Probing the first stars and black holes in the early Universe with the Dark Ages Radio Explorer (DARE)

Burns, Jack O.; Lazio, Joseph; Bale, S. D.; Bowman, Judd D.; Bradley, Richard F.; Carilli, C. L.; Furlanetto, Steve R.; Harker, G.; Loeb, Abraham; Pritchard, Jonathan R.

doi:10.1016/j.asr.2011.10.014

Cited by 127 publications

(127 citation statements)

References 43 publications

(43 reference statements)

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“…So-called "global" experiments such as EDGES (Bowman & Rogers 2010), the LWA (Ellingson et al 2013), LEDA (Greenhill & Bernardi 2012;Bernardi et al 2015), DARE (Burns et al 2012), SciHi (Voytek et al 2014), BigHorns (Sokolowski et al 2015), and SARAS (Patra et al 2015) seek to measure the mean brightness temperature of 21 cm relative to the CMB background. These experiments typically rely on auto-correlations from a small number of dipole elements to access the sky-averaged 21 cm signal, although recent work is showing that interferometric cross-correlations may also be used to access the signal (Vedantham et al 2015;Presley et al 2015).…”

Section: Introductionmentioning

confidence: 99%

PAPER-64 CONSTRAINTS ON REIONIZATION: THE 21 cm POWER SPECTRUM ATz= 8.4

Ali

Parsons

Zheng

et al. 2015

ApJ

265

224

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In this paper, we report new limits on 21 cm emission from cosmic reionization based on a 135 day observing campaign with a 64-element deployment of the Donald C. Backer Precision Array for Probing the Epoch of Reionization in South Africa. This work extends the work presented in Parsons et al. with more collecting area, a longer observing period, improved redundancy-based calibration, improved fringe-rate filtering, and updated power-spectral analysis using optimal quadratic estimators. The result is a new 2σ upper limit on Δ 2 (k) of (22.4 mK) 2 in the range k h 0.15 0.5 Mpc 1 < < -at z = 8.4. This represents a three-fold improvement over the previous best upper limit. As we discuss in more depth in a forthcoming paper, this upper limit supports and extends previous evidence against extremely cold reionization scenarios. We conclude with a discussion of implications for future 21 cm reionization experiments, including the newly funded Hydrogen Epoch of Reionization Array.

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Section: Introductionmentioning

confidence: 99%

PAPER-64 CONSTRAINTS ON REIONIZATION: THE 21 cm POWER SPECTRUM ATz= 8.4

Ali

Parsons

Zheng

et al. 2015

ApJ

265

224

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“…This approach is being pursued by the Experiment to Detect the Global EoR Signature (EDGES; Bernardi, McQuinn, & Greenhill 2015), Shaped Antenna measurement of background Radio Spectrum (SARAS Patra et al 2013;Singh et al 2015), and the Dark Ages Radio Explorer (DARE; Burns et al 2012). Both methods require careful and accurate subtraction of the sky foreground since the 21 cm signal is three to five orders of magnitude below the foreground.…”

Section: Introductionmentioning

confidence: 99%

Improved measurement of the spectral index of the diffuse radio background between 90 and 190 MHz

Mozdzen¹,

Bowman²,

Monsalve³

et al. 2016

Mon. Not. R. Astron. Soc.

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We report absolutely calibrated measurements of diffuse radio emission between 90 and 190 MHz from the Experiment to Detect the Global EoR Signature (EDGES). EDGES employs a wide beam zenith-pointing dipole antenna centred on a declination of −26.7 • . We measure the sky brightness temperature as a function of frequency averaged over the EDGES beam from 211 nights of data acquired from July 2015 to March 2016. We derive the spectral index, β, as a function of local sidereal time (LST) and find −2.60 > β > − 2.62 ±0.02 between 0 and 12 h LST. When the Galactic Centre is in the sky, the spectral index flattens, reaching β = −2.50 ±0.02 at 17.7 h. The EDGES instrument is shown to be very stable throughout the observations with night-to-night reproducibility of σ β < 0.003. Including systematic uncertainty, the overall uncertainty of β is 0.02 across all LST bins. These results improve on the earlier findings of by reducing the spectral index uncertainty from 0.10 to 0.02 while considering more extensive sources of errors. We compare our measurements with spectral index simulations derived from the Global Sky Model (GSM) of de Oliveira-Costa et al. (2008) and with fits between the Guzmán et al. (2011) 45 MHz andHaslam et al. (1982) 408 MHz maps. We find good agreement at the transit of the Galactic Centre. Away from transit, the GSM tends to over-predict (GSM less negative) by 0.05 < ∆ β = β GSM − β EDGES < 0.12, while the 45-408 MHz fits tend to over-predict by ∆ β < 0.05.

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“…Mapping experiments include PAPER (Pober et al 2013;Parsons et al 2013), GMRT-EoR (Paciga et al 2011), LOFAR (van Haarlem et al 2013), MWA (Bernardi et al 2013), and the proposed Hydrogen Epoch of Reionization Array (HERA) (2010) and Square Kilometer Array (SKA) (2013). All-sky experiments include EDGES (Bowman et al 2008), Large-Aperture Experiment to detect the Dark Ages (LEDA) (2013) and the proposed Dark Ages Radio Explorer (DARE) (Burns et al 2012).…”

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confidence: 99%