The IceCube Collaboration

By The IceCube Collaboration. 2007

673 citations recorded by the source corpus.

The AMANDA-II data collected during the period 2000–2003 have been analysed in a search for a diffuse flux of high-energy extra-terrestrial muon neutrinos from the sum of all sources in the Universe. With no excess events seen, an upper limit of Eν × dNν/dEν< 7.4×10−8 GeV cm−2 s−1 sr−1was obtained. The sensitivity of the diffuse analysis of IceCube 9 string for 137 days of data is calculated to be Eν × dNν/dEν< 1.3× 10−7 GeV cm−2 s−1 sr−1. No excess events are observed, which confirms the AMANDA-II upper limit.

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Citations in the corpus

Search for sterile neutrino mixing using three years of IceCube DeepCore data (2017, background): “This region, characterized by a short optical absorption length, is present due to dust accumulation during a geological period about 60 to 70 thousand years ago [52].”
Spectra of neutrinos from dark matter annihilations (2005, methodology): “IMB [6], Kamiokande [7], Baksan [8], Macro [9], Super-Kamiokande [10], AMANDA [11] and BAIKAL [12] already obtained constraints on DMν fluxes, while experiments that are under construction, like ANTARES [13] and ICECUBE [14], or that are planned, like NEMO [15], NESTOR [16] and a Mton-scale water Če”
Muon Track Reconstruction and Data Selection Techniques in AMANDA (2004, methodology): “It will consist of 4800 PMT deployed on 80 vertical strings and will surround the AMANDA detector [57].”
Light Sterile Neutrinos: A White Paper (2012, background): “652, 306 (2006), arXiv:astro-ph/0603775 [astro-ph]. [172] R. K. de Naray, G. D. Martinez, J. S. Bullock, and M. Kaplinghat, “The Case Against Warm or SelfInteracting Dark Matter as Explanations for Cores in Low Surface Brightness Galaxies,” (2009), arXiv:0912.3518 [astro-ph.CO]. [173] A. V. Maccio’ ”
New constraints on oscillation parameters fromνeappearance andνμdisappearance in the NOvA experiment (2018, background): “Comparison of measured 90% conﬁdence level contours for ∆ m 232 vs. sin 2 θ 23 for this result (black line; best-ﬁt value, black point), T2K [7] (green dashed), MINOS [6] (red dashed), IceCube [57] (blue dotted), and Super-Kamiokande [58] (purple dash-dotted). intervals in the inverted mass hierarch”
Atmospheric and Astrophysical Neutrinos above 1 TeV Interacting in IceCube (2014, methodology): “Spurious vetoes due to detector noise aremitigated by requiring that the photons are detected in local coincidence [5] at times that are causally compatible with the estimated vertex.”
Implication of neutrino backgrounds on the reach of next generation dark matter direct detection experiments (2013, methodology): “The atmospheric neutrino flux has been detected by several experiments: Super-Kamiokande [17], SNO [18], MINOS [19], and IceCube [20].”
Measurement of Atmospheric Neutrino Oscillations at 6-56 GeV with IceCube DeepCore (2017, background): “Systematics related to the response of the detector itself, including photon propagation through the ice and the anisotropic sensitivity of the DOMs, have the largest impact on this analysis.”
Measurement of the atmospheric neutrino energy spectrum from 100 GeV to 400 TeV with IceCube (2010, background): “The likelihood function to be maximized is the function [31]”
The IceCube Neutrino Observatory - Contributions to ICRC 2015 Part II: Atmospheric and Astrophysical Diffuse Neutrino Searches of All Flavors (2015, methodology): “However, this was not yet possible for the observed cosmic neutrino flux; the arrival directions of the neutrinos are consistent with an isotropic flux [2, 10].”
Dark matter direct search sensitivity of the PandaX-4T experiment (2018, result): “D 93, 052014 (2016) [32] M. G. Aartsen et al. (IceCube Collaboration), JCAP 1604, 022 (2016) [33] K. Choi et al. (Super-Kamiokande Collaboration), Phys.”
Observation of Gravitational Waves from the Coalescence of a 2.5–4.5 M ⊙ Compact Object and a Neutron Star (2024, methodology): “No significant counterpart candidates have been re-ported for GW230529 (IceCube Collaboration 2023; Karambelkar et al. 2023; Lipunov et al. 2023; Longo et al. 2023; Lesage et al. 2023; Savchenko et al. 2023; Sugita et al. 2023a,b; Waratkar et al. 2023).”
IceCube PeV-EeV neutrinos and secret interactions of neutrinos (2014, background): “Recently IceCube reported the detection of two PeV neutrinos and 26 additional events, more than expected from atmospheric backgrounds [1, 2].”
The IceCube data acquisition system: Signal capture, digitization,and timestamping (2008, background): “Digital information from the ensemble of DOMs allows reconstruction of event topology and energy, from which the nature of the event may be determined [7].”
Linking high-energy cosmic particles by black-hole jets embedded in large-scale structures (2017, background): “The IceCube Observatory recently discovered high-energy cosmic neutrinos [5, 6], which have been anticipated to provide crucial clues to this age-old mystery.”
Measurement of electron antineutrino oscillation based on 1230 days of operation of the Daya Bay experiment (2016, background): “• the disappearance of νμ produced by particle interactions in the upper atmosphere [70, 71], with energies >1 GeV and baselines up to the diameter of the Earth.”