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Recent Results and Prospects of High- Energy Neutrino Astronomy APPIC Meeting May 8, 2014 Paris

Recent Results and Prospects of High- Energy Neutrino Astronomy APPIC Meeting May 8, 2014 Paris. Christian Spiering , DESY Zeuthen. Detection principle and physics goals. Detection Modes. Muon track from CC muon neutrino interactions Angular resolution 0.5°/0.1° for ice / water 1km³

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Recent Results and Prospects of High- Energy Neutrino Astronomy APPIC Meeting May 8, 2014 Paris

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  1. RecentResultsandProspectsof High-EnergyNeutrino Astronomy APPIC Meeting May 8, 2014 Paris Christian Spiering, DESY Zeuthen

  2. Detectionprincipleandphysicsgoals

  3. Detection Modes • Muon track from CC muon neutrino interactions • Angular resolution0.5°/0.1° forice/water 1km³ • dE/dx resolution factor 2-3 • Cascade from CC electron/tau and NC all flavor interactions • Angular resolution 10°/3° at 100 TeVforice/water • Energy resolution ~ 15%

  4. Physics with neutrino telescopes • Search for the sources of high-energy cosmicrays • Dark Matter and Exotic Physics • WIMPs • Magnetic Monopoles and other superheavies • Violation of Lorentz invariance • Neutrino and Particle Physics • Neutrino oscillations (incl. mass hierachy) • Charm physics • Cross sections at highest energies • Supernova Collapse Physics • MeV neutrinos in bursts  early SN phase, neutrino hierarchy, ... • Cosmic Ray Physics • Spectrum, composition andanisotropies • Earth and marine science, glaciology

  5. Main physicsdriversfornewprojects Gtonscale • Search for the sources of high-energy cosmicrays • Dark Matter and Exotic Physics • WIMPs • Magnetic Monopoles and other superheavies • Violation of Lorentz invariance • Neutrino and Particle Physics • Neutrino oscillations (incl. mass hierachy) • Charm physics • Cross sections at highest energies • Supernova Collapse Physics • MeV neutrinos in bursts  early SN phase, neutrino hierarchy, ... • Cosmic Ray Physics • Spectrum, composition and anisotropies Mtonscale

  6. present Devices

  7. Existingdetectors Baikal NT200+ ANTARES AMANDA IceCube

  8. 3600 m Lake Baikal 1366 m Proofofprinciple First underwaterneutrinos NT200

  9. NT200+ 3600 m NT200 1366 m

  10. V. Bertin - CPPM - ARENA'08 @ Roma 2500m 450 m 70 m ANTARES • 885 PMTs • 12strings • Operating in final • configuration • since 2008 Proofforreliable, precision operationof a -telescope

  11. IceCube Neutrino Observatory IceTop air shower detector 81 pairs of water Cherenkov tanks IceCube 86 strings including 8 Deep Core strings 60 PMT per string DeepCore 8 closely spaced strings 1450m Threshold: IceCube ~ 100 GeV DeepCore ~10 GeV 2450m 2820m

  12. http://www.globalneutrinonetwork.org/ • Oct. 2013, Munich • Antares • Baikal • IceCube • KM3NeT

  13. Selected Recentresultswithfreshmotivationfornewgenerationdevices

  14. Atmosphericneutrinospectrum proton c,(b) prompt νe,μ e,μ π μ νμ e νμ νe conventional

  15. Atmospheric neutrinos in IceCube .. and ANTARES arXiv:1308.1599

  16. Muon neutrino survival probability Oscillations of atmospheric neutrinos Vertically upward ANTARES/DeepCore Horizontal cosmicray n Earth L q

  17. Muon neutrino survival probability Oscillations of atmospheric neutrinos Vertically upward ANTARES/DeepCore Horizontal cosmicray n Earth L q

  18. Search forpointsourcesofextra-terrestrial neutrinos

  19. Limits for steady pointsources(assuming E-2spectra) • Factor 1000 in 12 years • No detectionsyet • ANTARES is best at Southern Sky IceCube sensitivity at Southern sky only for cut-off at >> 100 TeV • Expectanother factor 5 for IceCube in 2016 • KM3Net+GVD would give ~ factor 50 w.r.t. Antares Southern Sky | Northern Sky

  20. IceCube 3 years: upper limits and predictions

  21. Diffuse fluxSearch for an excessathighestenergies

  22. HESE resultsIceCube 3rdyear 5.7 3rdPeVevent.

  23. HESE skyplot, 3 years Couldthatbe a pointsource?

  24. Importanceof Northern detector ANTARES, arXiv 1402.6182: IceCubeaccumulation in tensionwithpoint-sourceinterpretation !

  25. Through-goingmuons in IceCube IC-79: 3.7 IC-59: 1.8 Highest energy: ~550 TeV (neutrino energy likely in PeV range)

  26. Interpretations • Theoreticalinterpretations • GalacticSources • ExtragalacticSources • Exotics • … • Presentconclusions still based on poordata. Soon: • 4 years HESE • More upwgardgoingmuondata • More cascades • Stackingofpointsources • Weareentering a periodwheretheoreticalspeculationscanrely on betterdata, andsomeusefulconclusionscouldbedrawnfortheconfigurationoffuturedetectors

  27. The Future projects

  28. Baikal, MediterraneanSea, South Pole GVD KM3NeT (ORCA) GNN DecaCube (PINGU)

  29. Rationale forthe multi-km³scale, South & North • Identifypointsources ! • Measuretheirspectrum ! • IceCubeisscratchingthepointsourcediscoveryregionatbest • Need larger detectors! (Howmuch larger?) • Detectors on the North and South lookto different partsofthesky(but withsomeoverlap!) • Can cover different partsofthespectraofthe same sources. • Iceandwaterhave different sytematics. Importantforflavorratiosandspectral form, in particularfor diffuse fluxes. This is „astronomy“

  30. Overview on high-energyprojects • KM3NeT: 6 x 0.6 km³ • Phase 1 (scale ~3 x ANTARES ): complete 2016, funded • Phase 1.5 (2 x 0.6 km³): complete 2020 positive signalsforfunding • Phase 2 (6 x 0.6 km³): completemid 2020s • DecaCube („IceCube High-Energyextension“, HEX) 5-10 km³ • Start 2018/19 ? • Complete 2027 ? Including PINGU withthe 3 firstofthe 8 seasons • Positive firstresponsesfrom NSF … • GVD (Baikal): 0.4 km³ • First of 10 clusters in early 2015 • Fullarray in 2020

  31. Gigaton Volume DetectorBaikal GVD

  32. State Marine U. Petersburg • JINR Dubna INR, MSU Moscow • Techn State U. Nizhni Novgorod • Irkutsk State University Germany: EvoLogicsGmbH ~ 50 authors, roleofDubnaincreasing SAC installed(Berezinsky, de Wolf, Gerhstein, Rubakov, Spiering, Spiro)

  33. Gigaton Volume Detector GVD >250 km3 0.4 to 1.5 km³ Detector in Lake Baikal

  34. Gigaton Volume Detector GVD Stage 1 • 10-12 clusters with 8 strings each • Cluster diameter 120 m • Height 375 m • Volume ~ 0.4 km³ • 24 OMs per string PMT Hamamatsu R7081-HQE  = 10” QE ~ 0.35%

  35. Prototype phase 2011-2015: demonstrationcluster „DUBNA“ • 192 OMs at 8 Strings • 2 Sections per String • 12 OMs per Section • DAQ-Center • Cable to Shore • Acoustic Positioning System • Instrumentation String with detector calibration and environment monitoring equipment • Active depth 950 – 1300 m Layout - 2014 L~ 345 m Buoy Station (BS) String section, 12 OMs Instrumentation string - Operating strings R ~ 60 m

  36. GVD timelinecumulativenumberofclusters vs. year 1 cluster = 8 strings = 192 PMT = 1 event (> 100TeV, cascade)/year Cost of the first cluster (“Dubna”): ~ 2.2 M€

  37. KM3NeT

  38. Fermi: encourages Northern detctors w.r.t galacticsources • Fermi LAT: “This detection provides direct evidence that cosmic-ray protons are accelerated in SNRs.” Science 339 (15-02-2013) 807–811 E2dN/dE [erg cm-2s-1] Eg [eV] Eg [eV]

  39. KM3NeT Distributed infrastructure - KM3NeT-France (Toulon) ~2500m - KM3NeT-Italy (Capo Passero) ~3400m - KM3NeT-Greece (Pylos) ~4500m Until 2016: construction of KM3NeT phase I detectors in France and Italy (~30 M€)

  40. KM3NeT • 6 building blocks, 2 per site. Overall volume ~ 4 km³ • 115 strings at 90 m distance • 18 OMs per string, 36 m vertical distance ~ 600 m 1 km

  41. Muon angular resolution KM3NeT

  42. Key elements Launcher vehicle • rapid deployment • autonomous unfurling • recoverable Optical module • 31 x 3” PMTs • low-power HV, LED • White Rabbi time synch.

  43. In-situ testwith prototype DOM 50 Atmospheric muons K40 random coincidences + data Atmospheric muons + data (M ≥ 7) shadowing Photon countingDirectionality 40 30 Rate [Hz] Rate [a.u.] 20 10 0 PMT orientation [deg.] Multiplicity

  44. Management • EU funded Design Study 2006–2009 • EU funded Preparatory Phase 2008–2012 • KM3NeT phase-1 2013–20XX • established collaboration • 40 institutes, more than 240 persons • elected central management • set up project organisation • prototyping, cost review, planning, QA/QC • drafted Memorandum of Understanding • investments, facilities, human resources, access policy • set up Resources Review Board • set up Scientific & Technical Advisory Committee • Technical design agreed technology is part of existing CDR and TDR • updates ongoing following PRRs

  45. Cost • Totalinvestment costs 220–250 M€ • conform with ESFRI roadmap (2006) and TDR (2010) • includes contingency of 10%, provided no VAT • Operational costs 3% of investment per year • Operation > 15 yearss • Cost of 1 string incl. PMT ~ 230 k€ + Interlink cables, deployment and connections ~ 90k€

  46. Summary on thephasesof KM3NeT

  47. South Pole

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