Neutrino physics with IceCube DeepCore-PINGU … and comparison with alternatives TeVPA 2012 TIFR Mumbai, India Dec 10-14, 2012 Walter Winter Universität Würzburg Contents Introduction Oscillation physics with Earth matter effects Mass hierarchy determination with PINGU Neutrino beam to PINGU? Atmospheric neutrinos Comparison with alternatives, and outlook Summary 2 Atmospheric neutrino anomaly The rate of neutrinos should be the same from below and above But: About 50% missing from below Neutrino change their flavor on the path from production to detection: Neutrino oscillations (Super-Kamiokande: “Evidence for oscillations of atmospheric neutrinos”, 1998) 3 Three flavors: Summary Three flavors: 6 params (3 angles, one phase; 2 x Dm2) Atmospheric oscillations: Amplitude: q23 Frequency: Dm312 Coupling: q13 Suppressed effect: dCP Solar oscillations: Amplitude: q12 Frequency: Dm212 (Super-K, 1998; Chooz, 1999; SNO 2001+2002; KamLAND 2002; Daya Bay, RENO 2012) Describes solar and atmospheric neutrino anomalies, as well as reactor antineutrino disapp.! 4 (short baseline) (also: T2K, Double Chooz, RENO) 5 Consequences of large q13 q13 to be well measured by Daya Bay Mass hierarchy: 3s discovery for up to 40% of all dCP possible iff ProjectX, possibly until 2025 CP violation measurement extremely difficult Need new facility! Huber, Lindner, Schwetz, Winter, 2009 6 Oscillation physics with Earth matter effects Matter profile of the Earth … as seen by a neutrino (not to scale) Inner core (PREM: Preliminary Reference Earth Model) Core 8 Matter effect (MSW) (Wolfenstein, 1978; Ordinary matter: Mikheyev, Smirnov, electrons, but no m, t 1985) Coherent forward scattering in matter: Net effect on electron flavor Hamiltonian in matter (matrix form, flavor space): Y: electron fraction ~ 0.5 (electrons per nucleon) 9 Parameter mapping … for two flavors Oscillation probabilities in vacuum: matter: Matter resonance: In this case: - Effective mixing maximal - Effective osc. frequency minimal MH Resonance energy: For nm appearance, Dm312: - r ~ 4.7 g/cm3 (Earth’s mantle): Eres ~ 6.4 GeV - r ~ 10.8 g/cm3 (Earth’s outer core): Eres ~ 2.8 GeV 10 Mantle-core-mantle profile (Parametric enhancement: Akhmedov, 1998; Akhmedov, Lipari, Smirnov, 1998; Petcov, 1998) Probability for L=11810 km (numerical) ! Param. enhancement Core resonance energy Parametric enhancement through mantle-core-mantle profile of the Earth. Unique physics potential! Mantle resonance energy Threshold effects expected at: Naive L/E scaling does not apply! 2 GeV 4-5 GeV 11 Mass hierarchy determination with PINGU What is PINGU? (“Precision IceCube Next Generation Upgrade“) Fill in IceCube/DeepCore array with additional strings Drive threshold to lower energies LOI in preparation Modest cost ~30-50M$ (dep. on no. of strings) Two season deployment anticipated: 2015/2016/2017 (PINGU, 12/2012) 13 PINGU fiducial volume? A ~ Mt fiducial mass for superbeam produced with FNAL main injector protons (120 GeV) (PINGU, 12/2012) Multi-Mt detector for E > 10 GeV atmospheric neutrinos Fid. volume depends on trigger level (earlier Veff higher, which is used for following analyses!) LBNE-like Atm. beam neutrinos 14 Mass hierarchy measurement: statistical significance (illustrated) Source (spectrum, solid angle) Atmospheric neutrinos arXiv:1210.5154 Beams M. Bishai x Osc. effect (in matter) x Detector mass x Cross section ~E >2 GeV > 5 GeV Core res. Measurement at threshold application rather for future upgrades: MICA? 15 Beams to PINGU? Labs and potential detector locations (stars) in “deep underground“ laboratories: All these baselines cross the Earth‘s outer core! (Agarwalla, Huber, Tang, Winter, 2010) FNAL-PINGU: 11620 km CERN-PINGU: 11810 km RAL-PINGU: 12020 km JHF-PINGU: 11370 km 16 Example: “Low-intensity“ superbeam? Here: use most conservative assumption NuMI beam, 1021 pot (total), neutrinos only [compare to LBNE: 22+22 1020 pot without Project X ~ factor four higher exposure than the one considered here] (FERMILAB-PROPOSAL-0875, NUMI-L-714) Low intensity may allow for shorter decay pipe Advantage: Peaks in exactly the right energy range for the parametric enhancement M. Bishai Include all irreducible backgrounds (intrinsic beam, NC, hadronic cascades), 20% track mis-ID 17 Event rates (for Veff 03/2012) Normal hier. Inv. hierarchy Signal 1560 54 39 511 59 750 3 4 Neutral currents 2479 2479 Total backgrounds 3032 3292 Total signal+backg. 4592 Backgrounds: ne beam Disapp./track mis-ID nt appearance >18s (stat. only) 3346 18 Mass hierarchy with a beam All irreducible backgrounds included (Daya Bay best-fit; current parameter uncertainties included; based on Tang, Winter, JHEP 1202 (2012) 028 ) GLoBES 2012 Very robust mass hierarchy measurement (as long as either some energy resolution or control of systematics) 19 Atmospheric neutrinos Akhmedov, Razzaque, Smirnov, 2012 Neutrino source available “for free“ Source not flavorclean different channels contribute and mask effect Power law spectrum arXiv:1210.5154 Many different baselines at once, weighted by solid angle Detector: angular+energy resolution required! A. Smirnov 20 Mass hierarchy with atmospheric neutrinos Statistical significance depends on angular and energy resolution About 3-10s likely for reasonable values Final proof of principle will require event reconstruction techniques (in progress) Akhmedov, Razzaque, Smirnov, 2012 21 Comparison with alternatives … and outlook Mass hierarchy 3s No “conventional“ atm. neutrino experiment could be built on a similar timescale or at a similar cost Bottleneck: Cavern! Akhmedov, Razzaque, Smirnov, 2012; v5 PINGU completed by beginning of 2017? 3s, Project X and T2K with proton driver, optimized neutrino-antineutrino run plan PINGU 20182020? Huber, Lindner, Schwetz, Winter, JHEP 11 (2009) 44 23 Probabilities: dCP-dependence There is rich dCP-phenomenology: NH L=11810 km 24 Upgrade path towards dCP? Measurement of dCP in principle possible, but challenging Wish list: Electromagnetic shower ID (here: 1% mis-ID) Energy resolution (here: 20% x E) Maybe: volume upgrade (here: ~ factor two) Project X = LBNE + Project X! same beam to PINGU Currently being discussed in the context of further upgrades - MICA; requires further study PINGU as R&D exp.? Tang, Winter, JHEP 1202 (2012) 028 25 Matter density measurement Example: LBNE-like Superbeam Precision ~ 0.5% (1s) on core density Complementary to seismic waves (seismic shear waves cannot propagate in the liquid core!) from: Tang, Winter, JHEP 1202 (2012) 028; see also: Winter, PRD72 (2005) 037302; Gandhi, Winter, PRD75 (2007) 053002; Minakata, Uchinami, PRD 75 (2007) 073013 26 Conclusions: PINGU Megaton-size ice detector as upgrade of DeepCore with lower threshold; very cost-efficient compared to liquid argon, water Unique mass hierarchy measurement through MSW effect in Earth matter Atmospheric neutrinos: Neutrino source for free, many different baselines Requires energy and angular resolution (reconstruction work in progress) PINGU to be the first experiment to discover the mass hierarchy at 3-5s? Neutrino beam: Requires dedicated source, with relatively low intensity Proton beams from FNAL main injectior have just right energy to hit mantlecore-mantle parameteric enhancement region Even possible as counting experiment, no angular resolution needed Beyond PINGU: CPV and matter density measurements perhaps possible with beam to even denser array (MICA)? PINGU as R&D experiment; worth further study! Technology also being studied in water ORCA 27 BACKUP Possible neutrino sources There are three possibilities to artificially produce neutrinos Beta decay: Example: Nuclear reactors, Beta beams Pion decay: Superbeam From accelerators: Pions Protons Target Selection, focusing Muons, neutrinos Decay tunnel Neutrinos Absorber Muon decay: Muons produced by pion decays! Neutrino Factory 29 Detector paramet.: mis-ID misID: fraction of events of a specific channel mis-identified as signal 1.0? misIDtracks << misID <~ 1 ? (Tang, Winter, JHEP 1202 (2012) 028) 30 Detector requirements Want to study ne-nm oscillations with different sources: Beta beams: q13, dCP In principle best choice for PINGU (need muon flavor ID only) Superbeams: q13, dCP Need (clean) electron flavor sample. Difficult? Neutrino factory: q13, dCP Need charge identification of m+ and m- (normally) 31 Detector parameterization (low intensity superbeam) Challenges: Electron flavor ID Systematics (efficiency, flux normalization near detector?) Energy resolution Make very (?) conservative assumptions here: Fraction of mis-identified muon tracks (muon tracks may be too short to be distinguished from signal) ~ 20% Irreducible backgrounds (zeroth order assumption!): Intrinsic beam background Neutral current cascades nm nt cascades (hadronic and electromagnetic cascades indistinguishable) Systematics uncorrelated between signal and background No energy resolution (total rates only) (for details on parameterization: Tang, Winter, JHEP 1202 (2012) 028) 32 Measurement of dCP? Many proposals for measuring CP violation with a neutrino beam Require all a dedicated (new) detector + control of systematics Coloma, Huber, Kopp, Winter, 2012 33