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