Experimental Study of Acoustic Ultra–High‐Energy Neutrino Detection

Vandenbroucke, J.; Gratta, G.; Lehtinen, N. G.

doi:10.1086/425336

Cited by 76 publications

(62 citation statements)

References 28 publications

(41 reference statements)

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“…This is in contrast with most deep ocean sites, where refraction due to a vertical sound speed gradient is a significant challenge for acoustic neutrino detection [12].…”

Section: Implications For Neutrino Astronomymentioning

confidence: 86%

“…The neutrino-induced signal amplitude is larger in ice than in water due to its favorable elastic and thermal properties. Furthermore, we have determined the background noise to be very stable in South Pole ice [11], in contrast to ocean water where it is highly variable on multiple time scales, resulting in the necessity of sophisticated trigger algorithms [12], [13].…”

Section: Introductionmentioning

confidence: 99%

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Measurement of sound speed vs. depth in South Pole ice for neutrino astronomy

Abbasi

Abdou

Ackermann³

et al. 2010

Astroparticle Physics

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We have measured the speed of both pressure waves and shear waves as a function of depth between 80 and 500 m depth in South Pole ice with better than 1% precision. The measurements were made using the South Pole Acoustic Test Setup (SPATS), an array of transmitters and sensors deployed in the ice at South Pole Station in order to measure the acoustic properties relevant to acoustic detection of astrophysical neutrinos. The transmitters and sensors use piezoceramics operating at ∼5-25 kHz. Between 200 m and 500 m depth, the measured profile is consistent with zero variation of the sound speed with depth, resulting in zero refraction, for both pressure and shear waves. We also performed a complementary study featuring an explosive signal propagating from 50 to 2250 m depth, from which we determined a value for the pressure wave speed consistent with that determined with the sensors operating at shallower depths and higher frequencies. These results have encouraging implications for neutrino astronomy: The negligible refraction of acoustic waves deeper than 200 m indicates that good neutrino direction and energy reconstruction, as well as separation from background events, could be achieved.

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“…This is in contrast with most deep ocean sites, where refraction due to a vertical sound speed gradient is a significant challenge for acoustic neutrino detection [12].…”

Section: Implications For Neutrino Astronomymentioning

confidence: 86%

Section: Introductionmentioning

confidence: 99%

Measurement of sound speed vs. depth in South Pole ice for neutrino astronomy

Abbasi

Abdou

Ackermann³

et al. 2010

Astroparticle Physics

Self Cite

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show abstract

“…14(b) was calculated following the approach used for the first acoustic neutrino limit estimate [11]. The neutrinos were assumed to be down-going and to be uniformly distributed on a 2π half sphere.…”

Section: Estimated Neutrino Flux Limitmentioning

confidence: 99%

Background studies for acoustic neutrino detection at the South Pole

Abbasi

Abdou

Abu‐Zayyad

et al. 2012

Astroparticle Physics

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The detection of acoustic signals from ultra-high energy neutrino interactions is a promising method to measure the flux of cosmogenic neutrinos expected on Earth. The energy threshold for this process depends strongly on the absolute noise level in the target material. The South Pole Acoustic Test Setup (SPATS), deployed in the upper part of four boreholes of the IceCube Neutrino Observatory, has monitored the noise in Antarctic ice at the geographic South Pole for more than two years down to 500 m depth. The noise is very stable and Gaussian distributed. Lacking an in-situ calibration up to now, laboratory measurements have been used to estimate the absolute noise level in the 10 to 50 kHz frequency range to be smaller than 20 mPa. Using a threshold trigger, sensors of the South Pole Acoustic Test Setup registered acoustic events in the IceCube detector volume and its vicinity. Acoustic signals from refreezing IceCube holes and from anthropogenic sources have been used to test the localization of acoustic events. An upper limit on the neutrino flux at energies E ν > 10 11 GeV is derived from acoustic data taken over eight months.

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“…Within the ANTARES and NEMO collaborations, these activities were in parts driven also by the know-how gained in the use of (commercial) acoustic positioning systems [13] that are necessary to accurately determine the positions of the detector elements varying in the underwater currents. In addition to the setups in Cherenkov experiments, there are projects using existing military underwater acoustic arrays: SADCO [14], SAUND [15] and ACORNE [16]. A lot of experience was gained with all these setups which have mostly been used for fundamental feasibility studies.…”

Section: Introductionmentioning

confidence: 99%

Acoustic neutrino detection in sea water: Technical aspects

Graf¹

2013

AIP Conference Proceedings

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Abstract. The acoustic neutrino detection technique is a promising approach for future large-scale detectors with the aim of measuring the small expected flux of ultra-high-energy cosmogenic neutrinos. This article focuses on the technical aspects of the application of this technique in water. Though the technique is intriguingly simple, challenges arise from e.g. anisotropic sound propagation, ambient noise or transient background in a natural environment. We present major technical aspects of acoustic neutrino detection based on experience gained with different acoustic test arrays. Before aiming for a largescale acoustic or hybrid (opto-acoustic) detector, the acoustic detection technique needs to be investigated further in the next generation of Cherenkov neutrino telescopes that are currently prepared. We discuss the technical implementation into those large optical detectors, primarily focussing on the KM3NeT project.

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Experimental Study of Acoustic Ultra–High‐Energy Neutrino Detection

Cited by 76 publications

References 28 publications

Measurement of sound speed vs. depth in South Pole ice for neutrino astronomy

Measurement of sound speed vs. depth in South Pole ice for neutrino astronomy

Background studies for acoustic neutrino detection at the South Pole

Acoustic neutrino detection in sea water: Technical aspects

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