | – sequence: 1 givenname: Carina surname: Cheng fullname: Cheng, Carina email: ccheng@berkeley.edu organization: University of California Astronomy Department, Berkeley, CA, USA – sequence: 2 givenname: Aaron R. surname: Parsons fullname: Parsons, Aaron R. organization: University of California Radio Astronomy Laboratory, Berkeley, CA, USA – sequence: 3 givenname: Matthew surname: Kolopanis fullname: Kolopanis, Matthew organization: Arizona State University School of Earth and Space Exploration, Tempe, AZ, USA – sequence: 4 givenname: Daniel C. orcidid: 0000-0002-0917-2269 surname: Jacobs fullname: Jacobs, Daniel C. organization: Arizona State University School of Earth and Space Exploration, Tempe, AZ, USA – sequence: 5 givenname: Adrian orcidid: 0000-0001-6876-0928 surname: Liu fullname: Liu, Adrian organization: Berkeley Center for Cosmological Physics, Berkeley, CA, USA – sequence: 6 givenname: Saul A. orcidid: 0000-0001-6744-5328 surname: Kohn fullname: Kohn, Saul A. organization: University of Pennsylvania Department of Physics and Astronomy, Philadelphia, PA, USA – sequence: 7 givenname: James E. orcidid: 0000-0002-4810-666X surname: Aguirre fullname: Aguirre, James E. organization: University of Pennsylvania Department of Physics and Astronomy, Philadelphia, PA, USA – sequence: 8 givenname: Jonathan C. surname: Pober fullname: Pober, Jonathan C. organization: Department of Physics, Brown University , Providence, RI, USA – sequence: 9 givenname: Zaki S. surname: Ali fullname: Ali, Zaki S. organization: University of California Astronomy Department, Berkeley, CA, USA – sequence: 10 givenname: Gianni orcidid: 0000-0002-0916-7443 surname: Bernardi fullname: Bernardi, Gianni organization: INAF-Instituto di Radioastronomia, Bologna, Italy – sequence: 11 givenname: Richard F. surname: Bradley fullname: Bradley, Richard F. organization: University of Virginia Department of Astronomy, Charlottesville, VA, USA – sequence: 12 givenname: Chris L. orcidid: 0000-0001-6647-3861 surname: Carilli fullname: Carilli, Chris L. organization: Cavendish Laboratory, Cambridge, UK – sequence: 13 givenname: David R. surname: DeBoer fullname: DeBoer, David R. organization: University of California Radio Astronomy Laboratory, Berkeley, CA, USA – sequence: 14 givenname: Matthew R. surname: Dexter fullname: Dexter, Matthew R. organization: University of California Radio Astronomy Laboratory, Berkeley, CA, USA – sequence: 15 givenname: Joshua S. orcidid: 0000-0003-3336-9958 surname: Dillon fullname: Dillon, Joshua S. organization: University of California Astronomy Department, Berkeley, CA, USA – sequence: 16 givenname: Pat surname: Klima fullname: Klima, Pat organization: National Radio Astronomy Observatory, Charlottesville, VA, USA – sequence: 17 givenname: David H. E. surname: MacMahon fullname: MacMahon, David H. E. organization: University of California Radio Astronomy Laboratory, Berkeley, CA, USA – sequence: 18 givenname: David F. surname: Moore fullname: Moore, David F. organization: University of Pennsylvania Department of Physics and Astronomy, Philadelphia, PA, USA – sequence: 19 givenname: Chuneeta D. orcidid: 0000-0002-5445-6586 surname: Nunhokee fullname: Nunhokee, Chuneeta D. organization: Department of Physics and Electronics, Rhodes University , South Africa – sequence: 20 givenname: William P. surname: Walbrugh fullname: Walbrugh, William P. organization: Square Kilometre Array, Cape Town, South Africa – sequence: 21 givenname: Andre surname: Walker fullname: Walker, Andre organization: Square Kilometre Array, Cape Town, South Africa |
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Copyright | 2018. The American Astronomical Society. All rights reserved. Copyright IOP Publishing Nov 20, 2018 |
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Snippet | The Epoch of Reionization (EoR) is an uncharted era in our universe's history during which the birth of the first stars and galaxies led to the ionization of... Abstract The Epoch of Reionization (EoR) is an uncharted era in our universe’s history during which the birth of the first stars and galaxies led to the... The Epoch of Reionization (EoR) is an uncharted era in our universe’s history during which the birth of the first stars and galaxies led to the ionization of... |
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SubjectTerms | Astrophysics Contaminants dark ages, reionization, first stars early universe Galaxies Hydrogen Intergalactic media Ionization large-scale structure of universe methods: data analysis methods: statistical Sensitivity analysis techniques: interferometric Thermal energy |
Title | Characterizing Signal Loss in the 21 cm Reionization Power Spectrum: A Revised Study of PAPER-64 |
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