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8th Topical Seminar on Innovative Particle and Radiation Detectors Siena, 21 – 24 October 2002

8th Topical Seminar on Innovative Particle and Radiation Detectors Siena, 21 – 24 October 2002. SIENA is located in Tuscany about 50km south of Florence. Ancient Etruscan settlement, became Roman colony under the name of Sena Julia.

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8th Topical Seminar on Innovative Particle and Radiation Detectors Siena, 21 – 24 October 2002

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  1. 8th Topical Seminar on Innovative Particle and Radiation DetectorsSiena, 21 – 24 October 2002

  2. SIENA is located in Tuscany about 50km south of Florence Ancient Etruscan settlement, became Roman colony under the name of Sena Julia Its importance grew in Middle Ages until became a municipality in 12th century: flourished in XIV century Frequent confrontations with neighbouring towns: taken over by Florence in 16th century Still retains an authentic medieval atmosphere

  3. Piazza del Campo 14th century, is the heart of the city Location of the ancient roman forum, boasts 14th century gothic buildings Palazzo pubblico e Torre del mangia Fonte Gaia by Jacopo della Quercia The horse race (Palio) is held here, 2nd of July and 16th of August Of medieval origin, sees the 10 of the 17 contrade competing against each other: the winner gets the Palio (banner)

  4. The Dome,XIV century: one of the best roman-gothic architectural examples Masterpieces by Nicola Pisano, Donatello,Pinturicchio Floor consisting of 56 different mosaics, depicting sacred scenes, required more than 150 years to be completed

  5. High Energy Neutrino Astronomy Christian Spiering, Siena, October 2002

  6. Physics Goals A. High Energy Neutrino Astrophysics Weakly interacting neutrinos reach us from very distant sources: possible invaluable instrument for high-energy astrophysics B. Particle Physics Magnetic Monopoles, Oscillations, Neutrino Mass ... C. Others Supernova Bursts, CR composition, Black Holes, ...

  7. GZK cut-off 1 TeV Cosmic Rays

  8. Supernova shocks expanding in interstellar medium up to 1-10 PeV Crab nebula

  9. Active Galaxies: accretion disk and jets up to 1020 eV VLA image of Cygnus A

  10. Air showers Underground Radio,Acoustic Underwater pp core AGN p blazar jet log(E2 Flux) Top-down WIMPs Oscillations GZK GRB (W&B) Microquasars etc. 3 6 9 log(E/GeV) TeV PeV EeV

  11. 1 pp core AGN (Nellen) 2 p core AGN Stecker & Salomon) 3 p „maximum model“ (Mannheim et al.) 4 p blazar jets (Mannh) 5 p AGN (Rachen & Biermann) 6 pp AGN (Mannheim) 7 GRB (Waxman & Bahcall) 8 TD (Sigl) 9 GZK Macro Baikal Amanda Mannheim & Learned, 2000 Diffuse Fluxes: Predictions and Bounds 9

  12. Detection Methodsand Projects Underwater/Ice Cerenkov Telescopes Acoustic Detection Radio Detection Detection by Air Showers

  13. 4-string stage (1996) Underwater/Ice Cerenkov Telescopes Strings of widely spaced PMT put in deep water AMANDA: Antarctic Muon And Neutrino Detector Array

  14. Cerenkov radiation in H2O : v0.75c,  = tg-1[(n2 v2/c2-1)1/2] High-energy neutrinos through the earth may interact and create muons which emit Cherenkov light cascade muon

  15. 1 km 2 km SPASE air shower arrays  resolution Amanda-B10 ~ 3.5° results in ~ 3° for upward moving muons (Amanda-II: < 2°)

  16. AMANDA Super-K DUMAND 80PMTs 302PMTs Amanda-II: 677 PMTs at 19 strings (1996-2000) AMANDA-II

  17. Point Sources Amanda II (2000) 1328 events Preliminary limits (in units of 10-15 muons cm-2 s-1): Cas A:0.6 Mk421:1.4 Mk501:0.8 Crab: 6.8 SS433:10.5

  18. SS-433 -45 0 45 90 -90 Mk-421 / ~ 1 Expected sensitivity AMANDA 97-02 data southern sky northern sky m cm-2 s-1 4 years Super-Kamiokande 10-14 170 days AMANDA-B10 8 years MACRO 10-15 declination (degrees)

  19. IceTop AMANDA South Pole 1400 m 2400 m IceCube - 80 Strings - 4800 PMT • Instrumented volume: 1 km3 • Installation: 2004-2010 ~ 80.000 atm. per year

  20. mediterraneum Mediterranean Projects 2400m ANTARES 4100m 3400m NEMO NESTOR

  21. Site: Pylos (Greece), 3800m depth towers of 12 titanium floors each supporting 12 PMTs

  22. 40 km Submarine cable -2400m

  23. Shore station Optical module 10 strings 12 m between storeys hydrophone Compass, tilt meter 2500m float ~60m Electro-optic submarine cable ~40km 300m active Electronics containers Readout cables ~100m Junction box anchor Acoustic beacon ANTARES Design

  24. NEMO Neutrino Mediterranean Observatory • abs. length ~70 m • 80km from coast 3400 m deep

  25. NESTOR 1991 - 2000 R & D, Site Evaluation Summer 2002 Deployment 2 floors Winter 2003 Recovery & re-deployment with 4 floors Autumn 2003 Full Tower deployment 2004 Add 3 DUMAND strings around tower 2005 - ? Deployment of 7 NESTOR towers ANTARES 1996 - 2000 R&D, Site Evaluation 2000 Demonstrator line 2001 Start Construction September 2002 Deploy prototype line December 2004 10 (12?) line detector complete 2005 - ? Construction of km3 Detector NEMO 1999 - 2001 Site selection and R&D 2002 - 2004 Prototyping at Catania Test Site 2005 - ? Construction of km3 Detector

  26. ACOUSTIC DETECTION • Suitable for UHE Threshold > 10 PeV • Particle shower  ionization  heat  perpendicular pressure wave d 50s P t R Maximum of emission at ~ 20 kHz Attenuation of sea water → given a large initial signal, huge detection volumes can be achieved.

  27. AUTEC array in Atlanticexisting sonar array for submarine detection Atlantic Undersea Test and Evaluation Center 52 sensors on 2.5 km lattice (250 km2) 4.5 m above surface 1-50 kHz ! Threshold ~ 100 EeV

  28. RADIO DETECTION: Askaryan process Interaction in ice:e + n  p + e- e-  ... cascade Compton scattered electrons  shower develops negative net charge Qnet ~ 0.25 Ecascade (GeV). • Coherent Cherenkov signal for  >> 10 cm (radio)  relativist. pancake ~ 1cm thick,  ~10cm  each particle emits Cherenkov radiation  C signal is resultant of overlapping Cherenkov cones  C-signal ~ E2 nsec Threshold > 10 PeV

  29. Showers in RF-transparent media (ice, rock salt)RICE Radio Ice Cherenkov Experiment South Pole firn layer (to 120 m depth) 20 receivers + transmitters UHE NEUTRINO     DIRECTION E 2 · dN/dE < 10-4 GeV · cm-2 · s-1 · sr-1 at 100 PeV 300 METER DEPTH

  30. AntarcticImpulsiveTransientArray Flight in 2006

  31. el.-magn. cascade from e hard muons from CR Far inclined showers ( thousand per year) • Flat and thin shower front • Narrow signals • Time alignment Atmosphere Hard  s Deep inclined showers (~ one peryear?) • Curved and thick shower front • Broad signals Soft  s + e.m. Atmosphere Extensive Air Showers for E > 10 EeV produce Ionization trails

  32. Observation of upward going optical Cherenkov radiation emitted by tau neutrino -induced air-showers Need an observation from above (satellite)

  33. E > 1019 eV 500 km 60 ° Mass up to 10 Tera-tons Area up to 106 km2 Horizontal Air Showers seen by Satellite Horizontal air shower initiated deep in atmosphere 1 - 20 GZK ev./y

  34. Extreme Universe Space Observatory OWL Orbiting Wide-angle Light-collectors

  35. RICE AGASA Amanda, Baikal 2002 Anita 2004 AUGER nt AABN 2007 EUSO 2012 Auger Salsa km3 GLUE

  36. Conclusions Most promising: point sources 0.1 km3 and 1 km3 detectors underwater and ice Huge step in GZK region Exciting decade ahead Contacts: Christian Spiering csspier@ifh.de

  37. Solar Neutrino Spectrometer with InP Detectors P.G. Pelfer University of Florence and INFN, Firenze, Italy F. Dubecky Institute of Electrical Engineering, Slovak Academy of Sciences Bratislava, Slovakia A.Owens ESA/ESTEC Noordwijk,Netherland

  38. Why InP Solar Neutrino Experiment ? Semi Insulating InP Material base material for: Hard X-Ray Detectors Fast Electronics and Optoelectronics InP Spectrometer, the Smallest, Real Time, Lower Energy pp Solar Neutrino Spectrometer The Solar Neutrino Spectrometer from/for R&D on InP X-Ray Detectors ?

  39. DETECTOR APPLICATIONS • BASIC KNOWLEDGE • Solar Neutrino Physics • X-ray astronomy • X-ray physics • MEDICINE • Digital X-ray radiology (stomatology, mammography, ...) • Positron emission tomography • Dosimetry • NONDESTRUCTIVE ON-LINE PROCESS CONTROL • Material defectoscopy • MONITORING • Environmental control • Radioactive waste management • Metrology (testing of radioactive sources, spectrometry...) • NATIONAL SECURITY • Contraband inspections: cargo control • Detection of drugs and plastic explosives • Cultural heritage study

  40. Requirements for Hard X-Ray Detectors of the NewGeneration>10keV RT OPERATION: EG > 1.2 eV POLARISATION EFFECT: EG < 2.5 eV HIGH ENERGY RESOLUTION: EG small HIGH STOPPING POWER:Z > 30 HIGH CARRIER MOBILITY: > 2000 cm2/Vs CANDIDATES CdTe, HgI2, GaAs, InP • Room temperature (RT) operation • Portability • Fast reaction rate • Universal detection ability • Good detection parameters: CCE, FWHM, DE • Radiation hardness • Well established material technology • Well established device technology (10 m) • FE Electronics and Optoelectronics integration on the Detector • LOW COST

  41. Attenuation and mobility

  42. Neutrino from the Sun Water Kamioka, SuperK x + e-  x + e- (ES) Gallium SAGE, Gallex, GNO e + 71Ga  71Ge + e- Chlorine Homestake e + 37Cl  37Ar + e- D2O SNO x + e-  x + e- (ES) e + d  p + p + e- (CC) x + d  n + p + e- (NC)

  43. Requirements for Indium Solar Neutrino Spectrometer 1. Indium incorporated into the detector 2. Energy resolution ∆E/E of the order of 25% at 600 keV. Important for spectrometry as well as background reduction. 3. Time resolution of the order of 100 ns for ~ 100 keV radiations. 4. Position resolution ∆V/V  10-7 at a reasonable cost. Very important for background reduction 5. Good energy resolution for low energy radiations ( ~ 50 keV ) 6. Made with materials of high radiactive purity

  44. Neutrino Detection by In Target 1/2= 4.76  sec 7/2+ 612.81 keV e 9/2+ 1 3/2+ 497.33 keV 115In (95.7%) - 2 1/2=6x1014 y 1/2+ 0 115Sn E    e(E - 118 keV ) + 115 Sn*   Delay  = 4.76  sec   115Sn*  115Sn + e-(88  112 keV)/1(115.6 keV) +  2(497.33 keV)

  45. “ delayed event “ in a 27 cm3macrocell Solar Neutrino Event inInP Detector " prompt event “ in a “1 cm3 cell” 3 4 5 2 2 1 6 1 3 4 5 9 8 7 time 2 1 6 e 9 8 7 10 s 1 cm3 cell Detector made up of many ‘basic cells’ 106 InP “1 cm3 cell” Calorimeter Module

  46. FULL NEUTRINO SPECTROMETER Spectrometer Building Block Nmodules  125 Spectrometer Module 100 mm 200 mm Pad Detectors Vmicrocell 1 mm3 Nmicrocell /cm3 1000 1 neutrino event once a day for 1011 background events

  47. Present InP Material and Detector Technology SemiInsulating InP Wafer 6” diameter, 1 mm thick Basic Component of Neutrino Spectrometer Pad Detectors

  48. SI InP Material and Detector Technology Producer: JAPAN ENERGY Co., Japan Growth Technique: LEC High-Temperature Wafer Annealing Resistivity (300 K):4.9x107 cm Hall Mobility (300K):4410 cm2/Vs Fe Content:2x1015 cm-3 Orientation:<100> Final Wafer Thickness:~200 m Original BUFFERS realisedusing ion implantation in backside (PATENTED) Symmetrical circular contact configuration, 2mm  , using both-sided photolithography Final metallisation: TiPtAu on top and AuGeNi on backside Surface passivation by Silicon Nitride

  49. InP Detector Test Setup 3.142 mm2 x 200 m

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