Field Deployment of Prototype Antenna Tiles for the Mileura Widefield Array Low Frequency Demonstrator

Bowman, Judd D.; Barnes, David G.; Briggs, F.; Corey, B. E.; Lynch, M.; Bhat, N. D. R.; Cappallo, R. J.; Doeleman, Sheperd S.; Fanous, B. J.; Herne, D.; Hewitt, Jacqueline N.; Johnston, Chris; Kasper, J. C.; Kocz, J.; Kratzenberg, E.; Lonsdale, Colin J.; Morales, M. F.; Oberoi, D.; Salah, J. E.; Stansby, Bruce; Stevens, J.; Torr, G.; Wayth, R. B.; Webster, R. L.; Wyithe, J. Stuart B.

doi:10.1086/511068

Cited by 52 publications

(34 citation statements)

References 19 publications

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“…4.2. Detection of the reionization at 21 cm has been an active field in the last decade, and different groups have built instruments to detect a reionization signal around 100 MHz: LOFAR (Rottering et al 2006), MWA (Bowman et al 2007;Lonsdale et al 2009), and PAPER (Parsons et al 2010). Several authors have studied the instrumental noise and statistical uncertainties when measuring the reionization signal power spectrum, and the methods presented here to compute the instrument response and sensitivities are similar to the ones developed in these publications (Morales & Hewitt 2004;Bowman et al 2006;McQuinn et al 2006).…”

Section: Instrument Responsementioning

confidence: 99%

“…An alternative and elegant approach for mapping the matter distribution, which uses neutral atomic hydrogen (H I ) as a tracer with intensity mapping, has been proposed in recent years (Peterson et al 2006;Chang et al 2008). Mapping the matter distribution using H I 21 cm emission as a tracer has been extensively discussed in the literature Tegmark & Zaldarriaga 2009) and is being used in projects such as LOFAR (Rottering et al 2006) or MWA (Bowman et al 2007) to observe reionization at redshifts z ∼ 10.…”

Section: Introductionmentioning

confidence: 99%

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21 cm observation of large-scale structures atz ~ 1

Ansari

Campagne

Colom

et al. 2012

A&A

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Context. Large-scale structures (LSS) in the universe can be traced using the neutral atomic hydrogen H I through its 21 cm emission. Such a 3D matter distribution map can be used to test the cosmological model and to constrain the dark energy properties or its equation of state. A novel approach, called intensity mapping, can be used to map the H I distribution, using radio interferometers with a large instantaneous field of view and waveband. Aims. We study the sensitivity of different radio interferometer configurations, or multi-beam instruments for observing LSS and baryon acoustic oscillations (BAO) in 21 cm, and we discuss the problem of foreground removal. Methods. For each configuration, we determined instrument response by computing the (u, v) or Fourier angular frequency plane coverage using visibilities. The (u, v) plane response determines the noise power spectrum, hence the instrument sensitivity for LSS P(k) measurement. We also describe a simple foreground subtraction method of separating LSS 21 cm signal from the foreground due to the galactic synchrotron and radio source emission. Results. We have computed the noise power spectrum for different instrument configurations, as well as the extracted LSS power spectrum, after separating the 21 cm-LSS signal from the foregrounds. We have also obtained the uncertainties on the dark energy parameters for an optimized 21 cm BAO survey. Conclusions. We show that a radio instrument with few hundred simultaneous beams and a collecting area of ∼10 000 m 2 will be able to detect BAO signal at redshift z ∼ 1 and will be competitive with optical surveys.

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Section: Instrument Responsementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

21 cm observation of large-scale structures atz ~ 1

Ansari

Campagne

Colom

et al. 2012

A&A

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“…The shire of Murchison has a quiet radio environment, making it an excellent site for this and other radio facilities [1]. Each of the 512 antennas will be a 4 × 4 tile of dipoles.…”

Section: Introductionmentioning

confidence: 99%

“…For large fields this is not the case, but the problem can still be reduced to 2D transforms (a good overview is given in [6]). 1 Post processing typically involves calibrating the visibilities, gridding them onto the uv-plane to form a regularly sampled interference pattern, and then applying a 2D FFT to form an image. Techniques such as self-calibration can then be used in an attempt to improve the calibration by iterating back and forth between the visibilities and the image.…”

Section: Introductionmentioning

confidence: 99%

Real-Time Calibration of the Murchison Widefield Array

Mitchell

Greenhill

Wayth

et al. 2008

IEEE J. Sel. Top. Signal Process.

206

266

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Abstract-The interferometric technique known as peeling addresses many of the challenges faced when observing with low-frequency radio arrays, and is a promising tool for the associated calibration systems. We investigate a real-time peeling implementation for next-generation radio interferometers such as the Murchison Widefield Array (MWA). The MWA is being built in Australia and will observe the radio sky between 80 and 300 MHz. The data rate produced by the correlator is just over 19 GB/s (a few Peta-Bytes/day). It is impractical to store data generated at this rate, and software is currently being developed to calibrate and form images in real time. The software will run on-site on a high-throughput real-time computing cluster at several tera-flops, and a complete cycle of calibration and imaging will be completed every 8 seconds. Various properties of the implementation are investigated using simulated data. The algorithm is seen to work in the presence of strong galactic emission and with various ionospheric conditions. It is also shown to scale well as the number of antennas increases, which is essential for many upcoming instruments. Lessons from MWA pipeline development and processing of simulated data may be applied to future low-frequency fixed dipole arrays.

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“…A new generation of radio telescopes will search for transient pulses from the universe [1,2,3,4,5]. Such searches, using pre-existing data, have recently found surprising pulses of galactic and extragalactic origin [6,7,8].…”

Section: Introductionmentioning

confidence: 99%

Transient pulses from exploding primordial black holes as a signature of an extra dimension

Kavic

Simonetti

Cutchin

et al. 2008

J. Cosmol. Astropart. Phys.

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An evaporating black hole in the presence of an extra spatial dimension would undergo an explosive phase of evaporation. We show that such an event, involving a primordial black hole, can produce a detectable, distinguishable electromagnetic pulse, signaling the existence of an extra dimension of size L ∼ 10 −18 − 10 −20 m. We derive a generic relationship between the Lorentz factor of a pulse-producing "fireball" and the TeV energy scale. For an ordinary toroidally compactified extra dimension, transient radio-pulse searches probe the electroweak energy scale (∼0.1 TeV), enabling comparison with the Large Hadron Collider.

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Field Deployment of Prototype Antenna Tiles for the Mileura Widefield Array Low Frequency Demonstrator

Cited by 52 publications

References 19 publications

21 cm observation of large-scale structures atz ~ 1

21 cm observation of large-scale structures atz ~ 1

Real-Time Calibration of the Murchison Widefield Array

Transient pulses from exploding primordial black holes as a signature of an extra dimension

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