Probing neutrino flavor transition mechanism with ultrahigh energy astrophysical neutrinos
Neutrino Telescopes and Neutrinos from LHC Neutrino Telescopes and Neutrinos from LHC ISPM – 2005...
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Neutrino TelescopesNeutrino Telescopesandand
Neutrinos from LHCNeutrinos from LHC
ISPM – 2005ISPM – 2005Physics at the future colliders Physics at the future colliders
17-21/10/2005, Tbilisi, Georgia17-21/10/2005, Tbilisi, Georgia
Rezo ShanidzeUniversity of Erlangen-Nuremberg
& IHEPI, Tbilisi State University
Neutrino TelescopeNeutrino Telescope Detector for registration of high energy extra-terrestial neutrinos.
High energy extra-terrestial radiation (cosmic rays, gamma radiation, neutrinos) – detected with the help of methods developed in particle physics. High Energy Astrophysics / Astroparticle Physics / Particle Astrophysics: understanding the nature of cosmic high energy phenomena. Energy of the highest energy CR: ECR > 1020 ev (108 TeV ~ x 10 7 LHC beam)
21.11.2005 21.11.2005 Rezo shanidzeRezo shanidze 33
Astroparticle PhysicsAstroparticle Physics PAO
ANTARES
H.E.S.S
The High Energy Cosmic Radiation
ultrahigh energy ’sassociated with the sources of
high energy cosmic rays top-down scenarios:decays of massive cosmological relics bottom-up scenarios:
”cosmic accelerators”accreting black holes (eg AGN)colliding neutron stars/ black holes
fireball (eg GRB)
cosmogenic ’s supernova ’s dark matter WI MP, Kaluza-Klein exotica monopoles, Q-balls,
mini black holes
p + (p or ) e ,
The Science ultrahigh energy ’s
associated with the sources ofhigh energy cosmic rays
top-down scenarios:decays of massive cosmological relics bottom-up scenarios:
”cosmic accelerators”accreting black holes (eg AGN)colliding neutron stars/ black holes
fireball (eg GRB)
cosmogenic ’s supernova ’s dark matter WI MP, Kaluza-Klein exotica monopoles, Q-balls,
mini black holes
p + (p or ) e ,
ultrahigh energy ’sassociated with the sources of
high energy cosmic rays top-down scenarios:decays of massive cosmological relics bottom-up scenarios:
”cosmic accelerators”accreting black holes (eg AGN)colliding neutron stars/ black holes
fireball (eg GRB)
cosmogenic ’s supernova ’s dark matter WI MP, Kaluza-Klein exotica monopoles, Q-balls,
mini black holes
p + (p or ) e ,
The Science
Cosmic accelerators -
Where and how Cosmic Particles get energy >1019 eV?
Most energetic astrophysical Objects: AGN, GRB, SN,…?
Bottom-up models:
Top-down models:
Decays of heavy particles, …?
CM
B
CMB
CMB
CMB
CMB
21.11.2005 21.11.2005 Rezo shanidzeRezo shanidze 66
UHECR: EAS/FluorescenceUHECR: EAS/Fluorescence
Ei(xi,ti) E(m0,,)MC codes: HEMAS,CORSIKA,…MC codes: HEMAS,CORSIKA,…
GZK cut-off ?
GZK cut-off
Greisen- Zatsepin- Kuzmin
EAS
Fluorescence
(AGASA/HiRes)
Ep> 1019 eV: p +CMB N
EiEi
Extensive Air ShowersExtensive Air Showers
Cosmic Ray Sources ?Cosmic Ray Sources ?
AGASA UHECR:E> 4 x 1019eV (72 events)4-10 x1019 eV, E>1020 eV (11 events) ApJ, 522(1999), 225
Galactic plane survey by H.E.S.S. VHE ( > 200 GeV )
or ee + ? (Inverse Compton Scattering)
UHECR and VHE propagationis affected by CMB radiation.
High Energy cosmic neutrinos do not Interact with CMB !
21.11.2005 21.11.2005 Rezo shanidzeRezo shanidze 88
High Energy High Energy -Astronomy-Astronomy
CC intearctions: High energy has a longe range (~ km) in water/ice and produce Cherenkov radiation.
Sources of high energy cosmic
e e
Weak decays of hadronse =2 : 1 : 0
e : =1 : 1 : 1
+ N ()+X
-interactions:
t ~ 0E0.363
0=7.84x1036cm2
W(Z)
cosc= 1/n
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21.11.2005 21.11.2005 Rezo shanidzeRezo shanidze 1010
Baukal NT First Baukal NT First Telescope Telescope
BAIKAL NTBAIKAL NT(36, 96, 192)(36, 96, 192)
1.1 km depth 1.1 km depth
Baikal Neutrino Telescope
Started: 1993
Russia/Germany(INR, MSU, JINR, … /DESY Zeuthen)
Fisrt event
4 km from shore 1070 m deep
1998-1999 Data
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AMANDAAMANDA Detector Detector AAntarctic ntarctic MMuon uon AAnd nd NNeutrino eutrino DDetector etector AArrayrray
Location:South Pole
Collaboration of 19 Instititions from US/Europe/ Venezuela
AMANDA B10 (97-99): 10 strings,302 OM
AMANDA II (2000):19 strings677 OM
(http://amanda.uci.edu)
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ANTARES ANTARES -Telescope-Telescope
2005-2007: deployment of the full detector
12 lines
25 storeys/line
3 PMT/storey
900 PMT
for high energies: < 0.3o (Quality of water!)
14.5m0.1 km2
21.11.2005 21.11.2005 Rezo shanidzeRezo shanidze 1414
21.11.2005 21.11.2005 Rezo shanidzeRezo shanidze 1515
The Sky ViewThe Sky View for High Energy NT for High Energy NT
AMANDAAMANDAANTARESANTARES
ANTARES - 2/3 of time: Galactic CentreANTARES - 2/3 of time: Galactic Centre
21.11.2005 21.11.2005 Rezo shanidzeRezo shanidze 1616
High Energy Neutrino TelescopesHigh Energy Neutrino Telescopes
AMANDA/IceCube
Baikal
NESTOR
ANTARESANTARES
NEMONEMO
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kmkm33 scale scale : IceCube : IceCube @South Pole@South Pole
Digital Optical module (DOM)
a self -contained ”mini”-DAQ
records timestamps digitizes stores transmits to
surface at request
an optical sensor10 inch Hamamatsu R-7081
mu metal cage
PMT
penetrator HV board
flasher board
DOMmain board
pressure sphere
optical gel
delay board
Dark noise rate < 1 kHz SN monitoring within
our Galaxy
Digital Optical module (DOM)
a self -contained ”mini”-DAQ
records timestamps digitizes stores transmits to
surface at request
an optical sensor10 inch Hamamatsu R-7081
mu metal cage
PMT
penetrator HV board
flasher board
DOMmain board
pressure sphere
optical gel
delay board
Dark noise rate < 1 kHz SN monitoring within
our Galaxy
Collaboration: 9 countries, 26 Institutions.
80 str./ 4800 OM (2010+)
Instrumented volume: 1 km3
~80.000 atm./y
Eµ=10 TeVEµ=10 TeV
http://icecube.wisc.eduhttp://icecube.wisc.edu
The KM3NeT ProjectThe KM3NeT ProjectKM3NeT project is EU-funded Design StudyKM3NeT project is EU-funded Design Studyfor kmfor km33 NT in the Mediterranenan Sea NT in the Mediterranenan SeaConsortium: 8 EU countries / 35 Institutions Coordinated by Erlangen University
Time Schedule:
02/2006: Start of Design Study
mid-2007: Conceptual Design Report
End-2008: Technical Design Report
2009-13: Constraction
From 2010: Data Taking
High Energy Accelerator NeutrinosHigh Energy Accelerator Neutrinos
Accelerator neutrinos with well defined energy spectra : Accelerator neutrinos with well defined energy spectra : - significantly improve Neutrino Telescope significantly improve Neutrino Telescope performanceperformance - important role in neutrino physics. - important role in neutrino physics.
VLVnT - sensitive to high energy neutrinos VLVnT - sensitive to high energy neutrinos (above ~ 50-100 GeV )(above ~ 50-100 GeV ) Currently several experiments performed/ planned with high Currently several experiments performed/ planned with high
energy accelerator neutrinos:energy accelerator neutrinos: K2K, NuMI/MINOS, CNGS, T2KK2K, NuMI/MINOS, CNGS, T2K Long-baseline neutrino experiments. Long-baseline neutrino experiments.
21.11.2005 21.11.2005 Rezo shanidzeRezo shanidze 2121
KM3NeT Design StudyKM3NeT Design Study MC simulations in Erlangen: Testing different MC simulations in Erlangen: Testing different
concepts and options for photodetectors/Optical concepts and options for photodetectors/Optical Modules and design geometryModules and design geometry..
2nd Workshop onVery Large Volume neutrino TelescopesCatania, 8-11/2005
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Long-baseline Long-baseline Beams Beams
Exp. Acc. Ep
(GeV)
L(km)
E
(GeV)
POT 1019
ND(Kt)/Events
K2K KEK 12 250 1.5 ~2
50 / 150
NuMI/MINOS FNAL 120 730 15.0 25 5 / ~10000
CERN-LNGS SPS 400 732 30.2 ~4-8 ~2000 /kt
Neutrino telescopes: 103-106 ND ANTARES - ~ 10 Mtone KM3NeT ~ 1Gtone (109 m3 ) E(LHC) > 17.5 E (SPS)
21.11.2005 21.11.2005 Rezo shanidzeRezo shanidze 2424
NuMI/MINOS ExperimentNuMI/MINOS ExperimentR.Plankett (FNAL), 23/02/2005Talk @ XI International Workshop on Neutrino Telescopes
cEmc.8m
2.5 1013 p/pulse (1.9s)n CC Events in MINOS 5kt detector (2.5 x1020 POT/y)
Low ~ 1600/yrMedium ~ 4300/yr High ~ 9250/yr
21.11.2005 21.11.2005 Rezo shanidzeRezo shanidze 2525
NT projects for Mediterranean
ExperimentExperiment Lat.(N)/Long(E)Lat.(N)/Long(E) Deep(m)Deep(m) L(km) L(km) Acc.(mrad)Acc.(mrad)
ANTARES 42o50´/ 6o10´ ~2500 ~400 0.45
NEMO 36o38´/21o35´ ~4000 ~1400 0.40
NESTOR 36o / 16o ~3400 ~1700 0.11
ANTARES
NESTOR
NEMO
KM3NeT
21.11.2005 21.11.2005 Rezo shanidzeRezo shanidze 2626
Large Hadron Collider Large Hadron Collider LHC@CERN - from 2007
Beam energy: - 7000 GeV Protons per beam: 4 x1014
Beam lifetime 14.9 hProtons/year = 200 d x(24/14.9)x41014=1.3x1017
How LHC beams are used:
1) High Luminosity pp interaction: ATLAS, CMS exprerimets (~10%) 2) Low Luminosity pp interaction: ALICE, LHC-b 3) Unused (dumped) ( ~ 80%)
Neutrinos from High EnergyNeutrinos from High Energyproton-proton Interactionsproton-proton Interactions
Neutrino sources: Neutrino sources:
- Weak decays of hadrons:- Weak decays of hadrons: unflavored: neutrons, unflavored: neutrons, Flavored : strange, charm, Flavored : strange, charm, bottombottom
-Decays of leptons (Decays of leptons () and weak) and weak bosons (W, Z)bosons (W, Z)
Charged Pions and Flavored ParticlesCharged Pions and Flavored Particles
Charged pions: Charged pions: (139.5 MeV) (139.5 MeV)
BR ( BR ( ) = 100 %, l=) = 100 %, l=cccc=7.8 m=7.8 m Strange Particles: KStrange Particles: K(493.7 MeV), K(493.7 MeV), KLL (497.6) (497.6)
BR(KBR(K ) = 63.34 % , c ) = 63.34 % , c= 3.7 m = 3.7 m BR(KBR(KLL
ee ) = 38.81 % , c ) = 38.81 % , c=15.8 m=15.8 m BR(KBR(KLL
) = 27.12 % ) = 27.12 %
Charmed mesons: DCharmed mesons: Doo(1.865 GeV ), D(1.865 GeV ), D(1.869 ) , D(1.869 ) , Ds s (1.968)(1.968)
BR(DBR(Doo eX)=6.9 % c eX)=6.9 % c=123 =123 mmBR(DBR(Doo X)=6.5 X)=6.5 BR(DBR(D±± eX)=17.2 % c eX)=17.2 % c=312 =312 mm
The LHC Interaction PointsThe LHC Interaction Points
Beam dumping Arrea
pA,14.9 h (t: 86 s),Ecm=114 GeV
pp – 25 ns, ~ 109 pp/s, Ecm=14 TeV
Neutrinos from High Luminosity IRNeutrinos from High Luminosity IR
pp interactions @ 14 TeV:pp interactions @ 14 TeV: PYTHIA 6.2 (minimal bias interactions)PYTHIA 6.2 (minimal bias interactions) pppp=100 mb , ~ 50 =100 mb , ~ 50 / pp E ~ 360 GeV/ pp E ~ 360 GeV
1 mrad angle:1 mrad angle: beam pipe: R=25 10beam pipe: R=25 10-3-3 m, L=23 m, m, L=23 m, ~ 1~ 1/pp, E/pp, E ~ 900 GeV ~ 900 GeV Decay probability:Decay probability: w(w()=1-exp(-L/)=1-exp(-L/ll) ~ L/) ~ L/ll , , =E=E/m/m w(Ew(E=100 GeV) ~ 4 10=100 GeV) ~ 4 10-3-3
~ 10~ 1066 sec (X 2 p beams X 2 IR)
Charm Production at LHCCharm Production at LHC
P
N
Q
Q
pp 2HC + X + X
Charm production at high energies:-Diffractive production (soft process) - gluon-gluon, quark-antiquark sub-process (QCD)
Caclucable in QCD:
Implemented in MC (PYTHIA) P
Neutrinos from Neutrinos from High Luminosity IR High Luminosity IR
Neutrinos from different sources:
a) from decays
b) from K decays
c) from Charm particles
Neutrinos from Neutrinos from Beam Dumpimg System Beam Dumpimg System
High energyHigh energy
neutrinos from neutrinos from charmed particles.charmed particles.
- absorbed, - absorbed, strange particles – strange particles – multiple interctions multiple interctions before decaybefore decay
pA interactions at 114 GeV
Event Rates in Neutrino TelescopesEvent Rates in Neutrino Telescopes
NN==∫ ∫ (E(E) ) (E(E) M(E) M(E) N) NAA (E(E)) dE dE
(E) neutrino flux
(E) neutrino cross-section
M(E)=Veff(E) detector target mass
NA Avogadro number
(E) neutrino detection efficiency
NN==∫ ∫ (E(E)) AAeffeff(E(E)) dE dE
Effective Arrea for a Future Effective Arrea for a Future Mediterranean NTMediterranean NT
NT: Aeff(E,)= Veff(E,) (NA) (E) (E)
Neutrino Event RatesNeutrino Event Rates
KM3NeT-neutrinoCC event Rates in km3
NT as a functionof energy.
L=1000 km
a)pp neutrinos
b) beam dump neutrinos
Summary and Summary and OutlookOutlook
• LHC proton beams will produce large flux of high energy neutrinos. • A future VLVnT (KM3NeT) in
Mediterranean Sea can detect large statistics of LHC neutrinos.
• Feasibility study for LHC/KM3NeT neutrino experiment is necesary. .