Constraints on the diffuse high-energy neutrino flux from the third flight of ANITA

Gorham, P. W.; Allison, P.; Banerjee, O.; Batten, L.; Beatty, J. J.; Bechtol, K.; Belov, K.; Besson, D.; Binns, W. R.; Bugaev, V.; Cao, Pinlu; Chen, C. C.; Chen, C. H.; Chen, P.; Clem, J.; Connolly, A.; Cremonesi, L.; Dailey, B.; Deaconu, C.; Dowkontt, P. F.; Fox, B. D.; Gordon, J.; Hast, C.; Hill, B.; Hsu, Shih-Ying; Huang, J. J.; Hughes, K.; Hupe, R.; Israel, M. H.; Liewer, K. M.; Liu, T. C.; Ludwig, Andrew; Macchiarulo, L.; Matsuno, S.; Miki, C.; Mulrey, K.; Nam, J. W.; Naudet, C. J.; Nichol, R. J.; Novikov, Alexander; Oberla, E.; Prohira, S.; Rauch, B. F.; Roberts, Jason; Romero-Wolf, A.; Rotter, B.; Russell, John Wellesley; Saltzberg, D.; Seckel, D.; Schoorlemmer, H.; Shiao, Judith Shu-Chu; Stafford, S.; Stockham, J.; Stockham, M.; Strutt, B.; Sutherland, M.; Varner, G.; Vieregg, A. G.; Wang, S. H.; Wissel, S.

doi:10.1103/physrevd.98.022001

Cited by 87 publications

(111 citation statements)

References 28 publications

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“…IceCube has detected an astrophysical neutrino flux in the ∼ 50 TeV to ∼ 10 PeV energy range [32]. Bounds on neutrinos beyond ∼ 10 PeV energies, hereafter extremely-high energy (EHE) cosmic neutrinos, are provided by the Ice-Cube [33], Auger [34], and ANITA [35,36] experiments. IceCube's latest bound from 9 years of observation provides the strongest constraint in the ∼ 10 PeV to ∼ 10 EeV energy range, while the combined bound from four ANITA balloon flights provides the strongest constraint above ∼ 10 EeV.…”

Section: Multimessenger Datamentioning

confidence: 99%

Progress towards characterizing ultrahigh energy cosmic ray sources

2019

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We use a multimessenger approach to constrain realistic mixed composition models of ultrahigh energy cosmic ray sources using the latest cosmic ray, neutrino, and gamma-ray data. We build on the successful Unger-Farrar-Anchordoqui 2015 (UFA15) model which explains the shape of the spectrum and its complex composition evolution via photodisintegration of accelerated nuclei in the photon field surrounding the source. We explore the constraints which can currently be placed on the redshift evolution of sources and the temperature of the photon field surrounding the sources. We show that a good fit is obtained to all data either with a source which accelerates a narrow range of nuclear masses or a Milky Way-like mix of nuclear compositions, but in the latter case the nearest source should be 30-50 Mpc away from the Milky Way in order to fit observations from the Pierre Auger Observatory. We also ask whether the data allow for a subdominant purely protonic component at UHE in addition to the primary UFA15 mixed composition component. We find that such a two-component model can significantly improve the fit to cosmic ray data while being compatible with current multimessenger data.

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Section: Multimessenger Datamentioning

confidence: 99%

Progress towards characterizing ultrahigh energy cosmic ray sources

2019

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“…for Earth-skimming neutrinos, where the probability of detecting a tau in the atmosphere after a single neutrino interaction in the Earth is optimized [20][21][22][23][24][25][26][27][28]. Here, we show how using the secondary flux will extend this search to the entire sky.…”

Section: Cosmogenic Fluxmentioning

confidence: 93%

“…Similarly, neutrino detectors sensitive to higher energies compared to IceCube have typically limited searches to Earth-skimming or downgoing trajectories, where the column depth is optimal for detecting EHE neutrinos after a single interaction [20]. Experiments such as ANITA, ARA, ARIANNA, and the Pierre Auger Observatory have set limits on the cosmogenic flux taking advantage of the Earth-skimming technique [21][22][23][24][25][26][27][28].…”

Section: Introductionmentioning

confidence: 99%

Observing EeV neutrinos through Earth: GZK and the anomalous ANITA events

Safa

Pizzuto

Argüelles

et al. 2020

J. Cosmol. Astropart. Phys.

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Tau neutrinos are unique cosmic messengers, especially at extreme energies. When they undergo a charged-current interaction, the short lifetime of the produced tau gives rise to secondary tau neutrinos that carry a significant fraction of the primary neutrino energy. This effect, known as tau neutrino regeneration, has not been applied to its full potential in current generation neutrino experiments. In this work, we present an updated calculation of tau neutrino regeneration, and explore its implications for two scenarios: the recent anomalous ANITA events and the cosmogenic neutrino flux. For the former, we investigate the idea of localized emission and find that the maximum secondary neutrino flux allowed by IceCube measurements implies a primary flux that is incompatible with the ANITA observation, regardless of the assumed source energy spectrum. For the latter, we study the prospect of detecting the cosmogenic neutrino flux of regenerated PeV neutrinos with current and next generation neutrino detectors.

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“…It can be seen that the ES channel dominates the exposure, compensating for the small solid angle and the disadvantage of being sensitive to only one neutrino flavor. The reason is mainly that the interaction probability of the τ neutrino is much Corresponding limits from ANITA [11,12,13] and Ice-Cube [14] as well as predictions for several neutrino models (cosmogenic [15,5], astrophysical [16,17,18].) higher inside the Earth than in the atmosphere as it is proportional to the transversed matter depth.…”

Section: Limits On the Diffuse Flux Of Uhe Neutrinos And On Point-likmentioning

confidence: 96%

Ultra-high energy neutrino searches and GW follow-up with the Pierre Auger Observatory

Schimp

2019

Nuclear and Particle Physics Proceedings

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The surface detector array (SD) of the Pierre Auger Observatory is sensitive to neutrinos at energies in the 100 PeV to 100 EeV range. This sensitivity, together with its large acceptance, makes it a complementary detector to other neutrino telescopes, which have their peak sensitivities at lower energies. The neutrino-induced air showers that the SD of the Pierre Auger Observatory is sensitive to can be divided into those induced by interactions of neutrinos of any flavor deep in the atmosphere, and those induced by charged-current interactions of tau neutrinos in the Earth's crust. Both of these types can be efficiently distinguished from cosmic ray-induced air showers, provided that their zenith angles are larger than 60 • . As no neutrino candidates were found in the performed searches, we present limits on the diffuse all-flavor neutrino flux. Using these limits, we obtained constraints on cosmic-ray and neutrino production models. In the light of the recent observations of gravitational waves (GW), we also present the follow-up of LIGO/Virgo GW events. These include binary black hole merger events and also GW170817, the only binary neutron star merger ever observed directly.

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Constraints on the diffuse high-energy neutrino flux from the third flight of ANITA

Cited by 87 publications

References 28 publications

Progress towards characterizing ultrahigh energy cosmic ray sources

Progress towards characterizing ultrahigh energy cosmic ray sources

Observing EeV neutrinos through Earth: GZK and the anomalous ANITA events

Ultra-high energy neutrino searches and GW follow-up with the Pierre Auger Observatory

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