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KM3NeT The Birth of a Giant

KM3NeT The Birth of a Giant. Vlad Popa, Institute for Space Sciences, Magurele-Bucharest, Romania. Overview Introduction: what, who and why? Neutrino telescopes: how do they work? Physics goals, but not only… Present status, pilot experiments Many choices to be made…

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KM3NeT The Birth of a Giant

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  1. KM3NeT The Birth of a Giant Vlad Popa, Institute for Space Sciences, Magurele-Bucharest, Romania

  2. Overview • Introduction: what, who and why? • Neutrino telescopes: how do they work? • Physics goals, but not only… • Present status, pilot experiments • Many choices to be made… • Conclusions

  3. Overview • Introduction: what, who and why? • Neutrino telescopes: how do they work? • Physics goals, but not only… • Present status, pilot experiments • Many choices to be made… • Conclusions

  4. Overview • Introduction: what, who and why? • Neutrino telescopes: how do they work? • Physics goals, but not only… • Present status, pilot experiments • Many choices to be made… • Conclusions

  5. Overview • Introduction: what, who and why? • Neutrino telescopes: how do they work? • Physics goals, but not only… • Present status, pilot experiments • Many choices to be made… • Conclusions

  6. Overview • Introduction: what, who and why? • Neutrino telescopes: how do they work? • Physics goals, but not only… • Present status, pilot experiments • Many choices to be made… • Conclusions

  7. Overview • Introduction: what, who and why? • Neutrino telescopes: how do they work? • Physics goals, but not only… • Present status, pilot experiments • Many choices to be made… • Conclusions

  8. Introduction KM3NeT will be a very large volume (> km3 ) Neutrino Telescope, to be deployed in the Mediterranean Sea, after 2012.

  9. Introduction KM3NeT will be a very large volume (> km3 ) Neutrino Telescope, to be deployed in the Mediterranean Sea, after 2012. The consortium includes 40 Institutes or Universities from 10 European countries. The research is financed trough 2 European projects: “KM3NeT-DS” (completed), “KM3NeT-PP”, and by national agencies There will be room for Earth and Sea Sciences.

  10. Introduction KM3NeT will be a very large volume (> km3 ) Neutrino Telescope, to be deployed in the Mediterranean Sea, after 2012. The consortium includes 40 Institutes or Universities from 10 European countries. The research is financed trough 2 European projects: “KM3NeT-DS” (completed), “KM3NeT-PP”, and by national agencies There will be room for Earth and Ocean Sciences. One of the Magnificent Seven of the ASPERA Roadmap

  11. Introduction KM3NeT will be a very large volume (> km3 ) Neutrino Telescope, to be deployed in the Mediterranean Sea, after 2012. The consortium includes 40 Institutes or Universities from 10 European countries. The research is financed trough 2 European projects: “KM3NeT-DS” (completed), “KM3NeT-PP”, and by national agencies There will be room for Earth and Ocean Sciences. One of the Magnificent Seven of the ASPERA Roadmap Official web page: http://www.km3net.org

  12. Cyprus: University of Cyprus • France: CEA, CNRS, Haute Alsace University • Germany: Erlangen – Nurnberg University • Greece: Hellenic Open University, NCSR Demokritos, Athens National Observatory, Athens National University • Ireland: Advanced Study Institute, Dublin • Italy: INFN ( + Universities) • Netherlands: FOM (NIKHEF), NIOZ • Romania: ISS (INFLPR) • Spain: CSIC, Barcelona University, Valencia Technical University, Valencia University • United Kingdom: Aberdeen University, Leeds University, Sheffield University

  13. Neutrino telescopes: how do they work?

  14. Muon neutrinos (the “golden channel”): • Signature: muon (+ hadronic shower if reaction inside the detector) • Detectability: if muon crosses light acceptance • Measurement precision: Energy – fair (factor 2 at best for muon energies > 1TeV • Direction – very good (0.1o at high energies) • Remarks: the golden channel for point source searches (neutrino astronomy)

  15. Electron neutrinos • Signature: electromagnetic + hadronic shower (superimposed) • Detectability: if reaction is inside detector light acceptance • Measurement precision: Energy – good • Direction – fair (a few degrees at best) • Remarks: Important for diffuse flux measurements and flavour studies. Not distinguishable from other shower signatures.

  16. Tau neutrinos • Signatures: 1) if like • 2) if like • 3) if : hadronic shower • Detectability: if reaction is inside detector light acceptance (except 1) • Measurement precision: Energy – fair (large fraction goes to secondary ’s) • Direction – good for (1), fair otherwise • Remarks: Important for diffuse flux measurements and flavour studies. Only double-bang signatures might be distinctive. for E > few TeV “double bang sinature”

  17. All neutrinos (neutral current interactions) • Signatures: hadronic shower • Detectability: if reaction is inside detector light acceptance • Measurement precision: Energy – poor (large fraction goes to secondary ) • Direction – fair • Remarks: Important for diffuse flux measurements and flavour studies. Energy measurement much less precise, not distinguishable from other shower signatures.

  18. Physics goals, but not only… • . Neutrino astronomy • Diffuse neutrino flux • Dark Matter • Exotic Particles • Atmospheric muons and neutrinos • Neutrino Cross Sections • … • Earth and Sea Sciences

  19. The main scientific goal: Neutrino Astronomy • Point Sources • Supernova Remnants • Microquasars • Gamma Ray Bursters • Hidden Sources (not seen in other “wavelengths”)

  20. Neutrino Astronomy: Sky coverage (Galactic coordinates) From the South: IceCube (angular resolution ~ 10 ) From the North: KM3NeT (angular resolution ~ 0.10) > 75% of time >25% of time

  21. Other physics goals • Diffuse neutrino flux • Dark Matter • Exotic Particles • Atmospheric muons and neutrinos • Neutrino Cross Sections • …

  22. Diffuse neutrino energy flux Cosmogenic (extragalactic) C.R. p (E > 1019.5 eV) / CMB (pions, HE neutrinos) (GZK cutt-off) From all GRB’s and AGN’s, during the complete Universe history, extragalactic for E > 1017 – 1018 eV

  23. Other physics goals • Diffuse neutrino flux • Dark Matter Search based on WIMPS annihilation (in the center of the Sun) leading to HE neutrinos (directly in scenarios with extradimensions, or trough massive particle decays in supersymmetric scenarios).

  24. Other physics goals • Diffuse neutrino flux • Dark Matter • Exotic Particles • Atmospheric muons and neutrinos • Neutrino Cross Sections • …

  25. Exotic Particles • GUT Magnetic Monopoles • Intermediate mass Magnetic Monopoles • Nuclearites • Q-balls • …

  26. Magnetic Monopoles Magnetic charge g = n gD, n = 1,2,3,…? and gD= 137/2 e GUT monopoles Two categories Intermediate mass monopoles

  27. B=g/r2 Magnetic field of a point Dirac monopole 102 GeV 1015 GeV SU(3)C x [SU(2)L x U(1)y] SU(5) Confinement region: virtual gs, gluons, condensate of fermions -antifermion, 4 fermion virtual states SU(3)C x U(1)EM 10-35 s 10-9 s Electroweak unification: W, Z Grand Unification: virtual X,Y Radius (cm) 10-2910-16 10-13 Proton decay catalysis Gauge theories of unified interactions predict MMs GUT Monopoles Slowly moving! • Mass mM≥ mX/G > 1016 GeV ~ 0.02 mg  1017 GeV • Size: extended object r  few fmB ~ g/r2

  28. A proton decay is expected every Proton decay (Callan – Rubakov) Assuming Mon = 10-3, in water, 10 cm – 10m 30 s - 3 ms

  29. GUT MMs detectable trough the Cherenkov light emitted by the proton decay charged secondaries, between 3 ×104 – 105 photons with  = 300 – 600 nm for each event. A trigger should require multiple coincidences in a relatively large time window, and the efficiency of such a search depends stronglyon the assumed value of 0 and Mon… Best existing flux limit from MACRO:

  30. Intermediate mass MMs (105 - 1012 GeV)1994 De Rujula CERN-TH 7273/94E. Huguet & P. Peter hep-ph/ 901370 T.W. Kephart, Q. Shafi Phys. Lett. B520(2001)313Wick et al. Astropart. Phys. 18, 663 (2003) Produced in the Early Universe after GUT phase transitions ex. (Shafi)M ~ 1010 GeV , g = 2 gD , no p-decay catalysis IMMs can be accelerated in the galactic B field to relativistic velocities T = gD B L ~ 6 x 10 10 GeV (B/3x10-6 G) (L/300pc) Galaxy T  6 x 1010 GeV Neutron stars T  1011 - 1015 GeV AGN T  1014 - 1015 GeV Could they produce the highest energy cosmic ray showersE > 1020 eV ? 1015 GeV 109 GeV SU(3)x SU(2)x U(1) SU(4)x SU(2) x SU(2) SO(10) 10-35 s 10-23 s Relativistic!

  31. Intermediate mass MMs in VLVTs - By the monopole (and by  electrons) for Cherenkov light production - By  electrons for

  32. Cherenkov emission enhanced by a factor about 8500 compared to Cherenkov light emission by a single muon Direct Cherenkov emission ( > 0.74)

  33. Cherenkov light from δ rays (knock-on electrons), Mon>0.51

  34. Monopole • Direct • Recoil e- Muon Total number Cherenkov photons 300 < λ < 600 nm

  35. NuclearitesE. Witten, Phys. Rev. D30 (1984) 272A. De Rujula, S. L. Glashow, Nature 312 (1984) 734 • Aggregates of u, d, s quarks + electrons,ne=2/3 nu –1/3 nd –1/3 ns • Ground state of QCD; stable for 300 < A < 1057 rN 3.5 x 1014 g cm-3 rnuclei 1014 g cm-3 A qualitative picture… [black points are electrons] R(fm) 102 103 104 105 106 M(GeV) 106 109 1012 1015 1018 Produced in Early Universe or in strange star collisions (J. Madsen, PRD71 (2005) 014026) Candidates for cold Dark Matter! Searched for in CR reaching the Earth

  36. s e d e e u u d s • Essentially neutral (most if not all e- inside) • “Classical” properties: galactic velocities, elastic collisions, energy losses… • Could reach KM3NeTfrom above • Better flux limit from MACRO • (for nonrelativistic velocities): u s s s d d u u d e 1014 Too low masses to reach KM3NeT Could traverse the Earth, but very low expected fluxes M (GeV) Intermediate mass nuclearites 1022 M. Ambrosio et al., Eur.Phys. J. C13 (2000) 453; L. Patrizii, TAUP 2003 1010

  37. Nuclearites - basics A. De Rújula and S.L. Glashow,Nature 312 (1984) 734 • Typical galactic velocities   10-3 • Dominant interaction: elastic collisions with atoms in the medium • Dominant energy losses: • Phenomenological flux limit from the local density of DM:

  38. For M  8.4 1014 GeV it depends only on v2 The passage of a nuclearite in matter produces heat along its path In transparent media some of the energy dissipated could appear as visible light (black body radiation) The “optical efficiency” = the fraction of dE/dx appearing as light in water estimated to be  = 3  10-5 (lower bound) (A. De Ruhula, S.L. Glashow, Nature 312 (1984) 734) A little more on dE/dx…

  39. in the atmosphere: a = 1.2 10-3 g cm-3; b = 8.6 105 cm; H  50 km (T. Shibata, Prog. Theor. Phys. 57 (1977) 882.) in water: w  1 g cm-3 Arrival conditionsto the depth of KM3NeT The velocity of a nuclearite entering in a medium with v0, after a path L becomes At ~ 4000 m depth, nuclearites with masses larger than ~1015 GeV should be still fast enough to produce detectable black body light. Expected light yield >106 visible photons/cm!

  40. Nuclearites could be seen by KM3NeT (as well as all other VLVnT’s) as correlated light hits distributed in a time window of ~ 10 ms. Other possible exotic particles: Q-balls – nuggets of squarks and sleptons (“supersimetric nuclearites”…) - neutral Q-balls would absorb normal hadrons emitting pions: their signature would be as for nuclearites, combined with the GUT monopole signals - charged Q-balls would interact trough elastic collisions: would give nuclearite-like signals.

  41. KM3NeT sensitivity to exotic particles (one year of data tacking) should be at the level of 10-18 cm-2 s-1 sr-1, depending on: • The actual geometry of the telescope • The efficiency of the dedicated triggers • The efficiency of the off-line analysis (background removal, reconstruction strategy, etc.) Intensive simulations to be made after the completion of the telescope design…

  42. Other physics goals • Diffuse neutrino flux • Dark Matter • Exotic Particles • Atmospheric muons and neutrinos • Neutrino Cross Sections

  43. Atmospheric muons and neutrinos • More than 108 atm. muon (downward going) events expected each year: excellent callibration source, and CR primary composition from 10 TeV to 10 PeV • About 100 000 atmospheric neutrino (upward going) events expected each year: very good statistics above 1 TeV, the tomography of the Earth interior possible, for E>10TeV.

  44. Flavor analysis From pion photo-production: At distances >> oscillation length: For atmospheric neutrinos with E > 1 TeV, oscillation effects become negligible. Flavor ratio at H.E. will test neutrino production mechanisms, but also hypothesis about : - neutrino decays - neutrino oscillations into sterile states - CPT & Lorentz invariance violations ….

  45. Other physics goals • Diffuse neutrino flux • Dark Matter • Exotic Particles • Atmospheric muons and neutrinos • Neutrino Cross Sections: neutrino – nucleon interactions at very high energies (>> 200 GeV) • …

  46. Earth and sea sciences - continuous data collection for long periods at “high” (~1Hz) rates. - water dynamics, bioluminiscence and bioacoustics as byproducts of the telescope itself. - geophysics and seismology, geotechnics, chemistry, bio-chemistry, oceanography, biology, fisheries, environmental sciences… from dedicated junction boxes.

  47. KM3NeT will be part (node) of: EMSO – European Multidisciplinary Seafloor Observatories GMES – Global Monitoring for Environment and Security

  48. Present status, pilot experiments • KM3NeT – Design Study completed (FP6) • KM3NeT – Preparatory Phase ongoing (FP7, will end in 2012) • Construction and deployment foreseen to start mid 2012 or beginning 2013 • Telescope fully operational in 2016?

  49. KM3NeT takes advantage on the 3 pilot experiments ANTARES All in the Mediterranean Sea Most of the involved people are members of the KM3NeT NEMO NESTOR

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