A simulation-calibrated limit on the H i power spectrum from the GMRT Epoch of Reionization experiment

By G. Paciga, J. Albert, K. Bandura, Tzu-Ching Chang, Y. Gupta, C. Hirata, Julia Odegova, Ue-Li Pen, J. Peterson, J. Roy and 3 more. 2013

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The Giant Metrewave Radio Telescope Epoch of Reionization experiment is an ongoing effort to measure the power spectrum from neutral hydrogen at high redshift. We have previously reported an upper limit of (70 mK)^2 at wavenumbers of k ≈ 0.65 h Mpc^(−1) using a basic piecewise-linear foreground subtraction. In this paper, we explore the use of a singular value decomposition to remove foregrounds with fewer assumptions about the foreground structure. Using this method, we also quantify, for the first time, the signal loss due to the foreground filter and present new power spectra adjusted for this loss, providing a revised measurement of a 2σ upper limit at (248 mK)^2 for k = 0.50 h Mpc^(−1). While this revised limit is larger than previously reported, we believe it to be more robust and still represents the best current constraint on reionization at z ≈ 8.6.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/83e240f1daf45da9759ca57085e20abbc4e3de17

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Citations in the corpus

FIRST SEASON MWA EOR POWER SPECTRUM RESULTS AT REDSHIFT 7 (2016, methodology): “…with primary science goals to detect the highly redshift 21cm signal have been built, including the GMRT (Giant Metrewave Radio Telescope, Paciga et al. 2013), LOFAR (LOw Frequency Array29, van Haarlem et al. 2013; Yatawatta et al. 2013), PAPER (Donald C. Backer Precision Array for…”
Upper Limits on the 21 cm Epoch of Reionization Power Spectrum from One Night with LOFAR (2017, methodology): “Paciga et al. (2013) have used the GMRT to set a 2-σ upper limit on the brightness temperature at z = 8.6 of ∆221 < (248 mK) 2 at wave number k ≈ 0.5 h cMpc−1.”
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): “Several efforts have used the 21 cm line to place upper bounds on the reionization era (Bebbington 1986; Bowman & Rogers 2010; Paciga et al. 2013; Pober et al. 2013a) and z ∼ 3 (see, e.g., Subrahmanyan & Anantharamaiah (1990); Wieringa, de Bruyn & Katgert (1992)) without the need to crosscorrelate…”
PAPER-64 CONSTRAINTS ON REIONIZATION: THE 21 cm POWER SPECTRUM AT z = 8.4 (2015, methodology): “…polynomial fitting (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…”
Modeling the Radio Background from the First Black Holes at Cosmic Dawn: Implications for the 21 cm Absorption Amplitude (2018, methodology): “Interferometric experiments seeking to measure the power spectrum include the GMRT (Paciga et al. 2013), the MWA (Dillon et al. 2014; Beardsley et al. 2016; Ewall-Wice et al. 2016; Jacobs et al. 2016; Trott et al. 2016), PAPER (Parsons et al. 2014; Ali et al. 2015; Jacobs et al. 2015), LOFAR (Patil ”
Improved upper limits on the 21 cm signal power spectrum of neutral hydrogen at z ≈ 9.1 from LOFAR (2020, background): “Using the GMRT6, Paciga et al. (2013) reported a 2 − σ upper limit of ∆221 < (248 mK)2 at z = 8.6 and 1 Experiment to Detect the Global Epoch of Reionization Signature, https://loco.lab.asu.edu/edges/ 2 Shaped Antenna measurement of the background RAdio Spectrum, http://www.rri.res.in/DISTORTION/sar”
The Evolution of the Intergalactic Medium (2015, background): “The number of publications quoting upper bounds on the 21 cm power spectrum has been rapidly increasing in recent years (most recently for the GMRT, PAPER, and MWA efforts in Paciga et al. 2013; Ali et al. 2015; Dillon et al. 2015, respectively).”