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Particle Physics with Icecube-Deepcore and Beyond

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Particle physics with IceCube-DeepCore and beyond Darren R. Grant (for the IceCube Collaboration) Department of Physics, Centre for Particle Physics University of Alberta Winter Nuclear and Particle Physics Conference 2012 Mont Tremblant Quebec The Neutrino Detector Spectrum NOνA OPERA Accelerator MINOS K2K, T2K Energy ↔ Volume 10 MeV 100 MeV 1 GeV 10 GeV 100 GeV 1 TeV 10 TeV 1 EeV Solar/ Atmospheric/Astrophysical Reactor Atmospheric Borexino/KamLand/Daya Bay/Double AMANDA/ANTRES/IceCube/KM3Net/ Chooz/SNO/SuperK ANITA/RICE/Auger/ARIANNA Non-accelerator based * boxes select primary detector physics energy regimes and are not absolute limits February 24, 2012 WNPPC Darren R. Grant - University of Alberta Multimessenger Astronomy cosmic rays + neutrinos p π± ν 0 π γ p e± γ cosmic rays + gamma-rays γ Gamma rays and ν neutrinos should be produced at the sites of cosmic ray acceleration p The IceCube Neutrino Observatory Completed December 18, 2010 8 February 24, 2012 WNPPC Darren R. Grant - University of Alberta Universite Libre de Bruxelles University of Alberta Vrije Universiteit Brussel Universite de Mons-Hainaut Uppsala University Universiteit Gent Stockholm Universtiy Universitat Mainz Oxford University Humboldt Univ., Berlin DESY, Zeuthen Univ. Alabama, Tuscaloosa EPFL, Lausanne Universitat Dortmund Univ. Alaska, Anchorage University of Geneva Universitat Wuppertal Chiba University UC Berkeley University of West Indies MPI Heidelberg UC Irvine RWTH Aachen Clark-Atlanta University Universitat Bonn U. Delaware/Bartol Research Inst. Ruhr-Universitat Bochum Georgia Tech University of Kansas Lawrence Berkeley National Lab University of Maryland Ohio State University University of Adelaide Pennsylvania State University University of Wisconsin-Madison University of Wisconsin-River Falls University of Canterbury, ChristChurch Southern University, Baton Rouge Stony Brook University The IceCube Collaboration 38 institutions - 4 continents - ~250 Physicists February 24, 2012 WNPPC Darren R. Grant - University of Alberta IceCube Amundsen-Scott South Pole Station, Antarctica February 24, 2012 WNPPC Darren R. Grant - University of Alberta The Digital Optical Module (DOM) February 24, 2012 WNPPC Darren R. Grant - University of Alberta Neutrino Telescopes - Principle of Detection Tracks: • through-going muons • pointing resolution ~1° Candidate IC79 Cascade Cascades: • Neutral current for all flavors • Charged current for νe and low-E ντ • Energy resolution ~10% in log(E) Composites: • Starting tracks • high-E ντ (Double Bangs) •Good directional and energy resolution LED Calibration event simulating a double-bang February 24, 2012 WNPPC Darren R. Grant - University of Alberta The IceCube Neutrino Observatory - A Wealth of Science... AGNs, p+ accelerators GRBs γ γ Diffuse Sources χχ + Advances in Point Sources Glaciology χ Dark Matter Supernovae GZK/UHE Cosmic Rays/Atm. Neutrinos/Exotics February 24, 2012 WNPPC Darren R. Grant - University of Alberta Identify and reconstruct your best candidates (IceCube 40-string Detector) • Operated for 375.5 days • Northern sky - 14139 events • Southern sky - 23151 events • Search for clustering of events in direction and energy. February 24, 2012 WNPPC Darren R. Grant - University of Alberta Perform the Point Source Search (IceCube 40-strings) • Search for an excess of astrophysical neutrinos from a common direction over the atmospheric neutrino background • All sky search with >37K neutrino candidates (~23k from southern hemisphere atmospheric neutrinos • Hottest spot in the 40-string data set was not statistically significant (96% of scrambled sky maps have higher significance) February 24, 2012 WNPPC Darren R. Grant - University of Alberta Most Recently from IceCube Point Source Searches... February 24, 2012 WNPPC Darren R. Grant - University of Alberta The Neutrino Detector Spectrum NOνA OPERA Accelerator MINOS K2K, T2K Energy ↔ Volume 10 MeV 100 MeV 1 GeV 10 GeV 100 GeV 1 TeV 10 TeV 1 EeV Solar/ Atmospheric/Astrophysical Reactor Atmospheric Borexino/KamLand/Daya Bay/Double AMANDA/ANTRES/IceCube/KM3Net/ Chooz/SNO/SuperK ANITA/RICE/Auger/ARIANNA Non-accelerator based * boxes select primary detector physics energy regimes and are not absolute limits February 24, 2012 WNPPC Darren R. Grant - University of Alberta The Neutrino Detector Spectrum NOνA OPERA Accelerator MINOS K2K, T2K Energy ↔ Volume 10 MeV 100 MeV 1 GeV 10 GeV 100 GeV 1 TeV 10 TeV 1 EeV Solar/ Atmospheric Atmospheric/Astrophysical Reactor Gap Borexino/KamLand/Daya Bay/Double AMANDA/ANTRES/IceCube/KM3Net/ Chooz/SNO/SuperK ANITA/RICE/Auger/ARIANNA Dark Matter ντ Appearance Non-accelerator based νμ Neutrino Disappearance Mass Hierarchy * boxes select primary detector physics energy regimes and are not absolute limits February 24, 2012 WNPPC Darren R. Grant - University of Alberta IceCube February 24, 2012 WNPPC Darren R. Grant - University of Alberta IceCube February 24, 2012 WNPPC Darren R. Grant - University of Alberta IceCube-DeepCore February 24, 2012 WNPPC Darren R. Grant - University of Alberta IceCube-DeepCore • IceCube extended its “low” energy response with a densely instrumented infill array: DeepCore http://arxiv.org/abs/1109.6096 • Significant improvement in capabilities from ~10 GeV to ~300 GeV (νμ) • Scientific Motivations: • Indirect search for dark matter • Neutrino oscillations (e.g., ντ appearance) • Neutrino point sources in the southern hemisphere (e.g., galactic center) February 24, 2012 WNPPC Darren R. Grant - University of Alberta DeepCore Design • Eight special strings plus seven scattering nearest standard IceCube strings • 72 m inter-string horizontal spacing (six with 42 m spacing) IceCube • 7 m DOM vertical spacing extra • ~35% higher Q.E. PMTs veto cap • ~5x higher effective photocathode density AMANDA • Deployed mainly in the clearest ice, below 2100 m Deep Core 350 m • λeff > ~50 m • Result: 30 MTon detector with 250 m ~10 GeV threshold, will collect O(100k) physics quality atmospheric ν/yr February 24, 2012 WNPPC Darren R. Grant - University of Alberta DeepCore Effective Area and Volume 300 m Physical Deep Core Volume 400 m ~28 MT 200 DeepCore Trigger Effective area for νμ at trigger level DeepCore Online Filter IceCube Trigger w/o DC Megaton Reconstruction efficiencies not included 150 yet – relative effect likely to increase ) 2 IceCube Trigger w/o DeepCore 10 DeepCore+IceCube Trigger DeepCore Online Filter 100 1 10-1 Effective Area (m 50 10-2 10-3 0 -4 1.0 1.5 2.0 2.5 3.0 10 νµ Energy (Log10 GeV) 10-5 Effective volume for muons from νμ interacting in Deep Core 10-6 1.0 1.5 2.0 2.5 3.0 3.5 4.0 Log (ν Energy - GeV) 10 µ NB: full analysis efficiency not included yet Trigger: ≥3 DOMs hit in 2.5µs; Online Veto: No hits consistent with muons outside DeepCore volume February 24, 2012 WNPPC Darren R. Grant - University of Alberta DeepCore Atmospheric Muon Veto • Overburden of 2.1 km water- equivalent is substantial, but not as large as at deep underground labs • However, top and outer layers of IceCube provide an active veto IceCube shield for DeepCore extra • ~40 horizontal layers of modules veto cap above; 3 rings of strings on all sides • Effective μ-free depth much greater AMANDA • Can use to distinguish atmospheric μ from atmospheric or cosmological ν Deep Core • Atm. μ/ν trigger ratio is ~106 350 m • Vetoing algorithms expected to reach at least 106 level of background 250 m rejection February 24, 2012 WNPPC Darren R. Grant - University of Alberta First from DeepCore - Observation of Atmospheric Cascades • Disappearing νμ should appear in IceCube as ντ cascades Mena, Mocioiu & Razzaque, Phys. Rev. D78, 093003 (2008) • Effectively identical to neutral νµ→ νµ current or νe CC events 1.0 νµ→ ντ • Could observe ντ appearance 0.8 as a distortion of the energy ντ appearance spectrum, if cascades can be 0.6 separated from muon Oscillation Probabilities background 0.4 νµ disappearance 0.2 0.0 10 20 30 40 50 Neutrino Energy (GeV) February 24, 2012 WNPPC Darren R. Grant - University of Alberta First from DeepCore - Observation of Atmospheric Cascades • Disappearing νμ should appear in IceCube as ντ cascades Preliminary • Effectively identical to neutral current or νe CC events • Could observe ντ appearance as a distortion of the energy spectrum, if cascades can be separated from muon background • First results from DeepCore are neutrino cascade events • The dominant background now is CC νμ events with short tracks February 24, 2012 WNPPC Darren R. Grant - University of Alberta First from DeepCore - Observation of Atmospheric Cascades • A substantial sample of cascades has been obtained, final data set ~60% cascade events • Events have a mean energy ~200 GeV (not sensitive to oscillations with these first cuts) • Atmospheric muon background is being assessed (expected to be small) • The potential to discriminate between atmospheric neutrino models exists and thus measuring air shower physics February 24, 2012 WNPPC Darren R. Grant - University of Alberta Muon-neutrino disappearance • Full detector simulation of signal • 3-flavor oscillations, PREM • 1 year DC • No BG • cos(θ)<-0.6 • Number of hit channels used as simple energy estimator February 24, 2012 WNPPC Darren R. Grant - University of Alberta Indirect Dark Matter Searches χ • Search for neutrinos produced in the annihilation of dark matter collected in massive astrophysical objects (Sun, centre of Earth...) • Resultant neutrino energies of order GeV - TeV. atm μ atm ν νμ μ Krauss, Srednicki & Wilczek, ’86 Silk, Olive and Srednicki, ’85 atm μ Gaisser, Steigman & Tilav,
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  • Status of Neutrino Oscillations I: the Three-Neutrino Scenario

    Status of Neutrino Oscillations I: the Three-Neutrino Scenario

    International Workshop on Astroparticle and High Energy Physics PROCEEDINGS Status of neutrino oscillations I: the three-neutrino scenario Michele Maltoni∗ IFIC, CSIC/Universitat de Val`encia, Apt 22085, E{46071 Valencia, Spain YITP, SUNY at Stony Brook, Stony Brook, NY 11794-3840, USA E-mail: [email protected] Abstract: We present a global analysis of neutrino oscillation data within the three- neutrino oscillation scheme, including in our fit all the current solar neutrino data, the reactor neutrino data from KamLAND and CHOOZ, the atmospheric neutrino data from Super-Kamiokande and MACRO, and the first data from the K2K long-baseline accel- erator experiment. We determine the current best fit values and allowed ranges for the three-flavor oscillation parameters, discussing the relevance of each individual data set as well as the complementarity of different data sets. Furthermore, we analyze in detail the 2 2 status of the small parameters θ13 and ∆m21=∆m31, which fix the possible strength of CP violating effects in neutrino oscillations. Keywords: Neutrino mass and mixing; solar, atmospheric, reactor and accelerator neutrinos. 1. Introduction Recently, the Sudbury Neutrino Observatory (SNO) experiment [1] has released an im- proved measurement with enhanced neutral current sensitivity due to neutron capture on salt, which has been added to the heavy water in the SNO detector. This adds precious information to the large amount of data on neutrino oscillations published in the last few years. Thanks to this growing body of data a rather clear picture of the neutrino sector is starting to emerge. In particular, the results of the KamLAND reactor experiment [2] have played an important role in confirming that the disappearance of solar electron neu- trinos [3, 4, 5, 6, 7], the long-standing solar neutrino problem, is mainly due to oscillations and not to other types of neutrino conversions.