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KM3Net

KM3Net. KM3Net A Deep-Sea Research Infrastructure in the Mediterranean Sea Incorporating a Neutrino Telescope. Why particle physics community wants a neutrino telescope Principles behind a neutrino telescope Current telescope KM3NeT Science Data Access and distribution Current status.

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KM3Net

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  1. KM3Net KM3Net A Deep-Sea Research Infrastructure in the Mediterranean Sea Incorporating a Neutrino Telescope U. Katz: Neutrino Telescopy ...

  2. Why particle physics community wants a neutrino telescope Principles behind a neutrino telescope Current telescope KM3NeT Science Data Access and distribution Current status

  3. Why Neutrino Telescopes? • Neutrinos traverse space without deflection or attenuation • they point back to their sources; • they allow for a view into dense environments; • they allow us to investigate the universe over cosmological distances. • Neutrinos are produced in high-energy hadronic processes→ distinction between electron and proton acceleration. • Neutrinos could be produced in Dark Matter annihilation. • Neutrino detection requires huge target masses→ use naturally abundant materials (water, ice). U. Katz: Neutrino Telescopy ...

  4. Aiming at a km3-Detector in the Mediterranean HENAP Report to PaNAGIC, July 2002: • “The observation of cosmic neutrinos above 100 GeV is of great scientific importance. ...“ • “... a km3-scale detector in the Northern hemisphere should be built to complement the IceCube detector being constructed at the South Pole.” • “The detector should be of km3-scale, the construction of which is considered technically feasible.” U. Katz: Neutrino Telescopy ...

  5. protons E>1019 eV (10 Mpc) neutrinos gammas (0.01 - 1 Mpc) protons E<1019 eV Particle propagation in the Universe Cosmic accelerator 1 parsec (pc) = 3.26 light years (ly) Photons: absorbed on dust and radiation; Protons/nuclei: deviated by magnetic fields, reactions with radiation (CMB) U. Katz: Neutrino Telescopy ...

  6. The Principle of Neutrino Telescopes Čerenkov light: • In water: θC≈ 43° • Spectral range used: ~ 350-500nm. Role of the Earth: • Screening against all particlesexcept neutrinos. • Atmosphere = target for productionof secondary neutrinos. Neutrino reactions (key reaction is nmN→ mX): • Cross sections and reaction mechanisms known from acceleratorexperiments (in particular HERA). • Extrapolation to highest energies (> 100 TeV) uncertain. U. Katz: Neutrino Telescopy ...

  7. The Neutrino Telescope World Map U. Katz: Neutrino Telescopy ...

  8. IceCube IceCube: a km3 Detector in Antarctic Ice South Pole Dark sector Skiway Dome AMANDA U. Katz: Neutrino Telescopy ...

  9. AMANDA The IceCube Project IceTop Skiway • 80 Strings; • 4800 PMTs; • Instrumented volume: 1 km3 (1 Gigaton) • IceCube is designed to detect neutrinos of all flavors at energies from 107 eV (SN) to 1020 eV 1400 m 2400 m U. Katz: Neutrino Telescopy ...

  10. Locations of the sites of the three Mediterranean Neutrino Telescope projects U. Katz: Neutrino Telescopy ...

  11. ANTARES: Detector Design • String-based detector; • Underwater connectionsby deep-sea submersible; • Downward-looking PMs,axis at 45O to vertical; • 2500 m deep. 25 storeys, 348 m 14.5m 100 m Junction Box U. Katz: Neutrino Telescopy ...

  12. ANTARES: First Deep-Sea Data • Rate measurements: Strong fluctuation of bioluminescence backgroundobserved PM Rate (kHz) Constant baseline ratefrom 40K decays 10min 10min time (s) U. Katz: Neutrino Telescopy ...

  13. Schematic view of the major components of the KM3NeT neutrino telescope. Note that the drawing is not to scale and that the number of components indicated is much smaller than in reality. A marine science node is also shown Schematic concept of complementing the KM3NeT neutrino telescope with marine science instrumentation U. Katz: Neutrino Telescopy ...

  14. Seafloor layouts (top) and 3-dimensionl visualisations (bottom) of example neutrino telescope configurations of the type “homogeneous”, “cluster” and “ring” (left to right). In the top panel, each red point indicates a vertical arrangement of OMs or storeys, in the bottom panel each red point represents a storey. U. Katz: Neutrino Telescopy ...

  15. Suggested Sea Floor Geometry of KM3NeT at CDR 91 Towers Regular Hexagon U. Katz: Neutrino Telescopy ...

  16. Earth-Sea Science • Junction Boxes around the neutrino telescope. • Science instruments within the Neutrino telescope for monitoring the array behaviour and calculating the accurate position of the detection units • Initial instrumentation around the array consisting of mission proved and comercially available sensors and components. U. Katz: Neutrino Telescopy ...

  17. SUGGESTED SEA FLOOR GEOMETRYDISTRIBUTED CIRCLES CASE Safety Radius Max 10 km 1000m Each ESSJB can be located independently within 10km of the centre. Each requires a 500 m radius (minImum) “flat” area around it. Telescope site 2km diameter U. Katz: Neutrino Telescopy ...

  18. Criteria for selecting Earth-Sea Science node placement Outside the anticipated area of the Neutrino telescope expansion Monitoring a transect perpendicular to the continental margin line Monitoring of residual particle fluxes from canyons Current monitoring near the sea floor or within the water column Artificial reef effect of the telescope infrastructure on the benthic life Activities of marine mammals with respect to the infrastructure Position of backbone cables (interference between cables and instrumentation) Interference between experiments and their respective instrumentation set Maintenance activity (ROV manoeuvrability and support vessel drift due to currents) Future expansion over a twenty year span of the Earth-Sea science activities U. Katz: Neutrino Telescopy ...

  19. Earth-Sea Science Instruments within the telescope 1.Use Data from PMTs for Bioluminescence 2. Use data from acoustics 3. Study positions of the PMTs to interpret flow. 4. Utilise “house keeping” environmental instrumentation. E.g current meters Add additional earth sea science sensors within the array e.g. high speed, high precision thermistors U. Katz: Neutrino Telescopy ...

  20. NIOZ3: Custom-made sensitive temperature sensor to study internal waves and large turbulence scales Specifications: • Accuracy <0.001 °C • Response time 0.25 s • Autonomy 1.5 years at 1 Hz sampling • Sensors are independent : -> any number (100 or more) -> at any position on moorings -> no connecting cables • Every clock is synchronized inductively -> sensors stay synchronized at < 1 s • Broadcast programming with LED-code indicators -> no need to open the sensors U. Katz: Neutrino Telescopy ...

  21. 1. Eth 1000LX (fiber) – 400VDC – NTP/PTP • Applications: • Daisy chain for another JB, • high power equipment: • robotics, vertical profiler… • network extension up to 20km • 4. VDSL2 Modem – 400VDC – NTP/PTP • Network extension, • measurements in water column, • instrument or instrument cluster up to 5-6km • (low cost extension (vs. fiber), • seismic network, • acoustic network • 2. Eth 100BT (copper) – 48VDC – • NTP/PTP + PPS/NMEA • Ethernet scientific instruments, • Seismometer (OBS), • still camera , • video, • hydrophone, • crawler… • 3. RS232/422/485 – 48VDC – PPS/NMEA • Serial scientific instruments • ADCP, • piezometer (pore pressure sensor) , • seismometer, • CTD, • chemical analyzer,… Daisy chain Up to 5-6km Extension to 20 km <1km <1km U. Katz: Neutrino Telescopy ...

  22. Particle Physics data centre ? Earth-Sea Science dataflow Neutrino Telescope Science & calibration data U. Katz: Neutrino Telescopy ...

  23. Users and stakeholders of the KM3NeT marine science node(s) U. Katz: Neutrino Telescopy ...

  24. 25 storeys, 348 m 14.5m 100 m Junction Box ANTARES: Detector Design • String-based detector; • Underwater connectionsby deep-sea submersible; • Downward-looking PMs,axis at 45O to vertical; • 2500 m deep. U. Katz: Neutrino Telescopy ...

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