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

Outline Review main objectives of this workshop • 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 km 3 detectors • Links between the Neutrino Astronomy community and other High-Energy Astronomy communities 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 neutrino masses ν 3 squared -3 2 atmospheric, 3 10 ev ∆ 2 m ν 23 ν 3 µ ν 2 -4 ev ∆ m 12 2 2 solar < 210 ν 1 θ 23 ν τ ν ’ ν 2 ν e θ θ 12 13 ν From A. Blondel 1

� � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � Neutrino masses and mixings • 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( θ 12 , θ 13 , θ 23 , δ CP ) in the presence of at least 2 masses, with at least 2 non zero mixing angles e 1 U ( ) ij , CP 2 3 Oscillation experiments measure ∆ m 2 , not m

SuperK Allowed region (grand global fit) (FC + PC + UP-thru + UP-stop + multi-rings) 79.3 kt . yrs Within physical region; x 2 min = 157.5/170 dof sin 2 2 θ = 1.0, ∆ m 2 = 2.5 × 10 -3 eV 2 With unphysical region; x 2 min = 157.4/170 dof sin 2 2 θ = 1.01, ∆ m 2 = 2.5 × 10 -3 eV 2

What we know today • Maximal ν µ -> ν τ oscillation for ∆ m 2 = 2.5 10 -3 eV 2 ICARUS and OPERA should evidence ν µ -> ν τ (Problem of statistics? Need for intense beams ) • CHOOZ constrains ν e oscillations θ 13 < 10 -1 • Solar neutrinos � Several scenarii possible: 2 « large » – LMA (preferred) : θ 12 « large », ∆ m 12 to be tested soon by KAMLAND – Other scenarii (SMA, LOW, VAC) small mixing angles or small 2 can be tested by BOREXINO, LENS, … ∆ m 12 • 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 ( θ 13 , 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 θ 13 can be measured in superbeams (JHF, USA, CERN-Modane) to 1° or 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 21 st 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 Neutrinos can keep memory of distant objects: no deflection in magnetic fields not absorbed on dust clouds or background radiation New astronomic instruments often give unexpected results: Telescope User date Intended Use Actual use Optical Galileo 1608 Navigation Moons of Jupiter Expanding Optical Hubble 1929 Nebulae Universe Radio Jansky 1932 Noise Radio galaxies Penzias, 3K cosmic Micro-wave 1965 Radio-galaxies, noise Wilson background neutron stars X-ray Giacconi … 1965 Sun, moon accreating binaires Radio Hewish,Bell 1967 Ionosphere Pulsars Thermonuclear Gamma ray � -rays military 1960? (from F.Halzen) explosions bursts With Neutrino Telescopes, hope for completely new discoveries

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

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

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

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 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 Galactic Centre seen 80% of time AMANDA Southern Hemisphere Galactic Centre (Not seen) Need Neutrino Telescopes in both Northern and Southern Hemispheres

Optical properties are better AMANDA South pole in water ANTARES sea water ANTARES AMANDA B λ abs = 100 m λ abs ~ 55-65 m ; λ scat > 100 m Λ eff scatt = 25 m at large angles AMANDA Distance (m) T i m e d e l a y ( n s ) + ( 3 0 n s ) ANTARES Overall spread (PMT_tts + cali+ scattering+ ) s n ( y a l e d e m i T group velocity) = 2.1 ns @ 40 m 100 ns

Expected Performance: Effective Area (ANTARES 10 strings 60 m apart) trigger reconstruction selection 0.1 km 2 Geometrical surface

ANTARES expected performance: Resolutions Energy Resolution Angular Resolution o o 10 TeV • 5 GeV < E < 100 GeV Energy estimated from µ range σ E ~ 3 GeV • E > 1 TeV σ E / E ~ 3 Includes all effects (TTS, positioning, scattering etc.,) except phase → group velocity of light

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 10 15 eV) cf also • AUGER, EUSO (above 10 18 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 MONOCULAR Télescope on ISS/Colombus Watching the Atmosphere ! ∅ = 2.5m alt.: 380-410 km FOV : +-30° GEOMETRICAL FACTORs 2. 10 5 km 2 sr 10 12 tons of air Detect Extensive Air Showers ENERGY THRESHOLD ≥ 3 10 19 eV Fluorescence N2 + Cerenkov 300-400nm

Comparison of UHECR Experiments Auger EUSO 10 6 Status Under PhaseA 2 sr) construction 10 5 10 19 -10 21 > 4x10 19 Energy E U S O (eV) 1.3° 10 4 � resolution 0.3° ( ������ a u g e r @10 20 eV m ������ ( ������ (k h i-re s R Energy 25% 20% 10 3 O T resolution C A a g a s a 10 6 Aperture 7000 F L 10 2 (km² .str) A IC fly 's e y e Duty cycle 100% 10% R h a v e ra h p a rk T E Effective 7000 100 000 M 1 10 Running O Aperture v o lc a n o ra n c h E G Events/year 70 >500 Completed 10 0 E>10 20 eV none few GZK � 1950 1960 1970 1980 1990 2000 2010 2020 few TD � 150TD � Y E A R

Neutrino Telescopes Scientific Programme χ χ χ χ χ χ χ χ χχ χ χ χ χ χ χ χ χ χ χ χ χ χ Low energy Medium Energy High energy • Observation of neutrinos from • Search for neutralinos • Neutrino oscillations (extra-) galactic sources such via their self- via the modification in annihilation to as GRB, AGN, Supernovae the energy spectrum products containing remnants, molecular clouds, due to observation of neutrinos at the centre etc., the first oscillation of the Earth, Sun and • Microquasars (5 years ago??) minimum Galaxy

Gamma Ray Bursts ~1-2 / day, duration 10ms - 100s, isotropic distribution in sky, likely at extra galactic distances, Count rate in unit of 1000 counts s -1 energies ~10 51 ergs sec Coincidence in time ~10sec and in position ~1 o ν signal could be very clear with little background

Gamma Ray Burst in different Wavelengths Gamma Ray Burst in different Wavelengths Gamma Rays T B + 6,5 h T B + 12 h T B + 52 h Visible Light