• DOI:10.3847/1538-4357/ab55e4
• Corpus ID: 208268534

First Season MWA Phase II Epoch of Reionization Power Spectrum Results at Redshift 7

@article{Li2019FirstSM,
  title={First Season MWA Phase II Epoch of Reionization Power Spectrum Results at Redshift 7},
  author={W. Li and Jonathan C. Pober and Nichole Barry and Bryna J. Hazelton and Miguel F. Morales and Cathryn M. Trott and Adam E. Lanman and Michael J. Wilensky and I. S. Sullivan and Adam P. Beardsley and Tom Booler and Judd D. Bowman and Ruby L. Byrne and Brian Crosse and David Emrich and Thomas M. O. Franzen and Kenji Hasegawa and L. Horsley and Melanie Johnston-Hollitt and Daniel C. Jacobs and Christopher H. Jordan and Ronniy C. Joseph and Takeshi Kaneuji and David L. Kaplan and David Kenney and Kenji Kubota and Jack L. B. Line and Christene Lynch and Benjamin McKinley and Daniel A. Mitchell and Steven Murray and Dave Pallot and Bart Pindor and Masoud Rahimi and Jennifer Riding and Gregory Sleap and K. Steele and K. Takahashi and Steven J. Tingay and Mia Walker and Randall B. Wayth and Rachel L. Webster and A. Williams and C. Wu and J. Stuart B. Wyithe and Shintaro Yoshiura and Qian Zheng},
  journal={The Astrophysical Journal},
  year={2019},
  volume={887}
}

• W. Li, J. Pober, +44 authors Q. Zheng
• Published 23 November 2019
• Physics
• The Astrophysical Journal

The compact configuration of Phase II of the Murchison Widefield Array (MWA) consists of both a redundant subarray and pseudo-random baselines, offering unique opportunities to perform sky-model and redundant interferometric calibration. The highly redundant hexagonal cores give improved power spectrum sensitivity. In this paper, we present the analysis of nearly 40 hr of data targeting one of the MWA’s epoch of reionization (EoR) fields observed in 2016. We use both improved analysis techniques presented in Barry et al. and several additional techniques developed for this work, including data quality control methods and interferometric calibration approaches. We show the EoR power spectrum limits at redshift 6.5, 6.8, and 7.1 based on our deep analysis on this 40 hr data set. These limits span a range in k-space of 0.18 h Mpc−1 < k < 1.6 h Mpc−1, with a lowest measurement of Δ2 ≤ 2.39 × 103 mK2 at k = 0.59 h Mpc−1 and z = 6.5.