First constraints on the ultra-high energy neutrino flux from a prototype station of the Askaryan Radio Array

Allison, P.; Auffenberg, J.; Bard, Robert L.; Beatty, J. J.; Besson, D.; Bora, C.; Chen, C.-C.; Chen, P.; Connolly, A.; Davies, J.; DuVernois, Michael; Fox, B. D.; Gorham, P. W.; Hanson, K.; Hill, B.; Hoffman, K. D.; Hong, Eugene; Hu, Lei; Ishihara, A.; Karle, A.; Kelley, J. L.; Kravchenko, I.; Landsman, H.; Laundrie, A.; Li, C.-J.; Liu, T.; Lu, M.-Y.; Maunu, R.; Mase, K.; Meures, T.; Miki, C.; Nam, J. W.; Nichol, R. J.; Nir, G.; O’Murchadha, A.; Pfendner, C.; Ratzlaff, K.; Richman, M.; Rotter, B.; Sandstrom, P.; Seckel, D.; Shultz, A.; Stockham, J.; Stockham, M.; Sullivan, M.; Touart, J.; Tu, Huitzu; Varner, G.; Yoshida, Shigeru; Young, R.

doi:10.1016/j.astropartphys.2015.04.006

Cited by 70 publications

(108 citation statements)

References 38 publications

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“…Figure 3: The ARA 2 station neutrino limit for 7.5 months of operation compared to other detector limits and flux expectations. The projection for the ARA37 sensitivity is calculated at trigger level without accounting for systematic errors [9,10,13,14,12,15,16,17,18].…”

Section: Latest Data Analysis Results From Two Ara Stationsmentioning

confidence: 99%

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First results from two deep Askaryan Radio Array stations

Meures¹

2017

Proceedings of 38th International Conference on High Energy Physics — PoS(ICHEP2016)

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The Askaryan Radio Arrray (ARA) is a planned and in parts constructed detector for ultra-high energy neutrinos, utilizing radio emission from neutrino induced particle showers. With this detection method, ARA will be able to employ several gigatons of South-Pole ice as a detector medium needed to efficiently discover neutrinos with energies above 10 PeV. These neutrinos carry particularly interesting information about highest energy processes in the far universe. The detector is planned to consist of 37 widely-separated antenna clusters, so-called stations. Currently, 3 stations are deployed in the ice recording transient radio waves, with two more stations assembled for deployment in the austral summer 2017/2018. In this presentation, first analysis results from data recorded by two ARA stations in the year 2013 are summarized.

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Section: Latest Data Analysis Results From Two Ara Stationsmentioning

confidence: 99%

“…Currently, 3 ARA stations and a prototype are deployed at the South Pole. The prototype station, called Testbed, has been used to determine ice properties for radio measurements and for an initial neutrino search, described in [10]. It was decommissioned in 2013.…”

Section: The Detectormentioning

confidence: 99%

First results from two deep Askaryan Radio Array stations

Meures¹

2017

Proceedings of 38th International Conference on High Energy Physics — PoS(ICHEP2016)

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“…Three such repeating locations were identified and geometric cuts were designed to reject events from these locations. Descriptions of further cuts can be found in [8]. After a number of quality cuts, the effective livetime drops to 224 days.…”

Section: Pos(icrc2015)1105mentioning

confidence: 99%

“…This analysis only examines data from March to August 2011. A complete description of these analyses can be found in [8].…”

Section: Testbed Data Analysesmentioning

confidence: 99%

First cosmogenic neutrino limits from the ARA Testbed station at South Pole

Besson¹,

Connolly²,

Davies³

et al. 2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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The Askaryan Radio Array (ARA) is an ultra-high energy (UHE) cosmic neutrino detector located at the South Pole. The cosmic ray flux cut off above primary energies of 10 19.5 eV leads us to expect a UHE neutrino flux due to the Greisen-Zatsepin-Kuzmin (GZK) effect. The detection of these UHE cosmic neutrinos will add to the understanding of the sources and physics of UHE cosmic rays. The radio Cherenkov technique is the most promising technique for a long term program to investigate the UHE cosmic neutrino flux. ARA uses this radio Cherenkov technique by deploying radio frequency antennas at a depth of 200m in the Antarctic ice. A prototype ARA TestBed station was deployed in the 2010-2011 season and the first three ARA stations were deployed in the 2011-2012 and 2012-2013 seasons. We present the results of the first neutrino search with ARA, using data taken from 2011-2012 with the ARA TestBed station.

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“…Such emission has been measured and characterized at beam-line experiments [4,5,6]. This technique has been exploited by several experiments in Antarctica, including ANITA [7], ARA [8], and ARIANNA [9]. These experiments have thresholds > 50 PeV, however, recent studies have shown improved sensitivity to the PeV energy scale using phased arrays of antennas [10,11], which would complement studies of the few-PeV astrophysical neutrino signal discovered by IceCube [12].…”

Section: Introductionmentioning

confidence: 99%

Site Characterization and Detector Development for the Greenland Neutrino Observatory

Wissel¹,

Avva²,

Bechtol³

et al. 2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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The PeV neutrinos discovered by IceCube are of astrophysical origin, and their progenitors could be any of several source classes, including active galactic nuclei, gamma-ray bursts, or pulsars. Such high-energy accelerators would produce neutrinos up to hundreds of PeV, which motivates the development of neutrino telescopes with the sensitivity, energy resolution, and pointing resolution required to distinguish among models of the IceCube neutrinos as well as cosmogenic neutrinos. Radio detection of Askaryan radiation from neutrino showers in ice is well-suited to the detection of the highest energy neutrinos, with degree-scale pointing resolution and the ability to build sparse arrays, but the energy threshold of current experiments is currently set by the temperature of the ice. The uncorrelated thermal noise can be reduced by combining the signals from several antennas in a phased array. We report here on a June 2015 trip to Summit Station In Greenland for testing a phased array of dipoles, as well as the sensitivity of the array and background measurements of the site and discuss prospects for the Greenland Neutrino Observatory (GNO).

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First constraints on the ultra-high energy neutrino flux from a prototype station of the Askaryan Radio Array

Cited by 70 publications

References 38 publications

First results from two deep Askaryan Radio Array stations

First results from two deep Askaryan Radio Array stations

First cosmogenic neutrino limits from the ARA Testbed station at South Pole

Site Characterization and Detector Development for the Greenland Neutrino Observatory

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