Publisher’s Note: Search for ultrahigh energy neutrinos in highly inclined events at the Pierre Auger Observatory [Phys. Rev. D<b>84</b>, 122005 (2011)]

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doi:10.1103/physrevd.85.029902

Cited by 19 publications

(37 citation statements)

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“…Moreover, the X max distribution is narrower for heavier primary particles. This relation can be used to statistically distinguish mass groups of nuclei, as well as to search for photons [343], or neutrinos [344,345], because for inclined showers only weakly interacting neutrinos have a reasonable probability to interact deep in the atmosphere causing a shower maximum relatively close to the detector.…”

Section: Shower Maximum: X Maxmentioning

confidence: 99%

Radio detection of cosmic-ray air showers and high-energy neutrinos

Schröder

2017

Progress in Particle and Nuclear Physics

175

129

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In the last fifteen years radio detection made it back to the list of promising techniques for extensive air showers, firstly, due to the installation and successful operation of digital radio experiments and, secondly, due to the quantitative understanding of the radio emission from atmospheric particle cascades. The radio technique has an energy threshold of about 100 PeV, which coincides with the energy at which a transition from the highest-energy galactic sources to the even more energetic extragalactic cosmic rays is assumed. Thus, radio detectors are particularly useful to study the highest-energy galactic particles and ultra-high-energy extragalactic particles of all types. Recent measurements by various antenna arrays like LOPES, CODALEMA, AERA, LOFAR, Tunka-Rex, and others have shown that radio measurements can compete in precision with other established techniques, in particular for the arrival direction, the energy, and the position of the shower maximum, which is one of the best estimators for the composition of the primary cosmic rays. The scientific potential of the radio technique seems to be maximum in combination with particle detectors, because this combination of complementary detectors can significantly increase the total accuracy for air-shower measurements. This increase in accuracy is crucial for a better separation of different primary particles, like gamma-ray photons, neutrinos, or different types of nuclei, because showers initiated by these particles differ in average depth of the shower maximum and in the ratio between the amplitude of the radio signal and the number of muons. In addition to air-shower measurements, the radio technique can be used to measure particle cascades in dense media, which is a promising technique for detection of ultra-high-energy neutrinos. Several pioneering experiments like ARA, ARIANNA, and ANITA are currently searching for the radio emission by neutrino-induced particle cascades in ice. In the next years these two sub-fields of radio detection of cascades in air and in dense media will likely merge, because several future projects aim at the simultaneous detection of both, high-energy cosmic-rays and neutrinos. SKA will search for neutrino and cosmic-ray initiated cascades in the lunar regolith and simultaneously provide unprecedented detail for air-shower measurements. Moreover, detectors with huge exposure like GRAND, SWORD or EVA are being considered to study the highest energy cosmic rays and neutrinos. This review provides an introduction to the physics of radio emission by particle cascades, an overview on the various experiments and their instrumental properties, and a summary of methods for reconstructing the most important air-shower properties from radio measurements. Finally, potential applications of the radio technique in high-energy astroparticle physics are discussed.

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Section: Shower Maximum: X Maxmentioning

confidence: 99%

Radio detection of cosmic-ray air showers and high-energy neutrinos

Schröder

2017

Progress in Particle and Nuclear Physics

175

129

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“…where E GW (E ν , δ) is the effective exposure to a pointlike flux of UHE neutrinos as a function of neutrino energy E ν and declination. For each channel ES and DGH we calculate the exposure to UHE neutrinos E ES (E ν , δ) and E DGH (E ν , δ), respectively, following the procedure explained in [21][22][23][24][25]. The exposure is obtained by integrating the SD aperture (area × solid angle) over the search period T search , multiplied by the neutrino cross section for each neutrino channel, and weighted by the selection and detection efficiency obtained from Monte Carlo simulations [21].…”

Section: B Constraints On the Sources Of Gwmentioning

confidence: 99%

“…In previous publications [21][22][23][24] methods were established to identify inclined and deeply-initiated showers with the SD of the Pierre Auger Observatory. These were applied blindly to search for ES and DGH neutrinos in the data collected with the SD up to 20 June 2013.…”

Section: Introductionmentioning

confidence: 99%

Ultrahigh-energy neutrino follow-up of gravitational wave events GW150914 and GW151226 with the Pierre Auger Observatory

Aab¹,

Abreu²,

Aglietta³

et al. 2016

Phys. Rev. D

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On September 14, 2015 the Advanced LIGO detectors observed their first gravitational-wave (GW) transient GW150914. This was followed by a second GW event observed on December 26, 2015. Both events were inferred to have arisen from the merger of black holes in binary systems. Such a system may emit neutrinos if there are magnetic fields and disk debris remaining from the formation of the two black holes. With the surface detector array of the Pierre Auger Observatory we can search for neutrinos with energy Eν above 100 PeV from point-like sources across the sky with equatorial declination from about −65• to +60• , and in particular from a fraction of the 90% confidence-level (CL) inferred positions in the sky of GW150914 and GW151226. A targeted search for highly-inclined extensive air showers, produced either by interactions of downward-going 4 neutrinos of all flavors in the atmosphere or by the decays of tau leptons originating from tauneutrino interactions in the Earth's crust (Earth-skimming neutrinos), yielded no candidates in the Auger data collected within ±500 s around or 1 day after the coordinated universal time (UTC) of GW150914 and GW151226, as well as in the same search periods relative to the UTC time of the GW candidate event LVT151012. From the non-observation we constrain the amount of energy radiated in ultrahigh-energy neutrinos from such remarkable events.PACS numbers: 95.55. Vj, 95.85.Ry, 98.70.Sa

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“…The relative mass apertures as functions of the neutrino energy where calculated using data from Table I of ref. [10]. 4 Note that i=e,µ,τ m i CC + 3m NC + m mount = 1.…”

Section: Expected Number Of Neutrino Events At the Paomentioning

confidence: 99%

Warped extra dimension and inclined events at Pierre Auger Observatory

Kisselev

Shkalina

2016

EPJ Web Conf.

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Abstract. The generalized solution for the warp factor of the Randall-Sundrum metric is presented which is symmetric with respect to both branes and explicitly periodic in extra variable. Given that the curvature of the 5-dimensional space-time is small, the expected rate of neutrino-induced inclined events at the Surface Detector of the Pierre Auger Observatory is calculated. Both the "downward-going" (DG) and "Earth-skimming" (ES) neutrinos are considered. By comparing the expected event rate with the recent Auger data on searching for neutrino candidates, the lower bound on the fundamental gravity scale M 5 is obtained. The ratio of the number of the ES air showers to the number of the DG showers is estimated as a function of M 5 .

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Publisher’s Note: Search for ultrahigh energy neutrinos in highly inclined events at the Pierre Auger Observatory [Phys. Rev. D84, 122005 (2011)]

Cited by 19 publications

References 0 publications

Radio detection of cosmic-ray air showers and high-energy neutrinos

Radio detection of cosmic-ray air showers and high-energy neutrinos

Ultrahigh-energy neutrino follow-up of gravitational wave events GW150914 and GW151226 with the Pierre Auger Observatory

Warped extra dimension and inclined events at Pierre Auger Observatory

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