TY - JOUR
T1 - A Simplified, Lossless Reanalysis of PAPER-64
AU - Kolopanis, Matthew
AU - Jacobs, Daniel C.
AU - Cheng, Carina
AU - Parsons, Aaron R.
AU - Kohn, Saul A.
AU - Pober, Jonathan C.
AU - Aguirre, James E.
AU - Ali, Zaki S.
AU - Bernardi, Gianni
AU - Bradley, Richard F.
AU - Carilli, Chris L.
AU - Deboer, David R.
AU - Dexter, Matthew R.
AU - Dillon, Joshua S.
AU - Kerrigan, Joshua
AU - Klima, Pat
AU - Liu, Adrian
AU - MacMahon, David H.E.
AU - Moore, David F.
AU - Thyagarajan, Nithyanandan
AU - Nunhokee, Chuneeta D.
AU - Walbrugh, William P.
AU - Walker, Andre
N1 - Publisher Copyright:
© 2019. The American Astronomical Society. All rights reserved.
PY - 2019/10/1
Y1 - 2019/10/1
N2 - We present limits on the 21 cm power spectrum from the Epoch of Reionization using data from the 64 antenna configuration of the Donald C. Backer Precision Array for Probing the Epoch of Reionization (PAPER) analyzed through a power spectrum pipeline independent from previous PAPER analyses. Previously reported results from PAPER have been found to contain significant signal loss. Several lossy steps from previous PAPER pipelines have not been included in this analysis, namely delay-based foreground filtering, optimal fringe-rate filtering, and empirical covariance-based estimators. Steps that remain in common with previous analyses include redundant calibration and local sidereal time (LST) binning. The power spectra reported here are effectively the result of applying a linear Fourier transform analysis to the calibrated, LST-binned data. This analysis also uses more data than previous publications, including the complete available redshift range of z ∼ 7.5 to 11. In previous PAPER analyses, many power spectrum measurements were found to be detections of noncosmological power at levels of significance ranging from two to hundreds of times the theoretical noise. Here, excess power is examined using redundancy between baselines and power spectrum jackknives. The upper limits we find on the 21 cm power spectrum from reionization are (1500 mK)2, (1900 mK)2, (280mK)2, (200mK)2, (380mK)2, and (300mK)2 at redshifts z = 10.87, 9.93, 8.68, 8.37, 8.13, and 7.48, respectively. For reasons described in Cheng et al., these limits supersede all previous PAPER results.
AB - We present limits on the 21 cm power spectrum from the Epoch of Reionization using data from the 64 antenna configuration of the Donald C. Backer Precision Array for Probing the Epoch of Reionization (PAPER) analyzed through a power spectrum pipeline independent from previous PAPER analyses. Previously reported results from PAPER have been found to contain significant signal loss. Several lossy steps from previous PAPER pipelines have not been included in this analysis, namely delay-based foreground filtering, optimal fringe-rate filtering, and empirical covariance-based estimators. Steps that remain in common with previous analyses include redundant calibration and local sidereal time (LST) binning. The power spectra reported here are effectively the result of applying a linear Fourier transform analysis to the calibrated, LST-binned data. This analysis also uses more data than previous publications, including the complete available redshift range of z ∼ 7.5 to 11. In previous PAPER analyses, many power spectrum measurements were found to be detections of noncosmological power at levels of significance ranging from two to hundreds of times the theoretical noise. Here, excess power is examined using redundancy between baselines and power spectrum jackknives. The upper limits we find on the 21 cm power spectrum from reionization are (1500 mK)2, (1900 mK)2, (280mK)2, (200mK)2, (380mK)2, and (300mK)2 at redshifts z = 10.87, 9.93, 8.68, 8.37, 8.13, and 7.48, respectively. For reasons described in Cheng et al., these limits supersede all previous PAPER results.
KW - dark ages
KW - first stars
KW - reionization
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U2 - 10.3847/1538-4357/ab3e3a
DO - 10.3847/1538-4357/ab3e3a
M3 - Article
AN - SCOPUS:85074127513
SN - 0004-637X
VL - 883
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 133
ER -