C. Spiering, CERN School Zeuthen, Sept.2003

Transcription

1 C. Spiering, CERN School Zeuthen, Sept.2003

2 Neutrinos Cosmic Neutrinos - solar neutrinos (kev MeV) - neutrinos from a Supernova (MeV) - atmospheric Neutrinos (GeV) - extraterrestrial neutrinos (GeV-TeV-PeV) Low energy neutrinos: SN1987A and Sun High energy neutrino astrophysics - The mystery of high energy cosmics rays - TeV gamma observations - Neutrino telescopes - Amanda - Neutrino detection at ultra high energies

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4 energy spectrum of electrons from β - decay expected for 2-particle final state ν

5 m(ν e ) = 0 ev m(ν e ) = 20 ev Elektron Energy (kev)

6 Status 2003: ν e Moscow, Mainz The Future: Sensitivity Karlsruhe ν e... from WMAP follows: sum of all 3 neutrinos masses < 0.65 ev!!

7 n e - e - ν 2 n ν ν p p β e.g.. 76 Ge Present Limit ~ 0.3 ev Future: m ν down to 0.01 ev e (works only for Majorana neutrinos)

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9 All 3 Neutrinos are lighter than 2.2 ev! Observed for - solar neutrinos and reactor neutrinos m 2 ~ (10 mev) 2 - atmospheric neutrinos and accelerator neutrinos m 2 ~ (50 mev) 2

10 Solar Neutrinos: One reaction per 100 billions of ν 1 TeV: Every hundred th neutrino interacts TeV: The Earth is opaque even for neutrinos.

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13 Magellanic Clouds

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16 e + p n + ν e ms γ + γ ν x + ν x s Kamiokande (Japan) 12 Events IMB (USA) 8 Events Baksan (Russia) 3 Events Temperature in young neutron star ~ 40 Mia K Neutrino mass < 23 ev

17 Temperature in core ~ 15 Mio K Photon propagation through 0.6 Mio km radiation layer: some million years Neutrinos: 2 seconds

18 Proton-Proton-Cycle

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20 Kamioka

21 The Homestake Experiment Inverse Beta-Decay ( Neutrino-Capture ) 600 Tons Perchlor-Ethylene ( )

22 Result of Homestake Expectation Measured In 30 years 2000 neutrinos...

23 ν - Kamiokande: The sun in neutrinos

24 Deficit confirmed by other experiments ν e 100% electron neutrino flux from Sun 80% 60% 40% 20% 0% Gallex Super-Kamiokande Homestake Slide from W.Hofmann

25 Neutrino Oscillations? Neutrinos have mass SNO: Sudbury Neutrino Observatory Slide from W.Hofmann

26 ν e Deuterium Atoms in SNO Tank ν ν p pn p n Neutrino Flux From the Sun e Charged Current only ν e 100% 80% ν e ν µ ν τ Neutral Current all ν 60% 40% ν e Slide from W.Hofmann 20% 0% Neutrinos change Their identity on the Way from Sun to Earth!

27 solar and reactor neutrinos m 2 ~ (10 mev) 2 atmospheric neutrinos and accelerator neutrinos m 2 ~ (50 mev) 2 Hierarchy or Degeneration? Masse (ν i ) / ev ν 1 ν 2 ν 3 Masse (ν i ) / ev ν 1 ν 2 ν 3 Slide from W.Hofmann

28 Raymond Davis jr. Masatoshi Koshiba

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30 E max ~ β B L

31 16 Crab Nebula

32 20 VLA image of Cygnus A

33 at > ev around knee

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35 Gammaquant Particle Shower Gamma Rays from 100 GeV 10 TeV ~ 10 km Cherenkov Light ~ 1 o ~ 120 m

36 Supernova Remnant: Crab Nebula AGN: Markarian 501 All observations consistent with Synchrotron radiation at low energies Inverse Compton scattering at high energies

37 Neutrino Telescopes in Water and Ice Super-K µ Antares Nestor Baikal Km3: Nemo ν Amanda Km3: IceCube

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40 First Underwater Telescope First Neutrinos underwater 4-string stage (1996)

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44 Neumayer Amundsen-Scott Vostok Mirny Mc Murdo Concordia Antarktis Dumont D Urville

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46 Dark sector AMANDA Sky Way Dome

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51 depth Super-K AMANDA-II DUMAND Amanda-II: 677 PMTs at 19 strings ( )

52 myon cascade

53 CC muon neutrino interaction track ν µ µ

54 CC electron and tau neutrino interaction: ν (e, + N (e, τ) + X τ,) NC neutrino interaction: ν x + N ν x + X Cascades

55 spase-amanda SPASE air shower arrays 1 km calibration of AMANDA angular resolution and pointing! resolution Amanda-B10 ~ km results in ~ 3 for upward moving muons (Amanda-II: < 2 )

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58 Point source search

59 679 events below horizon above horizon: mostly fake events

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61 no indication of clustering at higher energies increasing energy deposition

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63 Crab - Nebula Cyg-X1 LMC SMC 30 kpc = ly

64 µ cm -2 s Südhimmel 4 Jahre Super-Kamiokande Nordhimmel 170 Tage AMANDA-B10 8 Jahre MACRO Sensitivität für AMANDA SS Deklination (Grad) Mk-501 ν/γ ~ 1

65 Diffuse Flux

66 Search for diffuse excess of extraterrestrial high energy neutrinos DUMAND FREJUS MACRO γ bound Muons in Amanda-B10 (1997) WB bound Expectation Amanda-II, 3 years Expectation IceCube, 3 years log E ν /GeV

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68 All-flavor limits Assuming ν e :ν µ :ν τ =1:2:0 at source ν e :ν µ :ν τ =1:1:1 at Earth factor 3 applied to ν µ channel AMANDA-II cascades 2000 ν µ analysis will yield all-flavour limit comparable to cascade limit

69 Differential all-flavor limits

70 BATSE:

71 - Low background (due narrow time and space coincidence) - Large effective areas Ψ=20 0 Upper limit: 16 Waxman/Bahcall flux Year 1997 # of GRB 78 Bkgd 0.06 seen events t=0+1h Total Waxman/Bahcall 99

72 χ ν 1. Neutrinos from the Center of Earth Assumptions: -Darkmatter in Galaxy due to neutralinos - Density 0.3 GeV/cm 3 χ + χ b + b C + µ + ν µ

73 Upper limits on muon flux from neutralino annihilations in center of Earth Green dots: Excluded by present direct searches Baikal 98/99 data Blue crosses: can be excluded by 10 times more sensitive direct searches

74 χ (b) Neutrinos from the Sun χ ν Amanda At South Pole the Sun sinks maximally 23 below horizon. Therefore only Amanda-II with its dramatically improved reconstruction capabilities for horizontial tracks (compared to Amanda-B10) can be used for solar WIMP search.

75 Upper limits on muon flux from neutralino annihilations in center of Sun AMANDA-II results: based on 193 days of live time Exclusion sensitivity from analyzing the off-source bins Will un-blind data soon and look to the Sun. ANTARES and ICECUBE: MC-calculated sensitivities

76 preliminary AMANDA (number of muons) 1 km 2 km Iron Proton log(e/pev) Spase (number of electrons)

77 03-04 drill equipment to Pole first strings (proof that 16/season are feasible, prepare 10 full strings) strings strings strings strings remaining strings Overall cost with personnel, contingency, overhead: ~ 250 M$ Detector: ~ 55 M$ Logistics, including drilling: ~ 40 M$

78 IceTop AMANDA South Pole - 80 Strings PMTs - Instrumented Volume: 1 km 3 - Installation: m ~ atm.ν per Jahr 2400 m

79 10-14 µ cm -2 s -1 Expected sensitivities for static point sources SS GX Mk-501 ν/γ ~ typical predictions for AGN, SNR,... typical predictions for AGN, SNR,

80 upper limit (cm -2 s -1 sr -1 ) Soudan KGF Baikal MACRO Orito Amanda δ electrons 0.50 IceCube β = v/c Relativistic Magnetic Monopoles Cherenkov-Light 2 2 n = 1.33 (g/e) = 137 / 2

81 Supernova-Monitor B10: 60% of Galaxy A-II: 95% of Galaxy Amanda-II Amanda-B10 Count rates sec IceCube: Up to LMC IceCube

82 Under construction: 2400m ANTARES NEMO 3400m 4100m NESTOR

83 Point sources: Fraction of time sky below horizon south detector + north detector

84 Above PeV: 10 cm P 50 µs t attenuation length in ice 1-4 km!! nsec 5-10 m

85 Radio Ice Cherenkov Experiment Firn ice (down to 120 m depth) 20 transmitter + receiver UHE NEUTRINO DIRECTION E 2 dn/de < 10-4 GeV cm -2 s -1 sr METER DEPTH at 100 PeV

86 Antarctic Impulsive Transient Array Flight in January 2006

87 Goldstone Lunar Ultra-high Energy Neutrino Experiment Lunar Radio Emission from Neutrino Reactions at > ev Gorham et al. (1999), 30 hr NASA Goldstone 70 m antenna + DSS 34 m antenna ν 1 nsec moon Earth Effective target volume ~ antenna aperture (0.3 ) 10 m stone layer E 2 dn/de < 10-4 GeV cm-2 s-1 sr-1 at ev 5 3

88 Atmosphere Far inclined showers ( thousand per year) p Deep inclined showers (~ one per year?) Flat and thin shower front Narrow signals Time alignment Hard µ s Atmosphere ν Curved and thick shower front Broad signals Soft µ s + e.m. 2001: AGASA (Japan) < 10-5 GeV cm-2 s-1 sr-1 for E > 10 EeV el.-magn. cascade from ν e hard muons from CR

89 E > GeV 500 km 60 Masse Up to 10 Tera-Tons Area up to 10 6 km 2

90 RICE AGASA 2002 Amanda, Baikal GLUE AABN AUGER ν τ Anita 2012 km 3 Auger Salsa EUSO

91 Success not guarantied, but history is on our side