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Particle Physics in Ice with Icecube Deepcore

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Particle Physics in Ice with IceCube DeepCore Tyce DeYoung Department of Physics Pennsylvania State University for the IceCube Collaboration RICAP ’11 Rome, Italy May 25, 2011 The Neutrino Detector Spectrum Accelerator-based Energy ↔ Volume 10 MeV 100 MeV 1 GeV 10 GeV 100 GeV 1 TeV 10 TeV 1 EeV Atmospheric/Astrophysical The Neutrino Detector Spectrum Accelerator-based Energy ↔ Volume 10 MeV 100 MeV 1 GeV 10 GeV 100 GeV 1 TeV 10 TeV 1 EeV SNO, Borexino, KamLAND, Super-K Double CHOOZ, Daya Bay, etc. Atmospheric/Astrophysical The Neutrino Detector Spectrum NOνA OPERA Accelerator-based K2K, MINOS T2K ↔ MiniBooNE Energy Volume 10 MeV 100 MeV 1 GeV 10 GeV 100 GeV 1 TeV 10 TeV 1 EeV SNO, Borexino, KamLAND, Super-K Double CHOOZ, Daya Bay, etc. Atmospheric/Astrophysical The Neutrino Detector Spectrum NOνA OPERA Accelerator-based K2K, MINOS T2K ↔ MiniBooNE Energy Volume 10 MeV 100 MeV 1 GeV 10 GeV 100 GeV 1 TeV 10 TeV 1 EeV ANITA, SNO, Borexino, AMANDA, Baikal, RICE, Auger, Super-K KamLAND, ANTARES IceCube, KM3NeT ARIANNA,... Double CHOOZ, Daya Bay, etc. Atmospheric/Astrophysical The Neutrino Detector Spectrum NOνA OPERA Accelerator-based K2K, MINOS T2K ↔ MiniBooNE Energy Volume 10 MeV 100 MeV 1 GeV 10 GeV 100 GeV 1 TeV 10 TeV 1 EeV ANITA, SNO, Borexino, AMANDA, Baikal, RICE, Auger, Super-K KamLAND, ANTARES IceCube, KM3NeT ARIANNA,... Double CHOOZ, Gap Daya Bay, etc. Atmospheric/Astrophysical The Neutrino Detector Spectrum NOνA OPERA Accelerator-based K2K, MINOS T2K ↔ MiniBooNE Energy Volume 10 MeV 100 MeV 1 GeV 10 GeV 100 GeV 1 TeV 10 TeV 1 EeV ANITA, SNO, Borexino, AMANDA, Baikal, RICE, Auger, Super-K KamLAND, ANTARES IceCube, KM3NeT ARIANNA,... Double CHOOZ, Gap Daya Bay, etc. Atmospheric/Astrophysical Gamma Ray Bursts Neutrino Oscillations Soft Galactic Dark Cosmic Ray Matter Accelerators The Neutrino Detector Spectrum NOνA OPERA Accelerator-based K2K, MINOS T2K ↔ MiniBooNE Energy Volume 10 MeV 100 MeV 1 GeV 10 GeV 100 GeV 1 TeV 10 TeV 1 EeV ANITA, SNO, Borexino, AMANDA, Baikal, RICE, Auger, Super-K KamLAND, DeepCore ANTARES IceCube, KM3NeT ARIANNA,... Double CHOOZ, Daya Bay, etc. Atmospheric/Astrophysical Gamma Ray Bursts Neutrino Oscillations Soft Galactic Dark Cosmic Ray Matter Accelerators IceCube DeepCore • IceCube collaboration decided to augment “low” energy response with a densely instrumented infill array: DeepCore • Significant improvement in capabilities from ~10 GeV to ~100 GeV (νμ) • Primary scientific rationale is the indirect search for dark matter • Particle physics using atmospheric neutrinos • Neutrino oscillations, including tau neutrino appearance • Neutrino sources in Southern Hemisphere • Galactic cosmic ray accelerators, dark matter in the Galactic center • Neutrino astronomy at low energies (e.g. GRBs) Tyce DeYoung RICAP ’11 May 25, 2011 Overhead View 2010 configuration IceCube DeepCore DeepCore • DeepCore extends the reach of IceCube to lower energies • Denser module spacing scattering • Hamamatsu super-bialkali PMTs IceCube Strings HQE DeepCore Strings DeepCore Infill Strings (Mix of HQE and • Deployed in the clearest ice normal DOMs) DeepCore strings have Side View 10 DOMs with a DOM-to-DOM spacing of 10 meters Dust Layer 50 HQE DOMs with an DOM-to-DOM spacing of 7 meters 21 Normal DOMs with a DOM-to-DOM spacing of 17 meters Overhead View 2010final configurationconfiguration IceCube DeepCore DeepCore • DeepCore extends the reach of IceCube to lower energies • Denser module spacing scattering • Hamamatsu super-bialkali PMTs IceCube Strings HQE DeepCore Strings DeepCore Infill Strings (Mix of HQE and • Deployed in the clearest ice normal DOMs) DeepCore strings have Side View 10 DOMs with a DOM-to-DOM spacing of 10 meters Dust Layer 50 HQE DOMs with an DOM-to-DOM spacing of 7 meters 21 Normal DOMs with a DOM-to-DOM spacing of 17 meters Online Atmospheric Muon Veto • Look for hits in veto region consistent with speed-of-light travel time to hits in DeepCore • Achieves 7 x 10-3 rejection of cosmic ray muon background • Loss of <2% of fiducial neutrinos Preliminary (Monte Carlo) speed of light (inward) speed of light (outward) cosmic ray muons neutrinos DeepCore Lepton Effective Volume 200 200 DeepCore Trigger DeepCore Trigger DeepCore Online Filter DeepCore Online Filter IceCube Trigger w/o DC IceCube Trigger w/o DC Megaton Megaton 150 150 300 m 100 Physical 100 Deep Core Volume 400 m ~28 MT 50 50 νe νμ 0 0 1.0 1.5 2.0 2.5 3.0 1.0 1.5 2.0 2.5 3.0 !e Energy (Log10 GeV) !µ Energy (Log10 GeV) • Many DeepCore triggers are events occurring in the rest of IceCube • These events are rejected by the online veto algorithm • Online efficiency for neutrinos interacting in the DeepCore volume is >98% • Efficiency in final analysis will be significantly lower; losses to reconstruction efficiency, background rejection DeepCore Neutrino Effective Area ) ) 2 2 IceCube Trigger w/o DeepCore IceCube Trigger w/o DeepCore 10 DeepCore+IceCube Trigger 10 DeepCore+IceCube Trigger DeepCore Online Filter DeepCore Online Filter 1 1 10-1 10-1 Effective Area (m Effective Area (m 10-2 10-2 10-3 10-3 10-4 10-4 νe νμ 10-5 10-5 10-6 10-6 1.0 1.5 2.0 2.5 3.0 3.5 4.0 1.0 1.5 2.0 2.5 3.0 3.5 4.0 Log (! Energy - GeV) Log (! Energy - GeV) 10 e 10 µ • DeepCore dominates total response for Eν below ~100 GeV, depending on flavor • Improved trigger efficiency overcomes much smaller volume • Linear growth at high energies reflects neutrino interaction cross section, not detector efficiency Neutrino Astronomy with DeepCore • Atmospheric neutrino veto • May allow observation of sources in the Southern hemisphere with fluxes too low to be seen above atmospheric background (Schönert et al. 2009) • Sensitivity to low energy neutrinos from transients • E.g. choked or magnetically atm. ν dominated GRBs (e.g., Ando & Beacom 2005; possible source with veto Razzaque, Meszaros & spectrum Waxman 2005; Meszaros & Rees 2011) Tyce DeYoung RICAP ’11 May 25, 2011 Sensitivity to MSSM WIMPs 0.05 < 1 h2 < 0.20 MSSM model scan -31 r ) 2 10 m < mlim CDMS(2010)+XENON100(2010) CDMS (2010) • Solar WIMP SI SI COUPP (2008) -32 m < 0.001xmlim CDMS(2010)+XENON100(2010) 10 SI SI KIMS (2007) dark matter IceCube (bb) Picasso (2009) + - + - SUPER-K 1996-2001 -33 IceCube (W W , o o for m] < mW = 80.4GeV) 10 + - + - searches probe IC80+DC6 sens.(180d) (W W , o o for m] < mW = 80.4GeV) *IceCube PRELIMINARY* SD scattering 10-34 cross section 10-35 -36 • SI cross section 10 Direct Detection Experiments 10-37 constrained well Super-K IceCube soft spectrum by direct search 10-38 experiments 10-39 IceCube hard spectrum Neutralino-proton SD cross-section (cm -40 10 IceCube+DeepCore hard spectrum(prelim.) sensitivity • DeepCore will -41 10 ( Lines are to Allowed probe large guide the eye ) MSSM models 10-42 10 102 103 104 region of Neutralino mass (GeV) allowed phase space Corresponding σSI more than factor Corresponding σSI within factor 103 beyond current direct limits 103 of current direct limits Mena, Mocioiu & Razzaque, Phys. Rev. D78, 093003 (2008) Neutrino Oscillations ντ appearance • Atmospheric neutrinos from Northern Hemisphere oscillating νμ disappearance over one earth diameter have νμ oscillation minimum at ~25 GeV L = D⊕ • Higher energy region than accelerator-based experiments 1400 Preliminary Unoscillated 1200 Oscillated • Plot of νμ disappearance shows No Reconstruction 1000 "23 = !/2 only simulated signal 2 -3 $m23 = 2.4 # 10 eV 800 Events/NChannel/Year Cos(zenith) < -0.6 • Analysis efficiencies not 600 included yet – work ongoing 400 • Uses number of hit DOMs as 200 a simple energy estimator 0 0 10 20 30 40 50 60 70 80 90 100 NChannels [Hit DOMs] Tyce DeYoung RICAP ’11 May 25, 2011 Observation of Neutrino Cascades (Preliminary) • Disappearing νμ should appear in IceCube as ντ cascades • 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 • We believe we see neutrino cascade events for the first time • The dominant background now Candidate cascade event is CC νμ events with short tracks Run 116020, Event 20788565, 2010/06/06 Tyce DeYoung RICAP ’11 May 25, 2011 Observation of Neutrino Cascades (Preliminary) • With harsh cuts to eliminate the νμ Data from 10% Preliminary background we “open” sample expect to obtain a Rate (mHz) sample of ~800 Rate (per year) neutrino cascades Sum of all MCs per year • Approximately 500 νe + νμ NC (~800 / year) background νμ CC νμ CC events expected Corsika (no events in current sample) • Contamination from Jun. 2010 Aug. 2010 Oct. 2010 Dec. 2010 Feb. 2011 atmospheric muons Month still being evaluated • Efforts to increase νe yield and reduce νμ CC background ongoing Tyce DeYoung RICAP ’11 May 25, 2011 Observation of Neutrino Cascades (Preliminary) • With harsh cuts to eliminate the νμ Data from 10% Preliminary background we “open” sample expect to obtain a Rate (mHz) sample of ~800 Rate (per year) neutrino cascades Sum of all MCs per year “Anything worth doing” • Approximately 500 νe + νμ NC (~800 / year) background νμ CC is worthνμ CCoverdoing events expected Corsika (no events in current sample) • Contamination from Jun. 2010 Aug. 2010 Oct. 2010 Dec. 2010 Feb. 2011 atmospheric muons Month still being evaluated • Efforts to increase νe yield and reduce νμ CC background ongoing Tyce DeYoung RICAP ’11 May 25, 2011 Beyond DeepCore: PINGU • Now developing a proposal one possible geometry to continue to instrument the New PINGU DeepCore volume Strings • An additional 18-20 strings, 1000-1200 DOMs • Make use of well-established IceCube drilling technology • Might get to a threshold Existing standard of ~1 GeV in a ~10 MTon Existing IceCube DeepCore volume strings Strings • Also an R&D platform for future detectors on a ~decade timeline • Price tag expected to be around $25M – $30M Tyce DeYoung RICAP ’11 May 25, 2011 R&D: Multi-PMT Digital Optical Module Courtesy E.
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    Elsevier Science 1 Journal logo IceCube and KM3NeT: Lessons and Relations Christian Spiering DESY, Platanenallee 6, Zeuthen, 15738 Germany Elsevier use only: Received date here; revised date here; accepted date here Abstract This talk presents conclusions for KM3NeT which may be drawn from latest IceCube results and from optimization studies of the IceCube configuration. It discusses possible coordinated efforts between IceCube and KM3NeT (or, for the time being, IceCube and ANTARES). Finally, it lists ideas for formal relations between neutrino telescopes on the cubic kilometer scale. © 2001 Elsevier Science. All rights reserved Keywords: Neutrino Telescopes 1. Introduction The IceCube neutrino telescope at the South Pole Assuming one detector on the Southern is approaching its completion and meanwhile has hemisphere (IceCube) and one or more detectors at provided first results from data taken with initial the Northern hemisphere (by now ANTARES [10] configurations [1]. KM3NeT will act as IceCube’s and NT200 [11], in the future KM3NeT [12] and counterpart on the Northern hemisphere, with a GVD [13]), various possibilities for coordinated sensitivity “substantially exceeding that of all physics programs and analyses open up. They are existing neutrino telescopes including IceCube” [2]. discussed in sections 3 and 4. KM3NeT is just finishing its design phase [3], but Finally, section 5 lists formal and procedural has not yet converged to a final configuration. The possibilities of cooperation between KM3NeT and cited sensitivity requirement results not only from IceCube. gamma ray observations and their phenomenological interpretation (see e.g. [4-9]), but also from early IceCube data. The first section of this paper is 2.
  • Muon Spallation in Double Chooz

    Muon Spallation in Double Chooz

    Muon Spallation in Double Chooz Claire Thomas∗ REU, Columbia University and MIT (Dated: August 10, 2009) This report presents my work for Double Chooz at MIT during the 2009 Summer REU program, funded by Columbia University. Double Chooz is a reactor neutrino experiment that aims to measure the mixing parameter θ13. The experiment detects electron antineutrinos via inverse beta decay. Neutrons and light nuclei made in muon spallation are a major background to the experiment. The delayed neutron emitter 9Li is especially problematic because it mimics the inverse beta decay signal. For this reason I studied muon spallation in Double Chooz, focusing on the production and subsequent decay of 9Li. There are two key differences between 9Li decay and inverse beta decay. The first is that 9Li is a β− decay, so it emits an electron, whereas inverse beta decay emits a positron. The second difference is the energy of the neutrons emitted. In 9Li decay the neutron energy is on the order of MeV, whereas the inverse beta decay neutron has a negligible kinetic energy. Since Double Chooz does not distinguish charge, the positrons and electrons are not easy to distinguish. First, I ran simulations of electrons and positrons in the Double Chooz detector and constructed a late light variable to distinguish them from electrons. This proved insufficient, so I wrote general software to simulate radioactive decays in the Double Chooz detector. In this report I present the deposited energy spectra of a few important decays. 1. INTRODUCTION The consequence of neutrino oscillation is that an ex- periment that is sensitive to only one of the three neu- 1.1.