MEASUREMENT OF 21 cm BRIGHTNESS FLUCTUATIONS AT z ∼ 0.8 IN CROSS-CORRELATION

By K. Masui, E. Switzer, N. Banavar, K. Bandura, C. Blake, L.-M. Calin, Tzu-Ching Chang, Xiaodian Chen, Yin-Jie Li, Yu-Wei Liao and 5 more. 2012

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In this Letter, 21 cm intensity maps acquired at the Green Bank Telescope are cross-correlated with large-scale structure traced by galaxies in the WiggleZ Dark Energy Survey. The data span the redshift range 0.6 < z < 1 over two fields totaling ∼41 deg. sq. and 190 hr of radio integration time. The cross-correlation constrains ΩH IbH Ir = [0.43 ± 0.07(stat.) ± 0.04(sys.)] × 10−3, where ΩH I is the neutral hydrogen (H i) fraction, r is the galaxy–hydrogen correlation coefficient, and bH I is the H i bias parameter. This is the most precise constraint on neutral hydrogen density fluctuations in a challenging redshift range. Our measurement improves the previous 21 cm cross-correlation at z ∼ 0.8 both in its precision and in the range of scales probed.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a3140c2b9b0f2cd0744420751ac7bcd0b015c7ef

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Citations in the corpus

A simulation-calibrated limit on the H i power spectrum from the GMRT Epoch of Reionization experiment (2013, methodology): “A similar technique has been used by Chang et al. (2010) and Masui et al. (2013) to clean foregrounds for H I intensity mapping at C alifornia Institute of T echnology on Septem ber 5, 2013 http://m nras.oxfordjournals.org/ D ow nloaded from at z ≈ 0.8, where the relative dominance of foregrounds…”
PAPER-64 CONSTRAINTS ON REIONIZATION: THE 21 cm POWER SPECTRUM AT z = 8.4 (2015, unknown): “…(Wang et al. 2006; Bowman et al. 2009a; Liu et al. 2009a), principal component analysis (Paciga et al. 2011; Liu & Tegmark 2011; Paciga et al. 2013; Masui et al. 2013), non-parametric subtractions (Harker et al. 2009; Chapman et al. 2013), and inverse covariance weighting (Liu & Tegmark 2011;…”
ALL-SKY INTERFEROMETRY WITH SPHERICAL HARMONIC TRANSIT TELESCOPES (2013, background): “We assume that the neutral hydrogen fraction takes a value ΩHI = 5× 10−4 (Masui et al. 2013).”
New Limits on 21cm EoR From PAPER-32 Consistent with an X-Ray Heated IGM at z=7.7 (2013, methodology): “We use Monte Carlo simulations (see, e.g., Masui et al. 2013, Paciga et al. 2013, and Switzer et al. 2013) to estimate the expected signal attenuation through the analysis chain from §3.6 onward, as illustrated by the red data-flow path in Figure 2.”
Determination of z ∼ 0.8 neutral hydrogen fluctuations using the 21 cm intensity mapping autocorrelation (2013, methodology): “Following Masui et al. (2013), we c© 2013 RAS, MNRAS000, 1–?? consider a conservativek-range where errors are better estimated (k > 0.12 hMpc−1 to avoid edge effects in the decorrelation operation) and before uncertainties in non-linear structurefo mation become significant (k < 0.3 hMpc−1).”
Cosmology with Phase 1 of the Square Kilometre Array Red Book 2018: Technical specifications and performance forecasts (2018, methodology): “Measurements using the Green Bank Telescope (GBT) produced the first tentative detection of the cosmological HI intensity signal by cross-correlating with the WiggleZ redshift survey (Chang et al. 2010; Switzer et al. 2013; Masui et al. 2013a).”
LATE-TIME COSMOLOGY WITH 21 cm INTENSITY MAPPING EXPERIMENTS (2014, methodology): “Practical experience of foreground subtraction from real data is quite limited so far (see Chang et al. 2010; Masui et al. 2013; Switzer et al. 2013 for some initial attempts), and so we do not have a good picture of how important various aspects of the foreground problem are yet.”