Browsing by Author "IceCube Collaboration"
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Item All-flavour search for neutrinos from dark matter annihilations in the Milky Way with IceCube/DeepCore(Springer, 2016) IceCube Collaboration; Palczewski, T.; Pepper, J.A.; Toale, P.A.; Williams, D.R.; RWTH Aachen University; University of Adelaide; University of Alaska System; University of Alaska Anchorage; Clark Atlanta University; University System of Georgia; Georgia Institute of Technology; Southern University System; Southern University & A&M College; University of California System; University of California Berkeley; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Humboldt University of Berlin; Ruhr University Bochum; University of Bonn; Universite Libre de Bruxelles; Vrije Universiteit Brussel; Massachusetts Institute of Technology (MIT); Chiba University; University of Canterbury; University System of Maryland; University of Maryland College Park; University System of Ohio; Ohio State University; University of Copenhagen; Niels Bohr Institute; Dortmund University of Technology; Michigan State University; University of Alberta; University of Erlangen Nuremberg; University of Geneva; Ghent University; University of California Irvine; University of Kansas; University of Wisconsin System; University of Wisconsin Madison; Johannes Gutenberg University of Mainz; Marquette University; University of Mons; National Research Nuclear University MEPhI (Moscow Engineering Physics Institute); Technical University of Munich; University of Munster; University of Delaware; Yale University; University of Oxford; Drexel University; South Dakota School Mines & Technology; Oskar Klein Centre; Stockholm University; State University of New York (SUNY) System; State University of New York (SUNY) Stony Brook; Sungkyunkwan University (SKKU); University of Toronto; University of Alabama Tuscaloosa; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; University of Rochester; Uppsala University; University of Wuppertal; Helmholtz Association; Deutsches Elektronen-Synchrotron (DESY)We present the first IceCube search for a signal of dark matter annihilations in the Milky Way using all-flavour neutrino-induced particle cascades. The analysis focuses on the DeepCore sub-detector of IceCube, and uses the surrounding IceCube strings as a veto region in order to select starting events in the DeepCore volume. We use 329 live-days of data from IceCube operating in its 86-string configuration during 2011-2012. No neutrino excess is found, the final result being compatible with the background-only hypothesis. From this null result, we derive upper limits on the velocity-averaged self-annihilation cross-section, \(\langle \sigma_A v\rangle\), for dark matter candidate masses ranging from 30 GeV up to 10 TeV, assuming both a cuspy and a flat-cored dark matter halo profile. For dark matter masses between 200 GeV and 10 TeV, the results improve on all previous IceCube results on \(\langle \sigma_A v\rangle\), reaching a level of 10⁻²³ cm³ s⁻¹, depending on the annihilation channel assumed, for a cusped NFW profile. The analysis demonstrates that all-flavour searches are competitive with muon channel searches despite the intrinsically worse angular resolution of cascades compared to muon tracks in IceCube.Item Constraints on the extremely-high energy cosmic neutrino flux with the IceCube 2008-2009 data (vol 83, 092003, 2011)(American Physical Society, 2011-10-13) IceCube Collaboration; National University of Singapore; Zhejiang University; University of Alabama TuscaloosaItem Development of a general analysis and unfolding scheme and its application to measure the energy spectrum of atmospheric neutrinos with IceCube(Springer, 2015) IceCube Collaboration; Palczewski, T.; Pepper, J.A.; Toale, P.A.; Williams, D.R.; Xu, D.L.; Zarzhitsky, P.; RWTH Aachen University; University of Adelaide; University of Alaska System; University of Alaska Anchorage; Clark Atlanta University; University System of Georgia; Georgia Institute of Technology; Southern University System; Southern University & A&M College; University of California System; University of California Berkeley; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Humboldt University of Berlin; Ruhr University Bochum; University of Wurzburg; University of Bonn; Universite Libre de Bruxelles; Vrije Universiteit Brussel; Chiba University; University of Canterbury; University System of Maryland; University of Maryland College Park; University System of Ohio; Ohio State University; University of Copenhagen; Niels Bohr Institute; Dortmund University of Technology; University of Alberta; University of Erlangen Nuremberg; University of Geneva; Ghent University; University of California Irvine; University of Kansas; University of Wisconsin System; University of Wisconsin Madison; Johannes Gutenberg University of Mainz; University of Mons; Technical University of Munich; University of Delaware; University of Oxford; South Dakota School Mines & Technology; Oskar Klein Centre; Stockholm University; State University of New York (SUNY) System; State University of New York (SUNY) Stony Brook; Sungkyunkwan University (SKKU); University of Toronto; University of Alabama Tuscaloosa; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; Uppsala University; University of Wuppertal; Helmholtz Association; Deutsches Elektronen-Synchrotron (DESY)We present the development and application of a generic analysis scheme for the measurement of neutrino spectra with the IceCube detector. This scheme is based on regularized unfolding, preceded by an event selection which uses a Minimum Redundancy Maximum Relevance algorithm to select the relevant variables and a random forest for the classification of events. The analysis has been developed using IceCube data from the 59-string configuration of the detector. 27,771 neutrino candidates were detected in 346 days of livetime. A rejection of 99.9999% of the atmospheric muon background is achieved. The energy spectrum of the atmospheric neutrino flux is obtained using the TRUEE unfolding program. The unfolded spectrum of atmospheric muon neutrinos covers an energy range from 100 GeV to 1 PeV. Compared to the previous measurement using the detector in the 40-string configuration, the analysis presented here, extends the upper end of the atmospheric neutrino spectrum by more than a factor of two, reaching an energy region that has not been previously accessed by spectral measurements.Item Development of an analysis to probe the neutrino mass ordering with atmospheric neutrinos using three years of IceCube DeepCore data IceCube Collaboration(Springer, 2020) IceCube Collaboration; PICO Collaboration; Kopper, S.; Santander, M.; Williams, D.R.; RWTH Aachen University; University of Adelaide; University of Alaska System; University of Alaska Anchorage; University of Texas System; University of Texas Arlington; Clark Atlanta University; University System of Georgia; Georgia Institute of Technology; Southern University System; Southern University & A&M College; University of California System; University of California Berkeley; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Humboldt University of Berlin; Ruhr University Bochum; University of Wurzburg; Universite Libre de Bruxelles; Vrije Universiteit Brussel; Massachusetts Institute of Technology (MIT); Chiba University; University of Canterbury; University System of Maryland; University of Maryland College Park; University System of Ohio; Ohio State University; University of Copenhagen; Niels Bohr Institute; Dortmund University of Technology; Michigan State University; University of Alberta; University of Erlangen Nuremberg; University of Geneva; Ghent University; University of California Irvine; University of Kansas; University of California Los Angeles; University of Wisconsin System; University of Wisconsin Madison; Johannes Gutenberg University of Mainz; University of Manchester; Marquette University; Technical University of Munich; University of Munster; University of Delaware; Yale University; University of Oxford; Drexel University; South Dakota School Mines & Technology; University of Rochester; Oskar Klein Centre; Stockholm University; State University of New York (SUNY) System; State University of New York (SUNY) Stony Brook; Sungkyunkwan University (SKKU); University of Alabama Tuscaloosa; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; Uppsala University; University of Wuppertal; Helmholtz Association; Deutsches Elektronen-Synchrotron (DESY); University of TokyoThe Neutrino Mass Ordering (NMO) remains one of the outstanding questions in the field of neutrino physics. One strategy to measure the NMO is to observe matter effects in the oscillation pattern of atmospheric neutrinos above \(\sim 1\phantom{\rule{0.166667em}{0ex}}\mathrm{GeV}\), as proposed for several next-generation neutrino experiments. Moreover, the existing IceCube DeepCore detector can already explore this type of measurement. We present the development and application of two independent analyses to search for the signature of the NMO with three years of DeepCore data. These analyses include a full treatment of systematic uncertainties and a statistically-rigorous method to determine the significance for the NMO from a fit to the data. Both analyses show that the dataset is fully compatible with both mass orderings. For the more sensitive analysis, we observe a preference for normal ordering with a p-value of \({p}_{\mathrm{IO}}=15.3%\) and \({\mathrm{CL}}_{s}=53.3%\) for the inverted ordering hypothesis, while the experimental results from both analyses are consistent within their uncertainties. Since the result is independent of the value of \({\delta }_{\mathrm{CP}}\) and obtained from energies \({E}_{\nu }\gtrsim 5\phantom{\rule{0.166667em}{0ex}}\mathrm{GeV}\), it is complementary to recent results from long-baseline experiments. These analyses set the groundwork for the future of this measurement with more capable detectors, such as the IceCube Upgrade and the proposed PINGU detector.Item eV-Scale Sterile Neutrino Search Using Eight Years of Atmospheric Muon Neutrino Data from the IceCube Neutrino Observatory(American Physical Society, 2020) IceCube Collaboration; Kopper, S.; Santander, M.; Williams, D.R.; RWTH Aachen University; University of Adelaide; University of Alaska System; University of Alaska Anchorage; University of Texas System; University of Texas Arlington; Clark Atlanta University; University System of Georgia; Georgia Institute of Technology; Southern University System; Southern University & A&M College; University of California System; University of California Berkeley; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Humboldt University of Berlin; Ruhr University Bochum; University of Wurzburg; Universite Libre de Bruxelles; Vrije Universiteit Brussel; Massachusetts Institute of Technology (MIT); Chiba University; Loyola University Chicago; University of Canterbury; University System of Maryland; University of Maryland College Park; University System of Ohio; Ohio State University; University of Copenhagen; Niels Bohr Institute; Dortmund University of Technology; Michigan State University; University of Alberta; University of Erlangen Nuremberg; Technical University of Munich; University of Geneva; Ghent University; University of California Irvine; Helmholtz Association; Karlsruhe Institute of Technology; University of Kansas; University of California Los Angeles; Mercer University; University of Wisconsin System; University of Wisconsin Madison; Johannes Gutenberg University of Mainz; Marquette University; University of Munster; University of Delaware; Yale University; University of Oxford; Drexel University; South Dakota School Mines & Technology; University of Rochester; Oskar Klein Centre; Stockholm University; State University of New York (SUNY) System; State University of New York (SUNY) Stony Brook; Sungkyunkwan University (SKKU); Institute for Basic Science - Korea (IBS); University of Alabama Tuscaloosa; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; Uppsala University; University of Wuppertal; Deutsches Elektronen-Synchrotron (DESY); University of Tokyo; University of Padua; National Research Nuclear University MEPhI (Moscow Engineering Physics Institute)The results of a \(3+1\) sterile neutrino search using eight years of data from the IceCube Neutrino Observatory are presented. A total of 305 735 muon neutrino events are analyzed in reconstructed energy-zenith space to test for signatures of a matter-enhanced oscillation that would occur given a sterile neutrino state with a mass-squared differences between 0.01 and \(100\text{}\text{}{\mathrm{eV}}^{2}\). The best-fit point is found to be at \({\mathrm{sin}}^{2}\left(2{\theta }_{24}\right)=0.10\) and \(\Delta {m}_{41}^{2}=4.5\text{}\text{}{\mathrm{eV}}^{2}\), which is consistent with the no sterile neutrino hypothesis with a \(p\) value of 8.0%.Item First search for dark matter annihilations in the Earth with the IceCube detector(Springer, 2017) IceCube Collaboration; Palczewski, T.; Pepper, J.A.; Toale, P.A.; Williams, D.R.; RWTH Aachen University; University of Adelaide; University of Alaska System; University of Alaska Anchorage; Clark Atlanta University; University System of Georgia; Georgia Institute of Technology; Southern University System; Southern University & A&M College; University of California System; University of California Berkeley; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Humboldt University of Berlin; Ruhr University Bochum; University of Wurzburg; University of Bonn; Universite Libre de Bruxelles; Vrije Universiteit Brussel; Massachusetts Institute of Technology (MIT); Chiba University; University of Canterbury; University System of Maryland; University of Maryland College Park; University System of Ohio; Ohio State University; University of Copenhagen; Niels Bohr Institute; Dortmund University of Technology; Michigan State University; University of Alberta; University of Erlangen Nuremberg; University of Geneva; Ghent University; University of California Irvine; University of Kansas; University of Wisconsin System; University of Wisconsin Madison; Johannes Gutenberg University of Mainz; Marquette University; University of Mons; Technical University of Munich; University of Munster; University of Delaware; Yale University; University of Oxford; Drexel University; South Dakota School Mines & Technology; Oskar Klein Centre; Stockholm University; State University of New York (SUNY) System; State University of New York (SUNY) Stony Brook; Sungkyunkwan University (SKKU); University of Toronto; University of Alabama Tuscaloosa; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; University of Rochester; Uppsala University; University of Wuppertal; Helmholtz Association; Deutsches Elektronen-Synchrotron (DESY); University of TokyoWe present the results of the first IceCube search for dark matter annihilation in the center of the Earth. Weakly interacting massive particles (WIMPs), candidates for dark matter, can scatter off nuclei inside the Earth and fall below its escape velocity. Over time the captured WIMPs will be accumulated and may eventually self-annihilate. Among the annihilation products only neutrinos can escape from the center of the Earth. Large-scale neutrino telescopes, such as the cubic kilometer IceCube Neutrino Observatory located at the South Pole, can be used to search for such neutrino fluxes. Data from 327 days of detector livetime during 2011/2012 were analyzed. No excess beyond the expected background from atmospheric neutrinos was detected. The derived upper limits on the annihilation rate of WIMPs in the Earth (\(\Gamma_A\) = 1.12 x 10¹⁴ s⁻¹ for WIMP masses of 50 GeV annihilating into tau leptons) and the resulting muon flux are an order of magnitude stronger than the limits of the last analysis performed with data from IceCube's predecessor AMANDA. The limits can be translated in terms of a spin-independent WIMP-nucleon cross section. For a WIMP mass of 50 GeV this analysis results in the most restrictive limits achieved with IceCube data.Item IceCube sensitivity for low-energy neutrinos from nearby supernovae (vol 535, pg A109, 2011)(EDP Sciences, 2014-02-27) IceCube Collaboration; University of Wisconsin System; University of Wisconsin Madison; Ghent University; University of Canterbury; University of Oxford; University of Wuppertal; University of Delaware; University of California System; University of California Irvine; University of California Berkeley; Helmholtz Association; Deutsches Elektronen-Synchrotron (DESY); United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; University System of Ohio; Ohio State University; Universite Libre de Bruxelles; Ruhr University Bochum; University of Wurzburg; University System of Maryland; University of Maryland College Park; University of Kansas; RWTH Aachen University; Oskar Klein Centre; Stockholm University; Vrije Universiteit Brussel; University of Bonn; Uppsala University; Dortmund University of Technology; Swiss Federal Institutes of Technology Domain; Ecole Polytechnique Federale de Lausanne; Max Planck Society; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; University System of Georgia; Georgia Institute of Technology; Clark Atlanta University; Southern University System; Southern University & A&M College; University of Alberta; Johannes Gutenberg University of Mainz; University of Mons; Chiba University; Humboldt University of Berlin; Gran Sasso Science Institute (GSSI); University of Alaska System; University of Alaska Anchorage; University West Indies Mona Jamaica; University of the West Indies Open Campus; National Aeronautics & Space Administration (NASA); NASA Goddard Space Flight Center; University of Alabama Tuscaloosa; Los Alamos National LaboratoryItem Improved limits on dark matter annihilation in the Sun with the 79-string IceCube detector and implications for supersymmetry(IOP Publishing, 2016) IceCube Collaboration; Palczewski, T.; Pepper, J.A.; Toale, P.A.; Williams, D.R.; RWTH Aachen University; University of Adelaide; University of Alaska System; University of Alaska Anchorage; Clark Atlanta University; University System of Georgia; Georgia Institute of Technology; Southern University System; Southern University & A&M College; University of California System; University of California Berkeley; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Humboldt University of Berlin; Ruhr University Bochum; University of Wurzburg; University of Bonn; Universite Libre de Bruxelles; Vrije Universiteit Brussel; Massachusetts Institute of Technology (MIT); Chiba University; University of Canterbury; University System of Maryland; University of Maryland College Park; University System of Ohio; Ohio State University; University of Copenhagen; Niels Bohr Institute; Dortmund University of Technology; Michigan State University; University of Alberta; University of Erlangen Nuremberg; University of Geneva; Ghent University; University of California Irvine; University of Kansas; University of Wisconsin System; University of Wisconsin Madison; Johannes Gutenberg University of Mainz; University of Mons; Technical University of Munich; University of Delaware; Yale University; University of Oxford; Drexel University; South Dakota School Mines & Technology; Oskar Klein Centre; Stockholm University; State University of New York (SUNY) System; State University of New York (SUNY) Stony Brook; Sungkyunkwan University (SKKU); University of Toronto; University of Alabama Tuscaloosa; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; University of Rochester; Uppsala University; University of Wuppertal; Helmholtz Association; Deutsches Elektronen-Synchrotron (DESY); University of Tokyo; National Aeronautics & Space Administration (NASA); NASA Goddard Space Flight Center; University of British Columbia; Imperial College London; University of AmsterdamWe present an improved event-level likelihood formalism for including neutrino telescope data in global fits to new physics. We derive limits on spin-dependent dark matter-proton scattering by employing the new formalism in a re-analysis of data from the 79-string IceCube search for dark matter annihilation in the Sun, including explicit energy information for each event. The new analysis excludes a number of models in the weak-scale minimal supersymmetric standard model (MSSM) for the first time. This work is accompanied by the public release of the 79-string IceCube data, as well as an associated computer code for applying the new likelihood to arbitrary dark matter models.Item Joint Constraints on Galactic Diffuse Neutrino Emission from the ANTARES and IceCube Neutrino Telescopes(IOP Publishing, 2018-11-20) ANTARES Collaboration; IceCube Collaboration; University of Alabama TuscaloosaThe existence of diffuse Galactic neutrino production is expected from cosmic-ray interactions with Galactic gas and radiation fields. Thus, neutrinos are a unique messenger offering the opportunity to test the products of Galactic cosmic-ray interactions up to energies of hundreds of TeV. Here we present a search for this production using ten years of Astronomy with a Neutrino Telescope and Abyss environmental RESearch (ANTARES) track and shower data, as well as seven years of IceCube track data. The data are combined into a joint likelihood test for neutrino emission according to the KRA(gamma) model assuming a 5 PeV per nucleon Galactic cosmic-ray cutoff. No significant excess is found. As a consequence, the limits presented in this Letter start constraining the model parameter space for Galactic cosmic-ray production and transport.Item Measurement of atmospheric tau neutrino appearance with IceCube DeepCore(American Physical Society, 2019) IceCube Collaboration; Kopper, S.; Nakarmi, P.; Santander, M.; Williams, D.R.; RWTH Aachen University; University of Adelaide; University of Alaska System; University of Alaska Anchorage; University of Texas System; University of Texas Arlington; Clark Atlanta University; University System of Georgia; Georgia Institute of Technology; University of California System; University of California Berkeley; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Humboldt University of Berlin; Ruhr University Bochum; University of Wurzburg; Universite Libre de Bruxelles; Vrije Universiteit Brussel; Massachusetts Institute of Technology (MIT); Chiba University; University of Canterbury; University System of Maryland; University of Maryland College Park; University System of Ohio; Ohio State University; University of Copenhagen; Niels Bohr Institute; Dortmund University of Technology; Michigan State University; University of Alberta; University of Erlangen Nuremberg; Technical University of Munich; University of Geneva; Ghent University; University of California Irvine; University of Kansas; University of California Los Angeles; University of Wisconsin System; University of Wisconsin Madison; Johannes Gutenberg University of Mainz; Marquette University; University of Munster; University of Delaware; Yale University; University of Oxford; Drexel University; South Dakota School Mines & Technology; University of Rochester; Oskar Klein Centre; Stockholm University; State University of New York (SUNY) System; State University of New York (SUNY) Stony Brook; Sungkyunkwan University (SKKU); Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; Uppsala University; University of Wuppertal; Helmholtz Association; Deutsches Elektronen-Synchrotron (DESY); University of Alabama TuscaloosaWe present a measurement of atmospheric tau neutrino appearance from oscillations with three years of data from the DeepCore subarray of the IceCube Neutrino Observatory. This analysis uses atmospheric neutrinos from the full sky with reconstructed energies between 5.6 and 56 GeV to search for a statistical excess of cascadelike neutrino events which are the signature of \({\nu }_{\tau }\) interactions. For \(\mathrm{CC}+\mathrm{NC}\) (CC-only) interactions, we measure the tau neutrino normalization to be \({0.73}_{-0.24}^{+0.30}\) (\({0.57}_{-0.30}^{+0.36}\)) and exclude the absence of tau neutrino oscillations at a significance of \(3.2\sigma \) (\(2.0\sigma \)) These results are consistent with, and of similar precision to, a confirmatory IceCube analysis also presented, as well as measurements performed by other experiments.Item Measurement of the high-energy all-flavor neutrino-nucleon cross section with IceCube(American Physical Society, 2021) IceCube Collaboration; Ghadimi, A.; Goswami, S.; Kopper, S.; Santander, M.; Williams, D.R.; RWTH Aachen University; University of Adelaide; University of Alaska System; University of Alaska Anchorage; University of Texas System; University of Texas Arlington; Clark Atlanta University; University System of Georgia; Georgia Institute of Technology; Southern University System; Southern University & A&M College; University of California System; University of California Berkeley; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Humboldt University of Berlin; Ruhr University Bochum; University of Wurzburg; Universite Libre de Bruxelles; Vrije Universiteit Brussel; Harvard University; Massachusetts Institute of Technology (MIT); Chiba University; Loyola University Chicago; University of Canterbury; University System of Maryland; University of Maryland College Park; University System of Ohio; Ohio State University; University of Copenhagen; Niels Bohr Institute; Dortmund University of Technology; Michigan State University; University of Alberta; University of Erlangen Nuremberg; Technical University of Munich; University of Geneva; Ghent University; University of California Irvine; Helmholtz Association; Karlsruhe Institute of Technology; University of Kansas; University of California Los Angeles; Mercer University; University of Wisconsin System; University of Wisconsin Madison; Johannes Gutenberg University of Mainz; Marquette University; University of Munster; University of Delaware; Yale University; University of Oxford; Drexel University; South Dakota School Mines & Technology; University of Rochester; Oskar Klein Centre; Stockholm University; State University of New York (SUNY) System; State University of New York (SUNY) Stony Brook; Sungkyunkwan University (SKKU); Institute for Basic Science - Korea (IBS); University of Alabama Tuscaloosa; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; Uppsala University; University of Wuppertal; Deutsches Elektronen-Synchrotron (DESY); University of Padua; National Research Nuclear University MEPhI (Moscow Engineering Physics Institute); University of TokyoThe flux of high-energy neutrinos passing through the Earth is attenuated due to their interactions with matter. The interaction rate is determined by the neutrino interaction cross section and affects the flux arriving at the IceCube Neutrino Observatory, a cubic-kilometer neutrino detector embedded in the Antarctic ice sheet. We present a measurement of the neutrino cross section between 60 TeV and 10 PeV using the high-energy starting event (HESE) sample from IceCube with 7.5 years of data. The result is binned in neutrino energy and obtained using both Bayesian and frequentist statistics. We find it compatible with predictions from the Standard Model. While the cross section is expected to be flavor independent above 1 TeV, additional constraints on the measurement are included through updated experimental particle identification (PID) classifiers, proxies for the three neutrino flavors. This is the first such measurement to use a ternary PID observable and the first to account for neutrinos from tau decay.Item Measurement of the nu(mu) energy spectrum with IceCube-79(Springer, 2017) IceCube Collaboration; Pepper, J.A.; Toale, P.A.; Williams, D.R.; RWTH Aachen University; University of Adelaide; University of Alaska System; University of Alaska Anchorage; Clark Atlanta University; University System of Georgia; Georgia Institute of Technology; Southern University System; Southern University & A&M College; University of California System; University of California Berkeley; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Humboldt University of Berlin; Ruhr University Bochum; University of Wurzburg; University of Bonn; Universite Libre de Bruxelles; Vrije Universiteit Brussel; Massachusetts Institute of Technology (MIT); Chiba University; University of Canterbury; University System of Maryland; University of Maryland College Park; University System of Ohio; Ohio State University; University of Copenhagen; Niels Bohr Institute; Dortmund University of Technology; Michigan State University; University of Alberta; University of Erlangen Nuremberg; University of Geneva; Ghent University; University of California Irvine; University of Kansas; University of Wisconsin System; University of Wisconsin Madison; Johannes Gutenberg University of Mainz; Marquette University; University of Mons; Technical University of Munich; University of Munster; University of Delaware; Yale University; University of Oxford; Drexel University; South Dakota School Mines & Technology; Oskar Klein Centre; Stockholm University; State University of New York (SUNY) System; State University of New York (SUNY) Stony Brook; Sungkyunkwan University (SKKU); University of Toronto; University of Alabama Tuscaloosa; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; University of Rochester; Uppsala University; University of Wuppertal; Helmholtz Association; Deutsches Elektronen-Synchrotron (DESY); University of TokyoIceCube is a neutrino observatory deployed in the glacial ice at the geographic South Pole. The \({\nu }_{\mu }\) energy unfolding described in this paper is based on data taken with IceCube in its 79-string configuration. A sample of muon neutrino charged-current interactions with a purity of 99.5% was selected by means of a multivariate classification process based on machine learning. The subsequent unfolding was performed using the software Truee. The resulting spectrum covers an E \({}_{\nu }\) -range of more than four orders of magnitude from 125 GeV to 3.2 PeV. Compared to the Honda atmospheric neutrino flux model, the energy spectrum shows an excess of more than \(1.9\phantom{\rule{0.166667em}{0ex}}\sigma \) in four adjacent bins for neutrino energies \({E}_{\nu }\ge 177.8\phantom{\rule{0.166667em}{0ex}}\text{TeV}\). The obtained spectrum is fully compatible with previous measurements of the atmospheric neutrino flux and recent IceCube measurements of a flux of high-energy astrophysical neutrinos.Item Neutrino oscillation studies with IceCube-DeepCore(Elsevier, 2016) IceCube Collaboration; Palczewski, T.; Pepper, J.A.; Toale, P.A.; Williams, D.R.; RWTH Aachen University; University of Adelaide; University of Alaska System; University of Alaska Anchorage; Clark Atlanta University; University System of Georgia; Georgia Institute of Technology; Southern University System; Southern University & A&M College; University of California System; University of California Berkeley; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Humboldt University of Berlin; Ruhr University Bochum; University of Wurzburg; University of Bonn; Universite Libre de Bruxelles; Vrije Universiteit Brussel; Massachusetts Institute of Technology (MIT); Chiba University; University of Canterbury; University System of Maryland; University of Maryland College Park; University System of Ohio; Ohio State University; University of Copenhagen; Niels Bohr Institute; Dortmund University of Technology; Michigan State University; University of Alberta; University of Erlangen Nuremberg; University of Geneva; Ghent University; University of California Irvine; University of Kansas; University of Wisconsin System; University of Wisconsin Madison; Johannes Gutenberg University of Mainz; University of Mons; Technical University of Munich; University of Delaware; Yale University; University of Oxford; Drexel University; South Dakota School Mines & Technology; Oskar Klein Centre; Stockholm University; Sungkyunkwan University (SKKU); University of Toronto; University of Alabama Tuscaloosa; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; Uppsala University; University of Wuppertal; Helmholtz Association; Deutsches Elektronen-Synchrotron (DESY); University of Tokyo; National Aeronautics & Space Administration (NASA); NASA Goddard Space Flight CenterIceCube, a gigaton-scale neutrino detector located at the South Pole, was primarily designed to search for astrophysical neutrinos with energies of PeV and higher. This goal has been achieved with the detection of the highest energy neutrinos to date. At the other end of the energy spectrum, the DeepCore extension lowers the energy threshold of the detector to approximately 10 GeV and opens the door for oscillation studies using atmospheric neutrinos. An analysis of the disappearance of these neutrinos has been completed, with the results produced being complementary with dedicated oscillation experiments. Following a review of the detector principle and performance, the method used to make these calculations, as well as the results, is detailed. Finally, the future prospects of IceCube-DeepCore and the next generation of neutrino experiments at the South Pole (IceCube-Gen2, specifically the PINGU sub-detector) are briefly discussed.Item Search for annihilating dark matter in the Sun with 3 years of IceCube data(Springer, 2017) IceCube Collaboration; Pepper, J.A.; Toale, P.A.; Williams, D.R.; RWTH Aachen University; University of Adelaide; University of Alaska System; University of Alaska Anchorage; Clark Atlanta University; University System of Georgia; Georgia Institute of Technology; Southern University System; Southern University & A&M College; University of California System; University of California Berkeley; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Humboldt University of Berlin; Ruhr University Bochum; University of Wurzburg; University of Bonn; Universite Libre de Bruxelles; Vrije Universiteit Brussel; Massachusetts Institute of Technology (MIT); Chiba University; University of Canterbury; University System of Maryland; University of Maryland College Park; University System of Ohio; Ohio State University; University of Copenhagen; Niels Bohr Institute; Dortmund University of Technology; Michigan State University; University of Alberta; University of Erlangen Nuremberg; University of Geneva; Ghent University; University of California Irvine; University of Kansas; University of Wisconsin System; University of Wisconsin Madison; Johannes Gutenberg University of Mainz; Marquette University; University of Mons; Technical University of Munich; University of Munster; University of Delaware; Yale University; University of Oxford; Drexel University; South Dakota School Mines & Technology; Oskar Klein Centre; Stockholm University; State University of New York (SUNY) System; State University of New York (SUNY) Stony Brook; Sungkyunkwan University (SKKU); University of Toronto; University of Alabama Tuscaloosa; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; University of Rochester; Uppsala University; University of Wuppertal; Helmholtz Association; Deutsches Elektronen-Synchrotron (DESY); University of TokyoWe present results from an analysis looking for dark matter annihilation in the Sun with the IceCube neutrino telescope. Gravitationally trapped dark matter in the Sun’s core can annihilate into Standard Model particles making the Sun a source of GeV neutrinos. IceCube is able to detect neutrinos with energies >100 GeV while its low-energy infill array DeepCore extends this to >10 GeV. This analysis uses data gathered in the austral winters between May 2011 and May 2014, corresponding to 532 days of livetime when the Sun, being below the horizon, is a source of up-going neutrino events, easiest to discriminate against the dominant background of atmospheric muons. The sensitivity is a factor of two to four better than previous searches due to additional statistics and improved analysis methods involving better background rejection and reconstructions. The resultant upper limits on the spin-dependent dark matter-proton scattering cross section reach down to \(1.46×{10}^{-5}\) pb for a dark matter particle of mass 500 GeV annihilating exclusively into \({\tau }^{+}{\tau }^{-}\) particles. These are currently the most stringent limits on the spin-dependent dark matter-proton scattering cross section for WIMP masses above 50 GeV.Item Search for annihilating dark matter in the Sun with 3 years of IceCube data (vol 77, pg 146, 2017)(Springer, 2019) IceCube Collaboration; Pepper, J.A.; Toale, P.A.; Williams, D.R.; RWTH Aachen University; University of Adelaide; University of Alaska System; University of Alaska Anchorage; Clark Atlanta University; University System of Georgia; Georgia Institute of Technology; Southern University System; Southern University & A&M College; University of California System; University of California Berkeley; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Humboldt University of Berlin; Ruhr University Bochum; University of Wurzburg; University of Bonn; Universite Libre de Bruxelles; Vrije Universiteit Brussel; Massachusetts Institute of Technology (MIT); Chiba University; University of Canterbury; University System of Maryland; University of Maryland College Park; University System of Ohio; Ohio State University; University of Copenhagen; Niels Bohr Institute; Dortmund University of Technology; Michigan State University; University of Alberta; University of Erlangen Nuremberg; University of Geneva; Ghent University; University of California Irvine; University of Kansas; University of Wisconsin System; University of Wisconsin Madison; Johannes Gutenberg University of Mainz; Marquette University; University of Mons; Technical University of Munich; University of Munster; University of Delaware; Yale University; University of Oxford; Drexel University; South Dakota School Mines & Technology; Oskar Klein Centre; Stockholm University; State University of New York (SUNY) System; State University of New York (SUNY) Stony Brook; Sungkyunkwan University (SKKU); University of Toronto; University of Alabama Tuscaloosa; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; University of Rochester; Uppsala University; University of Wuppertal; Helmholtz Association; Deutsches Elektronen-Synchrotron (DESY); University of TokyoIn the analysis published in 1, constraints on the number of signal events \(n_s\) can be interpreted as constraints on the volumetric neutrino to muon conversion rate \(\Lambda_{\nu\overline{\nu}\to\mu^{+}\mu{-}}\), \(\Lambda_{\nu\overline{\nu}\to\mu^{+}\mu{-}}^{90\%C.L.}\) = \(\frac{n_s^{90\%C.L.}}{\Sigma_jT_{live}^jV_{eff}^j}\), where \(T_{live}\) and \(V_{eff}\) are the livetime and effective volume of the data sample of index \(j\). These can then be interpreted as constraints on the muon flux \(\phi_{\mu^++\mu^-}\), dark matter (DM) annihilation rate in the Sun \(\Gamma_{\chi\chi\to SM}\), as well as the spindependent (SD) and spin-independent (SI) scattering cross sections \(\sigma_{SD}\) and \(\sigma_{SI}\) using WimpSim [2]. In Table 4 of Ref. [1], the labels and units of columns 7 and 8 suggest that the muon flux \(\phi_{\mu^++\mu^-}\) (in units km⁻² year⁻¹) is being presented. However for the first 12 rows, corresponding to points in which the DeepCore (DC) dataset was included, the volumetric neutrino to muon conversion rate \(\Lambda_{\nu\overline{\nu}\to\mu^{+}\mu{-}}\) (in units km⁻³ year⁻¹) were erroneously reported instead. The corrected table (Table 1) is presented hereby. All other columns remain unchanged. All quantities that go into the right hand side of Eq. 1 are presented in the table, as well as median sensitivities and 90% C.L. upper limits on themuon flux \(\phi_{\mu^++\mu^-}\) derived usingWimpSim[2]. The final results and conclusions presented in Ref. [1] in terms of constraints on theSDand SI scattering cross sections \(\sigma_{SD}\) and \(\sigma_{SI}\) as well as the DM annihilation rate in the Sun \(\Gamma_{\chi\chi\to SM}\), remain unchanged. In Section 4.2 of Ref. [1], themaximum zenith angle of the Sun is erroneously mentioned as 104°. The correct maximum zenith angle of the Sun is 114° at the South Pole.Item Search for dark matter annihilation in the Galactic Center with IceCube-79(Springer, 2015) IceCube Collaboration; Palczewski, T.; Pepper, J.A.; Toale, P.A.; Williams, D.R.; Xu, D.L.; Zarzhitsky, P.; RWTH Aachen University; University of Adelaide; University of Alaska System; University of Alaska Anchorage; Clark Atlanta University; University System of Georgia; Georgia Institute of Technology; Southern University System; Southern University & A&M College; University of California System; University of California Berkeley; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Humboldt University of Berlin; Ruhr University Bochum; University of Wurzburg; University of Bonn; Universite Libre de Bruxelles; Vrije Universiteit Brussel; Chiba University; University of Canterbury; University System of Maryland; University of Maryland College Park; University System of Ohio; Ohio State University; University of Copenhagen; Niels Bohr Institute; Dortmund University of Technology; Michigan State University; University of Alberta; University of Erlangen Nuremberg; University of Geneva; Ghent University; University of California Irvine; University of Kansas; University of Wisconsin System; University of Wisconsin Madison; Johannes Gutenberg University of Mainz; University of Mons; Technical University of Munich; University of Delaware; Yale University; University of Oxford; Drexel University; South Dakota School Mines & Technology; Oskar Klein Centre; Stockholm University; State University of New York (SUNY) System; State University of New York (SUNY) Stony Brook; Sungkyunkwan University (SKKU); University of Toronto; University of Alabama Tuscaloosa; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; Uppsala University; University of Wuppertal; Helmholtz Association; Deutsches Elektronen-Synchrotron (DESY)The Milky Way is expected to be embedded in a halo of dark matter particles, with the highest density in the central region, and decreasing density with the halo-centric radius. Dark matter might be indirectly detectable at Earth through a flux of stable particles generated in dark matter annihilations and peaked in the direction of the Galactic Center. We present a search for an excess flux of muon (anti-) neutrinos from dark matter annihilation in the Galactic Center using the cubic-kilometer-sized IceCube neutrino detector at the South Pole. There, the Galactic Center is always seen above the horizon. Thus, new and dedicated veto techniques against atmospheric muons are required to make the southern hemisphere accessible for IceCube. We used 319.7 live-days of data from IceCube operating in its 79-string configuration during 2010 and 2011. No neutrino excess was found and the final result is compatible with the background. We present upper limits on the self-annihilation cross-section, \(\langle \sigma_A \nu \rangle\), for WIMP masses ranging from 30 GeV up to 10 TeV, assuming cuspy (NFW) and flat-cored (Burkert) dark matter halo profiles, reaching down to \(\simeq 4 \cdot 10^{-24} cm^3 s^{-1}\), and \(\simeq 2.6 \cdot 10^{-23} cm^3 s^{-1}\) for the \(\upsilon{\overline{\upsilon}}\) channel, respectively.Item Search for Multimessenger Sources of Gravitational Waves and High-energy Neutrinos with Advanced LIGO during Its First Observing Run, ANTARES, and IceCube(IOP Publishing Ltd, 2019-01-10) ANTARES Collaboration; ANTARES Collaboration; IceCube Collaboration; IceCube Collaboration; LIGO Sci Collaboration; LIGO Sci Collaboration; Virgo Collaboration; Centre National de la Recherche Scientifique (CNRS); CNRS - National Institute of Nuclear and Particle Physics (IN2P3); UDICE-French Research Universities; Universites de Strasbourg Etablissements Associes; Universite de Strasbourg; Universitat Politecnica de Catalunya; Istituto Nazionale di Fisica Nucleare (INFN); Universitat Politecnica de Valencia; Aix-Marseille Universite; CEA; Universite Paris Cite; Universite Paris Saclay; Universite PSL; Observatoire de Paris; Consejo Superior de Investigaciones Cientificas (CSIC); CSIC - Instituto de Fisica Corpuscular (IFIC); University of Valencia; FOM National Institute for Subatomic Physics; Leiden University; Leiden University - Excl LUMC; Mohammed V University in Rabat; Institute of Space Science; University of Amsterdam; Sapienza University Rome; Gran Sasso Science Institute (GSSI); Cadi Ayyad University of Marrakech; University of Granada; Institut de Recherche pour le Developpement (IRD); Universite Cote d'Azur; Observatoire de la Cote d'Azur; University of Genoa; University of Erlangen Nuremberg; Mohammed First University of Oujda; University of Wurzburg; Universite Clermont Auvergne (UCA); Utrecht University; Royal Netherlands Institute for Sea Research (NIOZ); Institut Universitaire de France; Lomonosov Moscow State University; Universite de Haute-Alsace (UHA); University of Canterbury; Helmholtz Association; Deutsches Elektronen-Synchrotron (DESY); Universite Libre de Bruxelles; University of Copenhagen; Niels Bohr Institute; Oskar Klein Centre; Stockholm University; Marquette University; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; Massachusetts Institute of Technology (MIT); RWTH Aachen University; South Dakota School Mines & Technology; University of Geneva; University of Alberta; University of California System; University of California Irvine; Johannes Gutenberg University of Mainz; University of California Berkeley; University System of Ohio; Ohio State University; Ruhr University Bochum; University of Wuppertal; University of Rochester; University System of Maryland; University of Maryland College Park; University of Kansas; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Dortmund University of Technology; Uppsala University; University of Wisconsin System; University of Wisconsin Madison; University of Munster; Vrije Universiteit Brussel; University System of Georgia; Georgia Institute of Technology; Michigan State University; University of Delaware; Ghent University; Humboldt University of Berlin; Sungkyunkwan University (SKKU); Southern University System; Southern University & A&M College; Technical University of Munich; University of Adelaide; University of Tokyo; Chiba University; Clark Atlanta University; University of Texas System; University of Texas Arlington; State University of New York (SUNY) System; State University of New York (SUNY) Stony Brook; University of Alabama Tuscaloosa; Drexel University; Yale University; University of Alaska System; University of Alaska Anchorage; University of Oxford; University of California Los Angeles; California Institute of Technology; Louisiana State University System; Louisiana State University; Inter-University Centre for Astronomy & Astrophysics; University of Salerno; Monash University; Max Planck Society; Leibniz University Hannover; University of Cambridge; University of Birmingham; Instituto Nacional de Pesquisas Espaciais (INPE); Tata Institute of Fundamental Research (TIFR); International Centre for Theoretical Sciences, Bengaluru; University of Illinois System; University of Illinois Urbana-Champaign; University of Pisa; Australian National University; University of Wisconsin Milwaukee; University of Strathclyde; California State University System; California State University Fullerton; Chennai Mathematical Institute; University of Rome Tor Vergata; Communaute Universite Grenoble Alpes; Universite Grenoble Alpes (UGA); Embry-Riddle Aeronautical University; Montclair State University; Korea Institute of Science & Technology Information (KISTI); West Virginia University; University of Perugia; Syracuse University; University of Minnesota System; University of Minnesota Twin Cities; University of Glasgow; Eotvos Lorand Research Network; Hungarian Academy of Sciences; Hungarian Wigner Research Centre for Physics; State University System of Florida; University of Florida; Stanford University; University of Camerino; University of Padua; Polish Academy of Sciences; Nicolaus Copernicus Astronomical Center of the Polish Academy of Sciences; Friedrich Schiller University of Jena; Rochester Institute of Technology; Northwestern University; Raja Ramanna Centre for Advanced Technology; University of Western Australia; Radboud University Nijmegen; University of Zurich; CNRS - Institute for Engineering & Systems Sciences (INSIS); Universite de Rennes; Cardiff University; Washington State University; University of Oregon; College de France; Ecole Normale Superieure (ENS); Sorbonne Universite; University of Urbino; University of Warsaw; Vrije Universiteit Amsterdam; Universite Claude Bernard Lyon 1; University of Naples Federico II; National Aeronautics & Space Administration (NASA); NASA Goddard Space Flight Center; Tsinghua University; Texas Tech University System; Texas Tech University; University of Mississippi; National Tsing Hua University; Charles Sturt University; University of Chicago; Chinese University of Hong Kong; Seoul National University (SNU); Pusan National University; Carleton College; Istituto Nazionale Astrofisica (INAF); University of Melbourne; Columbia University; Universitat de les Illes Balears; Sonoma State University; Montana State University System; Montana State University Bozeman; University of Rhode Island; University of Texas Rio Grande Valley; Institute for Plasma Research (IPR); University of Sheffield; California State University Los Angeles; University of Trento; Colorado State University; Kenyon College; National Institutes of Natural Sciences (NINS) - Japan; National Astronomical Observatory of Japan (NAOJ); University of Toronto; University of Edinburgh; Indian Institute of Technology System (IIT System); Indian Institute of Technology (IIT) - Bombay; Szeged University; University of Michigan System; University of Michigan; American University; University of Bialystok; University of London; King's College London; University of Southampton; University of Washington; University of Washington Bothell; Russian Academy of Sciences; Institute of Applied Physics of the Russian Academy of Sciences; Ewha Womans University; Inje University; National Institute for Mathematical Sciences (NIMS), Republic of Korea; Ulsan National Institute of Science & Technology (UNIST); University of Hamburg; Maastricht University; National Centre for Nuclear Research; Institute of Mathematics of the Polish Academy of Sciences; Cornell University; Hillsdale College; Hanyang University; Korea Astronomy & Space Science Institute (KASI); Roma Tre University; Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI); Swinburne University of Technology; University of Portsmouth; William & Mary; Indian Institute of Technology (IIT) - Madras; Indian Institute of Science Education & Research (IISER) - Kolkata; Whitman College; University of Zielona Gora; University of Washington Seattle; University of West Scotland; Universite de Montreal; Polytechnique Montreal; Indian Institute of Technology (IIT) - Gandhinagar; Indian Institute of Technology (IIT) - Hyderabad; Universidade Federal do Rio Grande do Norte; Villanova University; Andrews University; University of Siena; Trinity University; University of GroningenAstrophysical sources of gravitational waves, such as binary neutron star and black hole mergers or core-collapse supernovae, can drive relativistic outflows, giving rise to non-thermal high-energy emission. High-energy neutrinos are signatures of such outflows. The detection of gravitational waves and high-energy neutrinos from common sources could help establish the connection between the dynamics of the progenitor and the properties of the outflow. We searched for associated emission of gravitational waves and high-energy neutrinos from astrophysical transients with minimal assumptions using data from Advanced LIGO from its first observing run O1, and data from the ANTARES and IceCube neutrino observatories from the same time period. We focused on candidate events whose astrophysical origins could not be determined from a single messenger. We found no significant coincident candidate, which we used to constrain the rate density of astrophysical sources dependent on their gravitational-wave and neutrino emission processes.Item Search for neutrinos from dark matter self-annihilations in the center of the Milky Way with 3 years of IceCube/DeepCore(Springer, 2017) IceCube Collaboration; Kopper, S.; Nakarmi, P.; Pepper, J.A.; Toale, P.A.; Williams, D.R.; RWTH Aachen University; University of Adelaide; University of Alaska System; University of Alaska Anchorage; University of Texas System; University of Texas Arlington; Clark Atlanta University; University System of Georgia; Georgia Institute of Technology; Southern University System; Southern University & A&M College; University of California System; University of California Berkeley; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Humboldt University of Berlin; Ruhr University Bochum; University of Wurzburg; Universite Libre de Bruxelles; Vrije Universiteit Brussel; Massachusetts Institute of Technology (MIT); Chiba University; University of Canterbury; University System of Maryland; University of Maryland College Park; University System of Ohio; Ohio State University; University of Copenhagen; Niels Bohr Institute; Dortmund University of Technology; Michigan State University; University of Alberta; University of Erlangen Nuremberg; University of Geneva; Ghent University; University of California Irvine; University of Kansas; University of Wisconsin System; University of Wisconsin Madison; Johannes Gutenberg University of Mainz; Marquette University; University of Mons; Technical University of Munich; University of Munster; University of Delaware; Yale University; University of Oxford; Drexel University; South Dakota School Mines & Technology; University of Rochester; Oskar Klein Centre; Stockholm University; State University of New York (SUNY) System; State University of New York (SUNY) Stony Brook; Sungkyunkwan University (SKKU); University of Alabama Tuscaloosa; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; Uppsala University; University of Wuppertal; Helmholtz Association; Deutsches Elektronen-Synchrotron (DESY); University of TokyoWe present a search for a neutrino signal from dark matter self-annihilations in the Milky Way using the IceCube Neutrino Observatory (IceCube). In 1005 days of data we found no significant excess of neutrinos over the background of neutrinos produced in atmospheric air showers from cosmic ray interactions. We derive upper limits on the velocity averaged product of the dark matter self-annihilation cross section and the relative velocity of the dark matter particles \(\langle \sigma_A v\rangle\). Upper limits are set for dark matter particle candidate masses ranging from 10 GeV up to 1 TeV while considering annihilation through multiple channels. This work sets the most stringent limit on a neutrino signal from dark matter with mass between 10 and 100 GeV, with a limit of 1.18 · 10⁻²³ cm³ s⁻¹ for 100 GeV dark matter particles self-annihilating via τ⁺τ⁻ to neutrinos (assuming the Navarro-Frenk-White dark matter halo profile).Item Search for non-relativistic magnetic monopoles with IceCube: IceCube Collaboration (vol 74, 2938, 2014)(Springer, 2019-02-08) IceCube Collaboration; RWTH Aachen University; University of Adelaide; University of Alaska System; University of Alaska Anchorage; Clark Atlanta University; University System of Georgia; Georgia Institute of Technology; Southern University System; Southern University & A&M College; University of California System; University of California Berkeley; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Humboldt University of Berlin; Ruhr University Bochum; University of Wurzburg; University of Bonn; Universite Libre de Bruxelles; Vrije Universiteit Brussel; Chiba University; University of Canterbury; University System of Maryland; University of Maryland College Park; University System of Ohio; Ohio State University; University of Copenhagen; Niels Bohr Institute; Dortmund University of Technology; University of Alberta; University of Erlangen Nuremberg; University of Geneva; Ghent University; University of California Irvine; University of Kansas; University of Wisconsin System; University of Wisconsin Madison; Johannes Gutenberg University of Mainz; University of Mons; Technical University of Munich; University of Delaware; University of Oxford; Oskar Klein Centre; Stockholm University; State University of New York (SUNY) System; State University of New York (SUNY) Stony Brook; Sungkyunkwan University (SKKU); University of Toronto; University of Alabama Tuscaloosa; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; Uppsala University; University of Wuppertal; Helmholtz Association; Deutsches Elektronen-Synchrotron (DESY); South Dakota School Mines & Technology; University of Tokyo; National Aeronautics & Space Administration (NASA); NASA Goddard Space Flight CenterIn the analyses, published in Ref. [1], the exclusion limits are calculated in dependence of the mean free path of the magnetic monopole - nucleon catalysis interaction.Item Search for steady point-like sources in the astrophysical muon neutrino flux with 8 years of IceCube data(Springer, 2019) IceCube Collaboration; Kopper, S.; Nakarmi, P.; Santander, M.; Williams, D.R.; RWTH Aachen University; University of Adelaide; University of Alaska System; University of Alaska Anchorage; University of Texas System; University of Texas Arlington; Clark Atlanta University; University System of Georgia; Georgia Institute of Technology; Southern University System; Southern University & A&M College; University of California System; University of California Berkeley; United States Department of Energy (DOE); Lawrence Berkeley National Laboratory; Humboldt University of Berlin; Ruhr University Bochum; University of Wurzburg; Universite Libre de Bruxelles; Vrije Universiteit Brussel; Massachusetts Institute of Technology (MIT); Chiba University; University of Canterbury; University System of Maryland; University of Maryland College Park; University System of Ohio; Ohio State University; University of Copenhagen; Niels Bohr Institute; Dortmund University of Technology; Michigan State University; University of Alberta; University of Erlangen Nuremberg; University of Geneva; Ghent University; University of California Irvine; University of Kansas; University of California Los Angeles; University of Wisconsin System; University of Wisconsin Madison; Johannes Gutenberg University of Mainz; Marquette University; Technical University of Munich; University of Munster; University of Delaware; Yale University; University of Oxford; Drexel University; South Dakota School Mines & Technology; University of Rochester; Oskar Klein Centre; Stockholm University; State University of New York (SUNY) System; State University of New York (SUNY) Stony Brook; Sungkyunkwan University (SKKU); University of Alabama Tuscaloosa; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; Uppsala University; University of Wuppertal; Helmholtz Association; Deutsches Elektronen-Synchrotron (DESY); University of TokyoThe IceCube Collaboration has observed a high-energy astrophysical neutrino flux and recently found evidence for neutrino emission from the blazar TXS 0506 \(+\) 056. These results open a new window into the high-energy universe. However, the source or sources of most of the observed flux of astrophysical neutrinos remains uncertain. Here, a search for steady point-like neutrino sources is performed using an unbinned likelihood analysis. The method searches for a spatial accumulation of muon-neutrino events using the very high-statistics sample of about 497,000 neutrinos recorded by IceCube between 2009 and 2017. The median angular resolution is \(\sim {1}^{\circ }\) at 1 TeV and improves to \(\sim 0.{3}^{\circ }\) for neutrinos with an energy of 1 PeV. Compared to previous analyses, this search is optimized for point-like neutrino emission with the same flux-characteristics as the observed astrophysical muon-neutrino flux and introduces an improved event-reconstruction and parametrization of the background. The result is an improvement in sensitivity to the muon-neutrino flux compared to the previous analysis of \(\sim 35%\) assuming an \({E}^{-2}\) spectrum. The sensitivity on the muon-neutrino flux is at a level of \({E}^{2}dN/dE=3·{10}^{-13}\phantom{\rule{0.166667em}{0ex}}\mathrm{TeV}\phantom{\rule{0.166667em}{0ex}}{\mathrm{cm}}^{-2}\phantom{\rule{0.166667em}{0ex}}{s}^{-1}\). No new evidence for neutrino sources is found in a full sky scan and in an a priori candidate source list that is motivated by gamma-ray observations. Furthermore, no significant excesses above background are found from populations of sub-threshold sources. The implications of the non-observation for potential source classes are discussed.