AMANDA: proof of concept Atmospheric Neutrinos Cosmic Ray e+ + e π+ Atmospheric Muons & Neutrinos 102 Hz atm.
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AMANDA: proof of concept Atmospheric Neutrinos Cosmic Ray e+ + e π+ Atmospheric Muons & Neutrinos 102 Hz atm. astrophysical • “Atmospheric muons” from cosmic ray showers, penetrating to the detector from above • “Atmospheric neutrinos” from the same air showers, forming a diffuse background and calibration beam atm. 10-4 Hz • Astrophysical neutrinos: interesting signal Detector medium: ice to meet you Scattering Absorption bubbles ice dust dust Measurements: ►in-situ light sources ►atmospheric muons • Scattering length 6 ~ 52 m • Absorption length 9 ~ 240 m Optimized 2002 analysis zenith distribution 10 events per day: •improved reco •no cuts 10,000 in 00-05 ATMOSPHERIC Neural Network energy reconstruction Regularized unfolding → energy spectrum & DIFFUSE FLUX LIMITS [] AMANDA test beams: atmospheric and First spectrum > 1 TeV (up to 100TeV) Neutrino fluxes vs. Energy Neutrino Energy spectrum Volkova flux parameterizations H.Geenen Previous analysis publication Phys. Rev. Lett. 90 251101 (2003) Includes 33% systematic uncertainty (GeV) 104 105 E Last bin info to calculate the limit to Extraterrestrial E2 neutrino flux E2μ(E) < 2.58·10–7 GeV cm-2 s-1 sr-1 IceCube IceCube Neutrino Observatory IceTop shower array 80 pairs of Cherenkov tanks IceCube 4800 optical modules on 80 strings Digital Optical Module Photomultiplier Tube 300 m size vs threshold 1500 m 50 m 2500 m South Pole: AMANDA IceCube IceCube 01/05 • drilling • 60 modules Drill modules at McMurdo IceTop – IceCube coincident muon µ-event in IceCube 300 atmospheric neutrinos per day AMANDA II IceCube: Larger Telescope Superior Detector 1 km Event Simulation in IceCube E = 10 TeV E = 375 TeV e muon event shower event ~300m for 10 PeV double shower event PeV (300m) decays Signatures in IceCube … 1013 eV (10 TeV) 6x1015 eV (6 PeV) Multi-PeV B10 +N+... ± (300 m!) +hadrons signature of signature of GZK event in AMANDA and IceCube SUPERNOVA SEARCH ’97 + ‘98 AMANDA-B10 with 302 OMs Selection of very stable OMs SN Signal proportional To number of OMs ! AMANDA-II with 677 OMs AMANDA-II CRUCIAL = LOW NOISE 215 Days live time; 90% = 9.8 kpc AMANDA-B10 Count rates Simulation (IceCube) IceCube 30 kpc 0 Astropart.Phys. 16 (2002) 345 70% of Galaxy coverage sn < 4.3 Event yr-1 5 10 sec B-10: 70% of Galaxy A-II: 95% of Galaxy IceCube: up to LMC Joined SNEWS (SuperNova Early Warning System) [with Super-K, SNO, Kamland, LVD, Boone] neutrinos: the sun and the Earth Symmetry Magazine 3 1 natural particle beams • Sun: resolution of solar neutrino puzzle ’s have mass John Bahcall understands how the sun shines • Supernova 1987A: 20 events only! confirmed basic scenario for the death of a star set records on neutrino properties • Cosmic neutrinos? Discovery, but also 106 atmospheric and 103 supernova neutrinos origin of cosmic rays beam for particle physics AMANDA performance ( Antares, Nestor soon ) •’s per day : •total statistics 3.5 10 per day 10,000 in 00-05 •energy 0.1 ~ 1,000 TeV IceCube -KM3NET •’s per day : > 100 per day •total statistics > 106 over 10yr •energy 0.1 ~ 10,000 TeV Neutrino Astronomy Explores Higher Dimensions atmospheric range 100 x SM GZK range TeV-scale gravity increases PeV -cross section IceCube tests • equivalence principle and • Lorentz invariance …general relativity will not last 200 years… M. Turner Cosmic neutrino beam from the decay of pions e : : ~ 1 : 2 : <10-5 @ the source e : : ~ 1 : 1 : 1 @ the detector Or, (maximal mixing) • zero mass eigenstates in vacuum • neutrino decay • neutrinos of varying mass cosmic anti - e beam from neutron decay directional cosmic rays from the Cygnus region and from the center of the galaxy e ? @ the source @ the detector •Measure sin2q13 from flavor composition at the detector •Decoherence? WIMP Capture and Annihilation c n DETECT c+cW+W+ WIMP search Limits on muon flux from Earth Limits on muon flux from Sun AMANDA 1y SK Disfavored by direct search (CDMS II) Antares 3 years 1km3 (IceCube) IceCube : particle physics with one million atmospheric neutrinos • Astronomy: new window on the Universe • Physics: • • • • • • • • measurement of the high-energy neutrino cross section TeV-scale gravity, quantum decoherence physics beyond 3-flavor oscillations test special and general relativity with new precision search for magnetic monopoles search for neutralino (or other) dark matter search for topological defects and cosmological remnants search for magnetic monopoles RICE Radio Detection in South Pole Ice Neutrino enters ice Neutrino interacts Antenna & Cable • Installed ~15 antennas few hundred m depth with AMANDA strings. • Tests and data since 1996. • Most events due to local radio noise, few candidates. • Continuing to take data, and first limits prepared. • Proposal to Piggyback with ICECUBE Cube is .6 km on side Two cones show 3 dB signal strength Antarctic Impulsive Transient Antenna Experiment ANITA Solar panels Antenna array Overall height ~8m ANITA Gondola & Payload RF Cherenkov air searching for GZK neutrinos with radio detection in Antarctic ice solid neutrino Cascade: ~10m length particle astrophysics • techniques of particle physics reborn to do astronomy • not mentioned: CCD development, massive data handling/analysis techniques … • cosmic ray puzzle will be solved less than 100 years after their discovery The real voyage is not to travel to new landscapes, but to see with new eyes. . . Marcel Proust conclusions • techniques of particle physics reborn to do astronomy • may still do particle physics ( mass ! ) • cosmic ray puzzle will be solved less than 100 years after their discovery