Analysis of the 4-year IceCube high-energy starting events

Vincent, Aaron C.; Palomares‐Ruiz, Sergio; Mena, Olga

doi:10.1103/physrevd.94.023009

Cited by 72 publications

(113 citation statements)

References 195 publications

(253 reference statements)

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“…As a result of flavor oscillation, ν e : ν µ : ν τ = 1:1:1 on Earth, assuming the standard full pion decay chain of neutrino production [21,44,45]. This is compatible with TeV-PeV flavor ratio measurements [46][47][48][49]. The neutrino distributions are summed over the three flavors.…”

Section: +0023mentioning

confidence: 53%

Constraints on Ultrahigh-Energy Cosmic-Ray Sources from a Search for Neutrinos above 10 PeV with IceCube

Aartsen¹,

Abraham²,

Ackermann³

et al. 2016

Phys. Rev. Lett.

143

129

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We report constraints on the sources of ultra-high-energy cosmic rays (UHECRs) above 10 9 GeV, based on an analysis of seven years of IceCube data. This analysis efficiently selects very high energy neutrino-induced events which have deposited energies from 5 × 10 5 GeV to above 10 11 GeV. Two neutrino-induced events with an estimated deposited energy of (2.6 ± 0.3) × 10 6 GeV, the highest neutrino energy observed so far, and (7.7 ± 2.0) × 10 5 GeV were detected. The atmospheric background-only hypothesis of detecting these events is rejected at 3.6σ. The hypothesis that the observed events are of cosmogenic origin is also rejected at >99% CL because of the limited deposited energy and the non-observation of events at higher energy, while their observation is consistent with an astrophysical origin. Our limits on cosmogenic neutrino fluxes disfavor the UHECR sources 3 having cosmological evolution stronger than the star formation rate, e.g., active galactic nuclei and γ-ray bursts, assuming proton-dominated UHECRs. Constraints on UHECR sources including mixed and heavy UHECR compositions are obtained for models of neutrino production within UHECR sources. Our limit disfavors a significant part of parameter space for active galactic nuclei and new-born pulsar models. These limits on the ultra-high-energy neutrino flux models are the most stringent to date. Introduction -The sources of ultra-high-energy cosmic rays (UHECRs; cosmic-ray energy E CR 10 18 eV) remain unidentified [1]. The majority of the candidate objects are extra-Galactic, such as Active Galactic Nuclei (AGN) [2-6] , γ-ray bursts [7][8][9][10][11][12][13], and starburst galaxies [14][15][16][17][18][19]. UHECR interactions with ambient photons and matter at sources generate astrophysical neutrinos with 5% of the parent UHECR energy, on average [20][21][22]. Thus, a substantial fraction of these Extremely High-Energy (EHE) astrophysical neutrinos is expected to have an energy above 10 7 GeV. Moreover, neutrinos with energies above ∼107 GeV are expected to be produced in the interactions between the highest-energy cosmic rays and background photons in the universe [23]. In the following we refer to the neutrinos produced in these interactions as cosmogenic neutrinos [24]. These astrophysical and cosmogenic EHE neutrinos can constitute key messengers identifying currently unknown cosmic accelerators, possibly in the distant universe, because their propagation is not influenced by background photon or magnetic fields.

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Section: +0023mentioning

confidence: 53%

Constraints on Ultrahigh-Energy Cosmic-Ray Sources from a Search for Neutrinos above 10 PeV with IceCube

Aartsen¹,

Abraham²,

Ackermann³

et al. 2016

Phys. Rev. Lett.

143

129

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“…The seemingly large differences in the best-fit slopes could suggest a break in the power-law spectrum arising from, e.g., a second harder astrophysical component. This possibility has been previously investigated using 4 years of HESE data [12]. Here, we performed a fit to the HESE 6-year dataset introducing a second astrophysical component, described by a power-law with an independent spectral index.…”

Section: Icecube Preliminarymentioning

confidence: 99%

Observation of Astrophysical Neutrinos in Six Years of IceCube Data

Kopper¹,

Giang²,

Kurahashi³

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

181

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Cosmic rays arriving at Earth include the most energetic particles ever observed. The mechanism of their acceleration and their sources are, however, still mostly unknown. Observing astrophysical neutrinos can help solve this problem. Because neutrinos are produced in hadronic interactions and are neither absorbed nor deflected, they will point directly back to their source. This contribution covers continued studies of the high-energy astrophysical neutrino flux observed at the IceCube neutrino observatory, extending them from four to six years of data with a focus on energies above 60 TeV. The spectrum and spatial clustering of the observed neutrinos are discussed. PoS(ICRC2017)981Observation of Astrophysical Neutrinos in Six Years of IceCube Data IntroductionObservation of high-energy neutrinos provides insight into the problem of the origin and acceleration mechanism of high-energy cosmic rays. Cosmic ray protons and nuclei interacting with gas and photons present in the environment of sources and in the interstellar and intergalactic space produce neutrinos through decay of charged pions and kaons. These neutrinos have energies related to the cosmic rays that produced them and point back to their sources since neutrinos are neither affected by magnetic fields nor absorbed by matter opaque to radiation. Large-volume Cherenkov detectors like IceCube [1] observe these neutrinos when they interact in or around the instrumented volume by measuring the light produced by charged particles created in the interaction.

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“…pion decay followed by averaged-out neutrino oscillations) fall in the red contour, taking into account the uncertainties in the mixing parameters (95% C.L.) [59].…”

Section: Jhep05(2017)102 3 Dark Mattermentioning

confidence: 99%

Neutrino lines from majoron dark matter

Garcia-Cely

Heeck

2017

J. High Energ. Phys.

105

151

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Models with spontaneously broken global lepton number can lead to a pseudoGoldstone boson as a long-lived dark matter candidate. Here we revisit the case of singlet majoron dark matter and discuss multiple constraints. For masses above MeV, this model could lead to a detectable flux of monochromatic mass-eigenstate neutrinos, which have flavor ratios that depend strongly on the neutrino mass hierarchy. We provide a convenient parametrization for the loop-induced majoron couplings to charged fermions that allows us to discuss three-generation effects such as lepton flavor violation. These couplings are independent of the low-energy neutrino parameters but can be constrained by the majoron decays into charged fermions.

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Analysis of the 4-year IceCube high-energy starting events

Cited by 72 publications

References 195 publications

Constraints on Ultrahigh-Energy Cosmic-Ray Sources from a Search for Neutrinos above 10 PeV with IceCube

Constraints on Ultrahigh-Energy Cosmic-Ray Sources from a Search for Neutrinos above 10 PeV with IceCube

Observation of Astrophysical Neutrinos in Six Years of IceCube Data

Neutrino lines from majoron dark matter

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