IceCube Collaboration

By A. Achterberg, M. Ackermann, J. Ahrens, X. Bai, B. Baret, M. Bartelt, R. Bay, K. Beattie, T. Becka, P. Berghaus and 72 more. 2007

696 citations recorded by the source corpus.

The PDF file lists the IceCube Collaboration.

Subfields: Computer Networks and Communications

View Paper: https://www.semanticscholar.org/paper/bb7ad4eebb3f8514f90a2eaf71821884af0c5f7b

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In Computer Networks and Communications

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Citations in the corpus

• Flavor Ratio of Astrophysical Neutrinos above 35 TeV in IceCube (2015, methodology): “Observatory above 100 TeV in three years of data [6,7].”
• Differential limit on the extremely-high-energy cosmic neutrino flux in the presence of astrophysical background from nine years of IceCube data (2018, methodology): “The event direction of surviving events is reconstructed by the LineFit algorithm [21] that masks photon hits which have substantially different timing distributions from Cherenkov photons radiated by an EHE muon track [22].”
• THE GAMMA-RAY AND NEUTRINO SKY: A CONSISTENT PICTURE OF FERMI-LAT, MILAGRO, AND ICECUBE RESULTS (2015, methodology): “The full-sky neutrino spectrum computed for the KRAγ and KRA models (both with global CR hardening) and two choices of the CR high-energy cutoff is compared with IceCube result [6].”
• Observation of High-Energy Astrophysical Neutrinos in Three Years of IceCube Data (2014, methodology): “IceCube detector [7] while it was under construction”
• Coherent propagation of PeV neutrinos and the dip in the neutrino spectrum at IceCube (2015, background): “8 × 10(2)TeV [3, 4] and the resonance condition for neutrino scattering is m(2)Z′ ≃ 2Eνmνi , we obtain a preferred range of Z ′ mass 5MeV .”
• Compatibility of DAMA/LIBRA dark matter detection with other searches (2008, background): “These annihilations lead to high-energy neutrinos that can be observed by Earth-based detectors such as Super-Kamiokande [29] (SuperK), which currently provides the tightest indirect detection bounds at light WIMP masses, AMANDA [30, 31], IceCube [32] and ANTARES [33].”
• Projected WIMP sensitivity of the LUX-ZEPLIN dark matter experiment (2018, background): “The sensitivity of LZ to SD WIMP-neutron and WIMP-proton scattering is shown in Fig.”
• Constraining High-Energy Cosmic Neutrino Sources: Implications and Prospects (2016, methodology): “To evaluate the background, we consider both the conventional and the prompt atmospheric muon neutrino backgrounds [121, 122].”
• Singlet-Doublet Dark Matter (2011, background): “A more promising probe is the DeepCore extension to IceCube, which should also provide stringent limits on σSD for dark matter in this mass range [33].”
• First year performance of the IceCube neutrino telescope (2006, background): “Several groups are exploring use of optical Cherenkov radiation in water or ice to detect neutrinos [16,17,18,19].”
• Methods for point source analysis in high energy neutrino telescopes (2008, methodology): “Neutrino telescopes are moving steadily toward the goal of detecting astrophysical neutrinos from the most powerful galactic and extragalactic sources.”
• IceCube-Gen2: A Vision for the Future of Neutrino Astronomy in Antarctica (2014, methodology): “IceCube[23, 24], completed and in full operation since 2010, builds upon the pioneering work of the Antarctic Muon and Neutrino Detector Array (AMANDA)[25] and has begun to probe signals from astrophysical neutrinos.”
• Improved limit to the diffuse flux of ultrahigh energy neutrinos from the Pierre Auger Observatory (2015, positive): “A refinement of the IceCube search technique to extend the neutrino sensitivity down to 10 TeV [37], yielded a power-law fit to the measured flux without cut-off given by dN/dE = Φ0(Eν/E0) −γ with Φ0 = 2.06×10−18 GeV−1 cm−2 s−1 sr−1, E0 = 105 GeV, and γ = 2.46.”
• Indirect dark matter signatures in the cosmic dark ages. I. Generalizing the bound on s-wave dark matter annihilation from Planck results (2015, background): “Interestingly, this bound is competitive with that placed by IceCube from observations of galaxy clusters [45], the Galactic Center [46], and the Milky Way halo [47], and unlike those limits is independent of uncertainties in the local DM density, the DM distribution, and the amount of DM substructu”
• Choked Jets and Low-Luminosity Gamma-Ray Bursts as Hidden Neutrino Sources (2015, background): “H E ] 2 2 M ar 2 01 6 Choked Jets and Low-Luminosity Gamma-Ray Bursts as Hidden Neutrino Sources Nicholas Senno,1 Kohta Murase,1 and Peter Mészáros1 1Department of Physics; Department of Astronomy & Astrophysics; Center for Particle and Gravitational Astrophysics, The Pennsylvania State University”
• Particle dark matter: Evidence, candidates and constraints (2004, background): “IceCube[18, 19], beginning construction in 2005, and scheduled for completion in 2010, will be the first kilometer scale high-energy neutrino telescope.”