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Next Generation Neutrino Telescopes NIAPP Topical Workshop Munich , July 2014

Next Generation Neutrino Telescopes NIAPP Topical Workshop Munich , July 2014. Christian Spiering , DESY Zeuthen. Existing detectors. Baikal NT200+. Antares. AMANDA. IceCube. 3600 m. Lake Baikal. 1366 m. NT200. NT200+. 3600 m. NT200. 1366 m. 2500m. 4 50 m. 70 m.

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Next Generation Neutrino Telescopes NIAPP Topical Workshop Munich , July 2014

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  1. Next Generation Neutrino Telescopes NIAPP Topical Workshop Munich, July 2014 Christian Spiering, DESY Zeuthen

  2. Existingdetectors Baikal NT200+ Antares AMANDA IceCube

  3. 3600 m Lake Baikal 1366 m NT200

  4. NT200+ 3600 m NT200 1366 m

  5. V. Bertin - CPPM - ARENA'08 @ Roma 2500m 450 m 70 m ANTARES • 885 PMTs • 12strings • Operating in final • configuration • since 2008

  6. 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

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

  8. Goals of GNN • organize schools and topical workshops, specifically the MANTS meetings and VLVNT conferences • provide forum for exchanges and consultation between partners • work toward framework for coordination of cooperative actions and self-organization of the neutrino astronomy community • establish common legacy of public documents that would form the foundation of the field (like Technical Design Reports, VLVNT proceedings, etc.) • create an annual award for an outstanding PhD thesis • create a public web page http://www.globalneutrinonetwork.org/ • stimulate joint outreach activities, • coordinate relations with other fields of science, such as particle physics, astrophysics, environmental sciences, geosciences, marine biology and oceanography, and glaciology • to prepare a foundation for even closer future cooperation, the GNO

  9. Goals of GNN Encourage formation of cooperative projects directed at the most effective use of our infrastructures by facilitating the combination of experimental data to achieve more reliable results and to further increase the sensitivity beyond that of individual detectors, e.g. • combinations of sky maps • cross-checks of results with different systematics • coordination of alert and multi-messenger policies • exchange and mutual checks of software • creation of a common software pool • standards for data representation • exchange of expertise through mutual working visits of scientists and engineers • exchange of expertise by forming ad-hoc advisory committees of members of the four participating collaborations, if requested by a participating party; this may generate better understanding of data, optimization of future detector configurations, or technological solutions for the next generation arrays.

  10. WhereareweNow ?

  11. Diffuse flux

  12. HESE: Ernie, Bert, Big-Bird + 34 moreevents 5.7

  13. Through-goingmuons in IceCube IC-79: 3.7 preliminary

  14. Puttingbothtogether

  15. Point sources

  16. HESE skyplot, 3 years: nopointsources (yet) ANTARES, arXiv 1402.6182: in tensionwithpoint-sourceinterpretation !

  17. Through-goingmuons: 4 years IC40/59/79/86 Nopointsources (yet) N o r t h S o u t h

  18. IceCube 4 years: upper limits and predictions CrabNebula

  19. IceCube 4 years: upper limits and predictions

  20. Through-goingmuons: sensitivities/limits • Factor 1000 in 12 years • No detections yet • ANTARES is best at Southern Sky IceCube sensitivity at Southern sky only for cut-off at >> PeV • Expect another factor 3 for IceCube in 2016 • KM3NeT/GVD would give ~ factor 50 w.r.t. Antares early Amanda limit IceCube 4 years preliminary Southern Sky | Northern Sky

  21. Combinedskymap • Toberelased in autumn • Best effectfordetectorsofsimilarsize in South and North

  22. Next challenges: • Need better understanding of • Diffuse spectrum, cut-off ? • Flavor ratio • Charm contribution to atmospheric background (“prompt ”) • Anisotropy ? • Most important: • Find point sources • … and later: measure spectrum of individual sources This isAstronomy!

  23. Next challenge: identifypointsourcesofrecordedneutrinos(Figuretakenfrom Marek Kowalski) 1%

  24. Next challenge: identifypointsourcesofrecordedneutrinos(Figuretakenfrom Marek Kowalski) Galaxy Clusters

  25. The Future projects

  26. Baikal, MediterraneanSea, South Pole GVD KM3NeT (ORCA) GNN Next Generation IceCube HEX (+PINGU + …)

  27. KM3NeT

  28. The BaikalCollaboration ~ 50 authors, 6 institutions (roleofDubnaincreasing!) • State Marine U. Petersburg • JINR Dubna INR, MSU Moscow • Techn State U. Nizhni Novgorod • Irkutsk State University Germany: EvoLogics GmbH

  29. KM3NeT

  30. KM3NeT Distributed infrastructure - KM3NeT-France (Toulon) ~2500m - KM3NeT-Italy (Capo Passero) ~3400m - KM3NeT-Greece (Pylos) ~4500m Until 2015: construction of KM3NeT phase I detectors in France and Italy (31+8 M€)

  31. The DOM anditsperformance • Long-term in situ test at ANTARES sitewithone DOM finished • At present: a sectionwith 3 DOMs operated in situ

  32. Directionalityof a single DOM

  33. 6 blocks at 3 locations: 6 x 0.6 km³ 115 strings per block18 DOMs per string 31 PMTs per DOM France Italy Greece

  34. 2blocks at 2 locations: Phase 1.5 (2020) France ORCA Italy

  35. Phase-1 (Italy) 8 towers • Start with 8 towers(necessary to match spending profile and to demonstrate construction activity) • Add 24 strings until 2016 • 3-4 times the sensitivity of ANTARES • Demonstrate feasibility and extract “physics on a 3-times-Antares scale” 24 strings

  36. KM3NeT Phase 1.5: diffuse fluxes • Motivated by IceCubesignal • 90 m string distance,36m vertical spacing of DOMs • Moderately increased string distance possible (e.g. 120 m) • Cost: 80-90 M€ (including Phase-1) Diffuse neutrino fluxes: Sensitivity to IceCube signal

  37. KM3NeT Phase 1.5: pointsourcesensitivity ForspecificfluxassumptionsforSupernova Remnants(modeledusingγ-rayresults) Kelneret al., Phys.Rev. D74 (2006) 034018  3σdetection in ~5 years IceCubesensitivity at the time KM3NeT-1.5 hasoperated 3 years Uli Katz, KM3NeT STAC Meeting June 27, 2014 preliminary

  38. KM3NeT Phase 1.5: containedcascades • Directionresolution ~ 1.5° • Point sourcesearchwithcascadesof > 100 TeVenergy • Position accuracy ~1 m; • Energyresolution ~ 10% Uli Katz, KM3NeT STAC meeting June 27, 2014 preliminary (muontracks ~0.1°)

  39. Phasesof KM3NeT

  40. Gigaton Volume DetectorBaikal GVD

  41. Gigaton Volume Detector GVD >250 km3 0.5 to 1.5 km³ Detector in Lake Baikal

  42. 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 Ang. resol. formuons ~ 0.25° Ang. resol. forcascades 3-4° PMT Hamamatsu R7081-HQE  = 10” QE ~ 0.35%

  43. Prototype phase 2011-2015: 5of 8 stringsinstalleddemonstrationcluster „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

  44. I. Belolaptikov, GVD SAC Meeting June 13, 2014 preliminary Prototype results Str.3 Str.2 • Angular distributionofdowngoingmuons • Laser signalreconstruction(only 2 strings, dist. 130 m) • E ~ 10% (@ 100 PeV) • r ~ 3.5 m ● z = -110.9 m ρ = 130.8 m Two strings Laser

  45. Project time-line DzhanDzhilkibaev, GVD SAC Meeting June 13, 2014 R & D Prototyping & Construction Data Taking Prototype Strings 2009 2010 2014 2008 2012 2011 2013 2020 2015 • Design, production and long-term in-situ tests of key elements and systems of GVD: • Optical Modules • FADC-readout system • Section Trigger Logics • Calibration system • Data Transmission • Cluster Trigger System, DAQ • Data Transport to Shore Engineering Arrays GVD-1 Cluster 8 strings 5strings (112 ОМ) 3 strings (72 ОМ) 3-strings (36 ОМs), 1 full string (24 ОМs) 3-strings (24 ОМ). Optical-electric cable to shore. Cluster DAQ-center. Shorestation.

  46. GVD, stage 2 (2025?) Stage 2 • 27 clusters with 8 strings each • Height 700 m (depth 600 m– 1300 m) • 48 OMs per string • Stage 1: volume ~0.5 km³ • Stage 2: volume ~ 1.5 km³

  47. Next Generation IceCubeNGIC

  48. South Pole infrastructure for neutrino (astro-)physics Device Volume Threshold Primary Goal • PINGU few Mton 2-3 GeV  mass hierarchy • HEX* 7-12 km³ ~10 TeV  astronomy cosmogenic neutrinos • Surface veto ~120 km² veto for IceCube CR physics • ARA ~120 km² ~50 PeV cosmogenic neutrinos * High Energy Extension. Including IceCube (1 km³ with 100 GeV threshold)

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