Outline Review main objectives of this workshop Physics topics - - PowerPoint PPT Presentation

Outline

• Physics topics

– Neutrino physics : neutrino oscillations and masses – Neutrino astronomy and astrophysics: detection of new astrophysical bodies and neutrino producing processes – Neutrino particle astrophysics: Neutralino Dark Matter and Topological Defects, superstrings and extra dimensions

• Neutrino telescopes : Present and future km3 detectors
• Links between the Neutrino Astronomy community and
• ther High-Energy Astronomy communities

Review main objectives of this workshop Main IN2P3 Involvement

Main issues in neutrino physics today

• Neutrinos : an important role in establishing the SM of

particle physics (parity violation, neutral currents, scaling violations, number of active neutrino families).

• Solar and atmospheric neutrino experiments

pattern of neutrino masses and mixings to explain !

• Higgs still missing but even its discovery would not

explain pattern

• CKM matrix (quark sector) difficult to use theoretically

(large uncomputable uncertainties of strong interactions).

The neutrino mixing matrix

µ

νe ν θ

12

θ

13 ’

θ

23

ν ν

2

ν

1

ν

3

ντ

ν ν2 ν1

3 neutrino

∆

23

m

squared

∆m12

2 2

atmospheric, 3 10

• 3

solar < 210

• 4 ev

2

ev

2 masses

From A. Blondel

• Mass of neutrino = probe of physics at GUT scale

(as proton lifetime)

• Atmospheric and solar neutrino experiments define

gross features of « standard 3 ν » leptonic mixing matrix U U= U(θ12, θ13,θ23, δCP) in the presence of at least 2 masses, with at least 2 non zero mixing angles Oscillation experiments measure ∆m2, not m

Neutrino masses and mixings

• 3

2 1 ,

) (

• CP

ij e

U

SuperK Allowed region (grand global fit) (FC + PC + UP-thru + UP-stop + multi-rings)

79.3 kt . yrs

Within physical region; x2min = 157.5/170 dof

sin22θ = 1.0, ∆m2 = 2.5×10-3 eV2

With unphysical region; x2min = 157.4/170 dof

sin22θ = 1.01, ∆m2 = 2.5×10-3 eV2

What we know today

• Maximal νµ ->ντ oscillation for ∆m2 = 2.5 10-3 eV2

ICARUS and OPERA should evidence νµ ->ντ (Problem of statistics? Need for intense beams )

• CHOOZ constrains νe oscillations θ13 < 10-1
• Solar neutrinos Several scenarii possible:

– LMA (preferred) : θ12 « large », ∆m12

2 « large »

to be tested soon by KAMLAND – Other scenarii (SMA, LOW, VAC) small mixing angles or small ∆m12

2 can be tested by BOREXINO, LENS, …

• LSND results to be confirmed or excluded: miniBOONE?

4th sterile neutrino ? Might need introduction of extra dimensions. EXCITING!

What next?

• If LMA solution OK: mixing matrix parameters

(θ13, mass hierarchy, CP phase) Prospect of measuring CP violation in the leptonic sector Neutrino Factory is the clear next step

• NOT LMA : Solar neutrino experiments crucial

– Still θ13 can be measured in superbeams (JHF, USA, CERN-Modane) to 1°

• r neutrino factory to 0.1°

– Other parameters ???

HE Neutrino Astronomy

• Novel messenger astronomy : window on new

discovery?

• Multi messenger astronomy : a necessary

complementarity to learn about physics mechanisms inside celestial bodies? ‘The astronomy event of the 21st century could be the simultaneous observation of TeV gamma rays, neutrinos and gravitational waves from cataclysmic events associated with the source of the cosmic rays’ F. Halzen

New Window on Universe

New astronomic instruments often give unexpected results: With Neutrino Telescopes, hope for completely new discoveries Neutrinos can keep memory of distant objects: no deflection in magnetic fields not absorbed on dust clouds or background radiation

(from F.Halzen)

Telescope User date Intended Use Actual use

Optical Galileo 1608 Navigation Moons of Jupiter Optical Hubble 1929 Nebulae Expanding Universe Radio Jansky 1932 Noise Radio galaxies Micro-wave Penzias, Wilson 1965 Radio-galaxies, noise 3K cosmic background X-ray Giacconi … 1965 Sun, moon neutron stars accreating binaires Radio Hewish,Bell 1967 Ionosphere Pulsars

• rays

military 1960? Thermonuclear explosions Gamma ray bursts

High Energy Neutrino Telescopes (cf previous talk of T. Capone)

• Km scale detector necessary to see neutrino signals in a

variety of topics: Highest Energy cosmic rays, GRB, DM, microquasars,…

• Problem to solve: reliable, expandable, affordable

technology.

• Experience now from Dumand, Baikal, Antares, Nemo,

Nestor in water, and AMANDA in ice.

• ICECUBE is under construction in South Pole.
• Only one Km3 detector in Mediterranean sea

AMANDA/ICECUBE

South Pole: glacial ice

1993 First strings AMANDA A 1998 AMANDA B10 ~ 300 Optical Modules 2000 AMANDAII ~ 700 Optical Modules → ICECUBE: 8000 Optical Modules The more advanced project

ANTARES Phase II : 0.1 km² Detector

10 strings : 900 PMTs in total Detector to be deployed at ANTARES site by 2003 - 2004

Deployed 2001

Lake Baikal, Siberia: surface frozen in winter 1993 36 Optical Modules 1998 192 Optical Modules

BAIKAL

The NESTOR Project

Site near Pylos (Greece) at 3800 m depth.

• Hexagonal tower deployment
• 168 photomultipliers
• 12 floors
• 32 m diameter

NEMO

• Site: Capo Passero,

Sicily (> 3300 m)

• Sea water optical

properties studies performed

• Participation in

ANTARES

• R&D towards KM3

View of Sky: Complementary with AMANDA

Need Neutrino Telescopes in both Northern and Southern Hemispheres Fraction of time sky visible

0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0

ANTARES Northern Hemisphere AMANDA Southern Hemisphere

Galactic Centre seen 80% of time Galactic Centre (Not seen)

Optical properties are better in water

ANTARES λabs ~ 55-65 m ; λscat > 100 m at large angles

ANTARES sea water AMANDA South pole

AMANDA B λabs = 100 m Λeff scatt= 25 m

AMANDA T i m e d e l a y ( n s )

Distance (m)

T i m e d e l a y ( n s ) + ( 3 n s ) 100 ns

Overall spread (PMT_tts + cali+ scattering+ group velocity) = 2.1 ns @ 40 m ANTARES

Expected Performance: Effective Area

(ANTARES 10 strings 60 m apart)

trigger reconstruction selection Geometrical surface

0.1 km2

Angular Resolution Energy Resolution

• 5 GeV < E < 100 GeV

Energy estimated from µ range σE ~ 3 GeV

• E > 1 TeV

σE / E ~ 3 Includes all effects (TTS, positioning, scattering etc.,) except phase→group velocity of light

ANTARES expected performance: Resolutions

• 10 TeV

R&D for KM3 (cf T. Capone’s talk)

• Higher efficiency PMTs / HPDs?
• Radio and acoustic detection studies for UHE neutrinos
• Towards a mixed concept of detector?

For UHE neutrinos (above 1015 eV) cf also

• AUGER, EUSO (above 1018 eV)
• New ideas (eg, Eusino, cf F. Vannucci’s talk)

UHE neutrinos Other detectors

GZK cut

Pierre AUGER observatory cf talk of A. Letessier Selvon

Atmosphere = beam dump Observation of Horizontal Air Showers most probably due to neutrinos

EUSO : THE APPROACH

Detect Extensive Air Showers ENERGY THRESHOLD ≥ 3 1019 eV Fluorescence N2 + Cerenkov 300-400nm GEOMETRICAL FACTORs

• 2. 105 km2 sr

1012 tons of air MONOCULAR Télescope on ISS/Colombus Watching the Atmosphere ! ∅ = 2.5m alt.: 380-410 km FOV : +-30°

Y E A R 1950 1960 1970 1980 1990 2000 2010 2020 G E O M E T R IC A L F A C T O R (k m

2 sr)

10 10

1

10

2

10

3

10

4

10

5

10

6

v

• lc

a n

• ra

n c h h a v e ra h p a rk fly 's e y e a g a s a h i-re s a u g e r

E U S O

Comparison of UHECR Experiments

Auger EUSO Status Under construction PhaseA Energy (eV) 1019-1021 > 4x1019 resolution @1020eV 1.3° 0.3° ( ( Energy resolution 25% 20% Aperture (km² .str) 7000 106 Duty cycle 100% 10% Effective Aperture 7000 100 000 Events/year E>1020eV 70 none few TD >500 few GZK 150TD

Completed Running

Neutrino Telescopes Scientific Programme

• Search for neutralinos

via their self- annihilation to products containing neutrinos at the centre

• f the Earth, Sun and

Galaxy

• Neutrino oscillations

via the modification in the energy spectrum due to observation of the first oscillation minimum

Low energy Medium Energy High energy

• Observation of neutrinos from

(extra-) galactic sources such as GRB, AGN, Supernovae remnants, molecular clouds, etc.,

• Microquasars (5 years ago??)

χ χ χ χ χ χ χ χ χ χ χ χ χ χ χ χ χχ χ χ χ χ χ

Gamma Ray Bursts

~1-2 / day, duration 10ms - 100s, isotropic distribution in sky, likely at extra galactic distances, energies ~1051 ergs Coincidence in time ~10sec and in position ~1o ν signal could be very clear with little background

Count rate in unit of 1000 counts s-1

sec

Gamma Ray Burst in different Wavelengths Gamma Ray Burst in different Wavelengths

TB+ 6,5 h TB + 12 h TB + 52 h

Gamma Rays Visible Light

View of the Sky (microquasars)

AMANDA (South Pole) ANTARES (43° North) Gamma ray flux >100 MeV observed by EGRET

Source type number of sources seen by Antares EGRET AGN 94 86% EGRET Pulsars 5 100% Known Microquasars 19 74%

Indicative, assumes efficiency=100% for 2π downwards

GX339-4

2500m 2500m

300m 300m 50m 50m

Electro-optical Electro-optical underwater cable underwater cable ~40km ~40km Junction box Junction box Readout Cables Readout Cables

Shore station Shore station anchor anchor float float

Electronics Containers Electronics Containers

~60m ~60m

• dules

acoustic detector acoustic detector

Light Sources

Indirect dark matter searches

ν, γ, p, e+

χ

Indirect Detections Distribution of Dark Matter in the Galaxy Accumulation + Annihilation of Dark Matter

Astroparticle detectors : positrons, antiprotons, gammas, neutrinos

Indirect detection of neutrinos from Dark Matter neutralino annihilations

• Possible Indirect Neutrino Detection from Sun and

Galactic Center (Northern Hemisphere Detector)

• Expectation of sensitivity : complementary and

sometimes better than for Direct Detection experiments.

• Complementarity with gamma detectors

Next generation of ACT

VERITAS

50 GeV to 50 TeV 104 m2@100 GeV 105m2 @ 1 TeV

MAGIC HEGRA 30 to 300 GeV

GLAST

Another particle detector in space

• Track detector About 1m2
• Calorimeter
• DAQ
• Anticoincidence detector

ApPEC Astroparticle Physics European Coordination

• Initiative for the promotion of astroparticle physics in

Europe

• Agreement between funding agencies of 5 different

European countries ( May 2, 2001):France, Germany, Italy, Netherlands, UK. Spain to join soon, and …

• Steering Committee : 1 representative of each funding

agency + 1 scientist per country

• Peer Review Committee: Scientists from different areas of

astroparticles

ApPEC goals

• Coordination of the promotion of scientific activities in astroparticle physics
• Reinforcement of cooperation and collaboration of astroparticle physicists
• Development of common long term strategies for European astroparticle

physics

• Recommendations to national funding agencies, EU-commission, European

Science Foundation

• Improvement of collaborations with scientific programmes at CERN, ESA,

ESO.

• Representation of astroparticle physics in international forums as OECD,

UNESCO, …

ApPEC Steering Committee

• H.F. Wagner (BMBF-Bonn, Germany)
• H.Völk (MPI Heidelberg, Germany)
• J. Eschke (GSI-KKS, BMPF, Darmstadt, Germany)
• E. Iarocci (INFN, Italy)
• R. Petronzio (INFN, Italy)
• J. Engelen (NIKHEF, Netherlands)
• H. Chang (FOM, Netherlands)
• I. F. Corbett (PPARC, UK)
• D. Wark (RAL, UK)
• M. Spiro (DSM-DAPNIA, France)
• J.J. Aubert (CNRS-IN2P3, France) Chairman

Peer Review committee

• Ricardo Barbieri (INFN Pisa – Chairman)
• Karsten Danzmann (MPI – Hanovre)
• Michel Davier (LAL- Orsay)
• Luigi Di Lella (CERN – Genève)
• Maarten De Jong (NIKHEF- Netherland)
• Enrique Fernandez (University Autonoma of Barcelona)
• Ettore Fiorini (INFN Milan)
• Gérard Smadja (IPN Lyon)
• Joe Silk (Nuclear & Astrophysics Laboratory University of Oxford)
• Nigel Smith (Rutherford Appleton Laboratory – Didcot Oxon, UK)
• Christian Spiering (DESY Zeuthen)
• Franz von Feilitzsch (Technical University Munchen)
• Alan Watson (PPARC, Leeds, UK)

ApPEC planned reviews

• Double beta decays ( Meeting Jan. 22, 2002, in Paris)
• Dark Matter
• Solar neutrinos
• Neutrino astronomy (AMANDA, ANTARES, ICECUBE,

WATERCUBE)

• Gravitational waves (VIRGO, GEO600, LIGO)
• Cosmic Rays (AUGER)
• Gamma rays astronomy (HESS, MAGIC, GLAST…)
• Space projects