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Neutrino Astroparticle Physics

Neutrino Astroparticle Physics. XXV Physics in Collision. Lutz Köpke University of Mainz, Germany July 8, 2005. probe physics beyond LHC. 50 GeV 1.4 TeV 40 TeV 1400 TeV. 10 18. 10 21. eV. 1 0 12. 10 15. Physics in collisions?. actually not ... fixed target physics:.

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Neutrino Astroparticle Physics

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  1. Neutrino Astroparticle Physics XXV Physics in Collision Lutz Köpke University of Mainz, Germany July 8, 2005

  2. probe physics beyond LHC 50 GeV 1.4 TeV 40 TeV 1400 TeV 1018 1021 eV 1012 1015 Physics in collisions? actually not ... fixed target physics: center of mass energy neutrino energy atmospheric neutrinos GZK: p+CMB n+X+ ...limits exist all the way up to 1025 eV

  3. pp  ± + X  e,.... • p  + + X  e ,.... Beam dump: Physics motivation ... astrophysics and particle physics • origin and acceleration of cosmic rays • understand cosmic cataclysms •  find new kind of objects? •  neutrino properties ( , cross sections ..) •  dark matter (neutralino annihilation) • tests of relativitiy .... • search for big bang relics ... • effects of extra dimension etc. ...

  4. protons E<1019 eV protons E>1019 eV (30 MLy) neutrinos Protons/nuclei: deviated by magnetic fields, reactions with radiation (CMB) Particle propagation in the Universe gammas (0.01 - 3 MLy) Cosmic accelerator Katz Photons: absorbed on dust and radiation

  5. Active Galaxy (optically dense, e.g. FRII)  106 Ly Black hole with 108 x mass of sun extra-galactic Neutrino source candidates Microquasar (SS433 etc.) Supernova remnant  1 Ly Crab nebula Black hole with  mass of sun galactic

  6.  Mannheim, Protheroe and Rachen (2000)  Waxman, Bahcall (1999) derive generic limits from  limits on extragalactic p‘s -ray flux MPR bound WB bound Required sensitivity ... for discovering extraterrestrial neutrinos many specific models for non-resolved sources ... -5 atmospheric -6 log [E2 · flux(E) / GeV cm-2 s-1 sr-1] -7 GZK AGN core (SS) -8 AGN Jet (MPR) GRB (WB) -9 log (E /GeV) 2 3 4 5 6 7 8 9 10 TeV PeV EeV

  7. Extended source with e:: =1:2:0 production (e.g.  decay): for 23 45°, 130°: e:: =1:1:1 on earth Can it be done ? Haim-Harrari: neutrino physics is the art to learn a lot from nothing .... Reaction probability [H2O, d=1km]: W=NAd  4 •10-7 • E[TeV] ... sources millions to billions light years away ...  Needs huge detectors making use of natural media  Require high energies  Need to detect all flavors

  8. extremely high energies (E>1018 eV) moon, ice, salt mountain ... radio, acoustics, particles ... detectors (earth based, balloon/satellite) Principle detection methods high energies (E> 1011 eV) grid of light sensors for Cherenkov radiation

  9. Single photon detection ... information: timing and amplitude of photons - position of PMTs IceCube …typically 300 MHz digitization

  10. O(km) long muon tracks Electromagnetic and hadronic cascades  15 m ~ 5 m direction determination by Cherenkov light timing Detection of  ,e , O(10) x less background for e – but you don’t profit from long -range  Regeneration of  - no absorption in earth even at very high energies !

  11. KM3Net? Antares Nestor Nemo The neutrino telescope world map Baikal Amanda/IceCube

  12. Mediterranean (ocean) Antares, Nestor, 1 km3 ... Importance of complete sky coverage Need earth as shielding agains cosmic rays for  (if E< 100 TeV) South Pole (ice) AMANDA, ICECUBE galactic center in middle 4  coverage for e ,  !

  13. Neutrino flavor nt Full flavor ID supernovae ne IceCube flavor ID, direction, energy ne Showers vs tracks IceCube triggered, partial reconstruction nm 9 12 18 21 6 15 TeV PeV Log(ENERGY/eV) Importance of large energy coverage

  14. Nestor Importance of low background cosmic ray muons : 105-106 x dominated by cosmic ray muons  need low misreconstruction e: background much lower (but smaller detection volume)  scattering helps ... Detector noise: low in inert ice (1 kHz/PMT) IceCube

  15. Importance of good angular resolution Expected  resolution for 1 km3 detectors ...can‘t compete with -telescopes ..but for many analyses not crucial Ice size of moon water atmospheric 

  16. moon water ... use existing moon …and radio antennas KM3Net: < 200 MEUR Price and ease of construction Ice IceCube: M$273 (US accounting) 50 M$ detector cost

  17. NESTOR Astrop. Phys. 23, 377 (2005) Northern hemisphere detectors Baikal NT200 Antares Nestor 1100 m deep data taking since 1998 new: 3 distant strings under construction 2400 m deep completion: early 2007 1 of 12 floors deployed 4000 m deep completion: 2007?

  18. BAIKAL NT200+ Excellent example that smart ideas can compensate small size and budget … concentrate on  induced showers data taking since 1998 3 external strings in operation since April 05 sensitivity quadrupled

  19. submarine cable Antares string based detector, 0.01 km3 instrumented volume prototype strings 2003, March 2005 1st „final“ string mid 2005 detector completion early 2007 40 km ~ 40 km -2400m

  20. ... detectors moving with currents…. acoustic positioning < 10 cm (2mm for fixed distance) Antares test string 2005 string based detector, 0.01 km3 instrumented volume  1st „final“ string mid 2005  detector completion early 2007

  21. Optical module (677) AMANDA and IceCube ..collaborations merged March 2005 ... 0.02 km3 AMANDA 1 km3 IceCube IceTop 0 m 1996-2000 1400 m 2400 m > 70 strings > 4200 modules  1500 atmospheric ‘s /year  80000 atmospheric ‘s /year

  22. the South-Pole laboratory First IceCube string 1400m 2400m South Pole Station IceCube Counting House 1500 m AMANDA 2000 m [not to scale]

  23. The new station operating at least until 2035

  24. First IceCube string ... January 2005: 60 optical modules Deepest module at 2450 m

  25. Amanda – IceCube IceCube coincident events .. IceTop – IceCube

  26. atmospheric neutrinos Eν E-3.8 Frejus Amanda 1 GeV 1 TeV The testbeams Energy spectrum with unfolding technique cosmic ray muons Eμ E-3.8 Eprimär E-2.7 EHadrfon E-2.7 0.02 1 TeV 1000 TeV ... Primary energy corrected Preliminary

  27. Atmospheric neutrinos ... IceCube will be abundant source of atmospheric neutrinos: AMANDA (5y)  10000, 70 between 10-100 TeV IceCube (5y)  300000, 2000 between 10-100 TeV e.g. study of equivalence principle, velocity induced oscillations: 2 orders of magnitude improvement in sensitivity

  28. Expect deviation at high energy (hard flux) cascades (2000 data) Neutrinos from unresolved sources  (2000 data) Preliminary

  29. Very high energies Special analysis for very high energies above 1000 TeV ....  large energy deposits (bremsstrahlung)  Earth starts absorbing  70 TeV: interaction length = earth diameter AMANDA reach (5y): 10-7 cm-2 s-1 sr-1 90% energy range: 1.8 105 - 1.8 109 GeV

  30. ..closing in on Waxman-Bahcall bound  gain factor 30 in sensitivity with 1 km3 detectors present AMANDA sensitivity IceCube (3y) --- Preliminary Experimental bounds and future DUMAND test string FREJUS MACRO atmospheric -5 AMANDA limits -6 BAIKAL log [E2 · flux(E) / GeV cm-2 s-1 sr-1] -7 GZK -8 -9 2 3 4 5 6 7 8 9 10 log (E /GeV)

  31. Maximum significance 3.4  compatible w. atmospheric  Search for localized sources (AMANDA) Preliminary quite expected ... 92% of experiments would yield even higher maximum 2000-2003 (807 days) 3329  from northern hemisphere 3438  expected from atmospheric  also search for neutrinos from unresolved sources

  32. Antares+Nestor AII+IceCube 2007 KM3NetIceCube 2012 ... measured limits and future 10-12 Macro Super-K 10-13 IMB Baksan Amanda 10-14 neutrino induced muon flux /(cm2 s) 10-15 10-16 10-17 10-18 declination (degrees)

  33. 1997 : ApJ 583, 1040  (2003) 2000 : PRL 92, 071102 (2004) 2000-02 : PRD 71 077102 (2005) IceCube: Astrop Phys 20, 507 (2004) * AMANDA-B10 average flux upper limit [cm-2s-1] AMANDA-II IceCube 1/2 year sin(d) ... steady progress in sensitivity optimized for E-2, (*) E-2, 3 signal * >10 GeV lim  0.68·10-8 cm-2s-1 time Preliminary

  34. ... closing in on predictions  predictions very model dependent ... some can be tested now .. e.g. SS-433 micro quasar: 10-5 SS-433 10-6 integrated neutrino flux /(cm2 s) [E>1 GeV] 10-7 Distefano 2002 10-8 preliminary

  35. May '02 June '02 July '02 Additional studies  Search for excess in galactic plane  Search for neutrino clusters (sliding time window)  coincidence with enhanced EM emision x-ray, radio and -ray) curosity: 1 neutrino candidate close to orphan peak (no radio signal) ...no statistically significant effects need multiwavelength campaigns! sliding search window Error bars: off-source background per 40 days

  36. GRB n search in AMANDA Search for  candiates correlated with GRBs - background established from data : <20° PRELIMINARY Cascade channel: worse pointing but 4! effective area  50000 m2 ()  limit assumíng WB spectrum: Eν2Φν < 3 x 10-8 GeV cm-2 s-1 sr-1() < 9.5x10-8 GeV cm-2 s-1 sr-1(cascades) No coincident events observed observed!

  37. SuperKamiokande (1454) AMANDA sensitivity AMANDA limit Further investigations ... Green’s Function Fluence Limit(allows for comparison with SK)  Search without temporal/spacial constr.: Eν2Φν < 6.7x 10-6 GeV cm-2 s-1 sr-1  detailed investigations of GRB 030329 - large model dependencies !! Future goal: determination of limits independent of specific model PRELIMINARY

  38.  can self-annihilate (Majorana particle) and produce neutrinos  gravitationally trapped in center of earth, sun or center of galaxy e.g.: +   b + b ; W+W- c + - +  Indirect search for dark matter neutralino is best particle physics candidate for dark matter  stable if R-parity conserved (for most parameters)  Nuclear Recoil and indirect searches are complementary and not equivalent !!

  39. Limits on muon flux from Sun AMANDA 1y SK Antares 3 years 1km3 (IceCube) WIMP search in AMANDA AMANDA results submitted for publication Limits on muon flux from Earth center Disfavored by direct search (CDMS II)

  40. New particles 10-14 Soudan high sensitivity to rare new particles if signature unambigous .... ... (slowly) moving bright particles ... KGF Amanda MACRO 10-15 Orito upper limit (cm-2 s-1 sr-1) 10-16 Baikal e.g magnetic monopoles: Cherenkov-light  (n·g/e)2 (1.33*137/2)2  electrons 10-17 1 km3 10-18 8300 times stronger than for ! 0.50 0.75 1.00  = v/c

  41. The (near) future complete construction of 1 km3 IceCube detector 2010 can already work with incomplete detector …  complete construction of smaller mediterranean detectors 2007?  decide on location/design of 1km3 mediterranean detector 2006?  Complete construction of KM3Net? 2012?  new ideas for detection of extremely high energy neutrinos ....  extend the search to higher energies with even bigger detectors

  42. IceCube: 11/2004 - 9/2010 Up to 18 holes per season: Nov.:preparation Dec.:construction Jan.:construction Feb.:commissioning 35% of money spent ...

  43. Signatures in IceCube … 1013 eV (10 TeV) 6x1015 eV (6 PeV) Multi-PeV  +N+... ± (300 m track!)  +hadrons signature of  signature of

  44. 1 km3 array in Mediterranean •  Extensive exploration and R&D (NEMO) •  efforts of all groups (Antares, Nestor, Nemo) • being joined to form single collaboration • EU-funded design study (10 M€ requested) • on list of proposed large EU-projects (ESFRI) • problems mainly „political“ (site e.g.) • new technological develoments design report 2008 construction 2009-2013? multianode PMTs with Winston cones) .... but time scale tight

  45. refracted radio Antarctic ice Anita - quest for GZK neutrinos surveys > 1 million km2 under construction launch Dec 2006 neutrino

  46. Preliminary! ... very rare - very high energy events many proposals for radio and acoustic detectors in ice, water, salt, from moon .. e.g. IceCube extension: >>km attenuation length sparse instrumentation 100-fold volume increase >100 > 10 GZK neutrinos/year IceCube

  47. RICE AGASA Glue 2002 Amanda, Baikal AUGER nt Anita 2004 0.1 km3 2008 km3 later satellites radio

  48. Summary ..no extraterrestrial neutrinos found yet ...but: plenty of results (limits) closing in on predictions … • 1 km3 IceCube  construction started • 30 times efffective area • mediterranean detectors under construction • taskforce for 1 km3 detector • innovative concepts for even larger detectors

  49. Source Nr. of n events (4 years) Expected backgr. (4 years) Flux Upper Limit F90%(En>10 GeV) [10-8cm-2s-1] Markarian 421 6 5.58 0.68 1ES1959+650 5 3.71 0.38 SS433 2 4.50 0.21 Cygnus X-3 6 5.04 0.77 Cygnus X-1 4 5.21 0.40 Crab Nebula 10 5.36 1.25 ... Limits on selected sources Sensitivity/~2 for 200 days of “high-state” (HEGRA) Crab Nebula: MC probability for excess 64% … out of 33 Sources Systematic uncertainties under investigation selected objects → no statistically significant effect observed

  50. IceCube Effective Area and Angular Resolution for Muons Galactic center • for a E-2nm spectrum • with quality selection and BG suppression (atm m reduction by ~106) • Median angular • reconstruction uncertainty ~ 0.8 • further improvement • expected using waveform info Energy resolution: s[log10(Em)]  20%-30%

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