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Toward Precision Neutrino Physics with Deepcore and Beyond

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Toward Precision Neutrino Physics with Deepcore and Beyond Toward Precision Neutrino Physics with DeepCore and Beyond Tyce DeYoung Department of Physics Pennsylvania State University VLVνT ’11 Erlangen, Germany October 14, 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, Super-K, KamLAND, LBNE 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, Super-K, KamLAND, LBNE 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, Super-K, AMANDA, Baikal, RICE, Auger, KamLAND, LBNE 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, Super-K, AMANDA, Baikal, RICE, Auger, KamLAND, LBNE 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, Super-K, AMANDA, Baikal, RICE, Auger, KamLAND, LBNE 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 was 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 VLVνT ’11, Erlangen, Germany October 14, 2011 IceCube DeepCore scattering • Eight special strings plus 12 nearest standard IceCube strings • 72 m interstring spacing IceCube • 7 m DOM spacing extra veto cap • High Q.E. PMTs • ~5x higher effective AMANDA photocathode density Deep • In the clearest ice, below 2100 m Core 350 m • λatten ≈ 40-45 m • 30 MTon detector with ~10 GeV 250 m threshold, O(105) atm. ν / year • IceCube is an active veto against cosmic ray muon background IceCube DeepCore scattering • Eight special strings plus 12 nearest standard IceCube strings • 72 m interstring spacing IceCube • 7 m DOM spacing extra veto cap • High Q.E. PMTs • ~5x higher effective AMANDA photocathode density Deep • In the clearest ice, below 2100 m Core 350 m • λatten ≈ 40-45 m • 30 MTon detector with ~10 GeV 250 m threshold, O(105) atm. ν / year • IceCube is an active veto against cosmic ray muon background 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 DeepCore 10-2 DeepCore 10-2 10-3 10-3 10-4 10-4 without νe without νμ 10-5 10-5 DeepCore DeepCore 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 (ν Energy - GeV) Log (ν Energy - GeV) 10 e 10 µ • DeepCore dominates total response for Eν below ~100 GeV • Improved trigger efficiency overcomes much smaller volume • Linear growth at high energy reflects neutrino cross section, not detector efficiency • Analysis efficiencies not included! First analyses accepted low (<10%) efficiency, expected to improve considerably in the future Neutrino Astronomy with DeepCore • Atmospheric neutrino veto? • May enhance observability of Galactic sources in the ~10 TeV band (Schönert et al. 2009) • Still difficult at these energies due to loss of muon range factor, rising neutrino cross section • Sensitivity to low energy neutrinos from transients? • E.g. choked or atm. ν magnetically dominated GRBs possible source with veto (e.g., Ando & Beacom 2005; spectrum Razzaque, Meszaros & Waxman 2005; Meszaros & Rees 2011) Tyce DeYoung VLVνT ’11, Erlangen, Germany October 14, 2011 Search for Solar Dark Matter Analysis Results from the Sun • Solar WIMP dark matter searches probe spin-dependent scattering cross section details on SUSY-WIMP limits: details on LKP limits: Abbasi et al., PRL. 102, 201302 (2009) (IC22 result) Abbasi et al., PRD 81 (2010) 057101. (IC22 result) ICRC 2011 (IC40+AMANDA result) ICRC 2011 (IC40+AMANDA result) • SI cross section constrainedICRC 2011 (IC86 well sensitivity) by direct search experiments • DeepCore is limits & sensitivity: essential to low Only data, when Sun is mass WIMPs below the horizon (below about main syst. uncertainty: 100 GeV) Photon propagation in the ice & absolute • For non-SUSY DOM efficiency (~20%) DM, even lower energies are of relate muon flux and WIMP - nucleon cross≠ interest section: 07/09/11 Matthias Danninger TAUP 2011 9 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 • Plot of νμ disappearance shows Unoscillated 1200 Oscillated only simulated signal (no BG), No Reconstruction 1000 θ = π/2 simple energy estimator 23 2 -3 Δm23 = 2.4 × 10 eV 800 ~15σ Events/NChannel/Year Cos(zenith) < -0.6 • Analysis efficiencies not per bin included yet – work ongoing 600 400 • Magnitude of the signal may help overcome poorer 200 0 control of systematics 0 10 20 30 40 50 60 70 80 90 100 NChannels [Hit DOMs] Observation of Atmospheric 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 VLVνT ’11, Erlangen, Germany October 14, 2011 Observation of Atmospheric Cascades C. Ha, TAUP 2011 • Substantial sample of cascades, final data set ~60% cascades • Mean energy ~180 GeV, not sensitive to oscillations (with these cuts) • Atmospheric muon background being assessed, but νμ CC dominant • Represents about 5x enrichment of cascades over νμ CC, but better neutrino particle ID clearly desirable • Potential to discriminate between Bartol, Honda atmospheric neutrino models – measuring air shower physics! ! Cascades CC νμ Total cascades Bartol 650 454 1104 observed CC Honda 551 415 966 μ ν preliminary Data 1029 Bartol Honda Data Beyond DeepCore 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, Super-K, AMANDA, Baikal, RICE, Auger, KamLAND, LBNE DeepCore ANTARES IceCube, KM3NeT ARIANNA,... Double CHOOZ, Daya Bay, etc. Atmospheric/Astrophysical Gamma Ray Bursts Neutrino Oscillations Soft Galactic Dark Cosmic Ray Matter Accelerators Beyond DeepCore 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, Super-K, AMANDA, Baikal, RICE, Auger, KamLAND, LBNE DeepCore ANTARES IceCube, KM3NeT ARIANNA,... Double CHOOZ, PINGU & Beyond? Daya Bay, etc. Atmospheric/Astrophysical Gamma Ray Bursts Neutrino Oscillations Soft Galactic Dark Cosmic Ray Matter Accelerators Toward Precision Particle Physics in Ice • First stage (“PINGU”) • Add ~20 further infill strings to DeepCore, extend energy reach to ~1 GeV • Improved sensitivity to DeepCore physics, and test bed for next stage • Use mostly standard IceCube technology, include some R&D toward new types of photodetectors • Include additional calibration devices with an eye toward few-% systematics • Ideas beyond PINGU • Using new photon detection technology, can we build a detector that can reconstruct Cherenkov rings for events well below 1 GeV? • PINGU topics, plus proton decay, supernova neutrinos • At least comparable in scope to IceCube, but in a much smaller volume Tyce DeYoung VLVνT ’11, Erlangen, Germany October 14, 2011 Beyond DeepCore: PINGU • Now developing a proposal to one possible geometry further increase density of New PINGU instrumentation in DC volume Strings • An additional 18-20 strings, 1000-1200 DOMs • Make use of well-established IceCube drilling technology • Might get to a Existing standard threshold of ~1 GeV Existing IceCube DeepCore in a ~10 MTon 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 VLVνT ’11, Erlangen, Germany October 14, 2011 PINGU Effective Volumes Preliminary 100 100 Megaton Megaton 10 10 1 1 0.1 IC2011 DC Contained
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