Neutrino Telescopes and Neutrinos from LHC Neutrino Telescopes and Neutrinos from LHC ISPM – 2005 Physics at the future colliders 17-21/10/2005, Tbilisi,

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:


fireball (eg GRB)


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:


fireball (eg GRB)


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


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 !


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

PDF

W(Z)

cosc= 1/n



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


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)


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



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


High Energy Neutrino TelescopesHigh Energy Neutrino Telescopes

AMANDA/IceCube

Baikal

NESTOR

ANTARESANTARES

NEMONEMO


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.


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


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)


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


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


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. .

Documents

Neutrino Telescopes and Neutrinos from LHC Neutrino Telescopes and Neutrinos from LHC ISPM – 2005 Physics at the future colliders 17-21/10/2005, Tbilisi,