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E xtreme U niverse S pace O bservatory

E xtreme U niverse S pace O bservatory. DETECTING NEUTRINOS WITH EUSO. Sergio Bottai INFN Firenze on behalf of the EUSO Collaboration. Paris neutrino2004. EUSO Consortium - Institutes. The EUSO instrument consortium is truly global in nature with >150 researchers

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E xtreme U niverse S pace O bservatory

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  1. Extreme Universe Space Observatory DETECTING NEUTRINOS WITH EUSO Sergio Bottai INFN Firenze on behalf of the EUSO Collaboration Paris neutrino2004

  2. EUSO Consortium - Institutes The EUSO instrument consortium is truly global in nature with >150 researchers in 50 institutions in 6 countries in Europe, the USA, Japan and Brazil. Participant Nations and Institutions Brazil France Italy Germany Portugal Spain Switzerland USA Japan • IAG, Univ Sao Paulo • APC, Paris • CdF, Paris • IAP, Paris • LPSC, Grenoble • LPTHE, Paris • OdP, Paris • MPIfP, Munich • MPIHLL, Munich • MPIfRA, Bonn • Univ. Wuerzburg • LIP, Lisbon • Obs. Neuchatel • IAA-CSIC, Granada • Dpt.FTC & CAFPE, Univ. Granada • MSFC & NSSTC, Huntsville • UAH, Huntsville • UCB, Berkeley • UCLA, Los Angeles • Vanderbilt Univ. • IASF, Palermo • ISAC-CNR, Bologna • INFN & Univ. Genova • INFN & Univ. Firenze • INFN & Univ. Torino • INFN & Univ. Trieste • INFN Catania & Univ. Palermo • Univ. Roma “La Sapienza” • Scuola Normale Sup. Pisa • Oss. Astrofisico Arcetri • Oss. Astrofisico Catania • CARSO • INOA • RIKEN • ICRR • Konan Univ. • ISAS • Rikkyo • KEK • NAO • Tokyo Univ. • Saytama • Aoyama • Kinki • Seikei • Kanazawa #2

  3. BASIC GUIDELINE • EUSO is an experiment devoted to measure the cosmic ray spectrum above 1020eV with high statistic • EUSO is at present in a phase of ‘feasibility study’ • EUSO has also some potentiality to detect extraterrestrial neutrinos of energy close to 1020eV. The sensitivity for such neutrino discover will be discussed in the presentation

  4. GZK mechanism Ｎ P Δ π γ3K UHECR Observational Situation as today E>1020eV particles hit the atmosphere at a rate of <1/(100km2•year). A great experimental challenge. AGASA - HIRES WE NEED NEW EXPERIMENTS : CONTROLL SYSTEMATICS -> AUGER INCREASE STATISTICS -> AUGER-EUSO #4

  5. Exposure (AGASA unit) EUSO

  6. Photons per m isotropic 330 – 400 nm Euso Area vs Auger Pierre-Auger EUSO EHECR FROM SPACE

  7. Advantage of a space-based fluorescence detector for EECR • Geometrical Factor (A · )  6 · 105 km2 sr (FoV=±30° at ISS mean distance hISS430km) • rather constant signal attenuation ~0.5 • Negligible Proximity Effect • (Dist./Dist. < 1%) • (acceptance not depending on energy) • Full Sky Coverage • Cerenkov “footprint” of shower ATMOSPHERE #7

  8. The instrument ELECTRONICS : PHOTON COUNTING TIME INFORMATION LENSES FOCAL SURFACE LIGHT SENSORS #8

  9. EUSO -The Optical System Optics Requirements • FoV  30° • Pupil entrance pupil  2 m • F/#  1.15 • Spot dimension ~ 0.1° • Spectral range 300-400 nm • Limited mass !! VERY challenging 2 Double sided Fresnel lens ! Pupil diameter 2.3m #9

  10. EUSO – TheFocal Surface 200.000 pixels at single PE Macrocell Microcell Support Structure MAPMT R8900 – M36 R8900 – M36 Filters Focal Surface assembly FILLING>0.9 #10

  11. The Atmosphering sounding G. D’Alì Staiti, Bologna, May 24, 2004 LIDAR LIDAR + IR camera • Cloud topology survey • Atmospheric transmission calibration #11 #11

  12. SIMULATION : The Detector Light Sensitivity The detected signal FOR 1020eV Signal ~10 Random Noise 0.5-0.8 The trigger efficiency for a subsample 20% The trigger efficiency Threshold reach ~5*1019eV #12

  13. clear no trigger The Real Atmosphere MCM’02 #13

  14. Golden Cerenkov only Fmax only The EUSO Acceptance In clear sky… …and in real atmosphere REALISTIC CLOUDS SCENARIO KILL ~40% OF SHOWERS The EUSO statistics E>1020eV ~1000 events/year in SuperGZK mode >70 events/year in GZK-suppressed mode #14

  15. EUSO resolution Angular res = 1o – 4o Energy res = 20% (RMS)+.. (with Lidar info) Xmax res = 50 g/cm2 (with Lidar info) #15

  16. NEUTRINO EVENTS IN ATMOSPHERE SHOWERS (ne,n t,nm) • km3we of target for EUSO • But : duty cycle, efficiency, very high energy threshold

  17. Proton – neutrino discrimination The probability of neutrino interaction in atmosphere is proportional to the atmospheric density. NEUTRINOS CC INTERACTIONS (LPM effect included) P+ n

  18. DOWNWARD NEUTRINO ACCEPTANCE FOR EUSO Fluorescence only events Golden events Xmax Select. Shape Select. P+ n Neutrino domain 1600g/cm2 n P+ Rejection > 10-4

  19. P+ TOP ATMOSPHERE The probability of a neutrino interaction in a volume element dV is proportional to density NEUTRINO NEUTRINO Showers Groundlevel

  20. EFFECTIVE ACCEPTANCE (g*sr) FOR NEUTRINOS Clear sky (duty cycle not contained) With clouds + Shower max visible Trigger + Selection CC CC ~300 km3we NC NC duty cycle ~50 km3we

  21. Classes of UHE n Models p blazar jet log(E2 Flux) pp core AGN GZK neutrinos Top-Down models EUSO GRB (W&B) 3 6 9 log(E/GeV) TeV PeV EeV

  22. Neutrino sensitivity Auger EUSO Sensitivity 1 events/decade/year EUSO has 10 times larger Aperture than Auger above GZK energy WB EUSO is sensitive Z-Burst, Top Down Models and High (MAXIMUM) GZK flux. ~ 10 events/year detected

  23. UPWARD TAU SHOWERS S. Bottai , S. Giurgola ICRC 2001 S. Bottai,S.Giurgola Astr. Phys. 18 2003 EUSO threshold EUSO X 20

  24. Just wishful thinking? 2003 2004 2005 2006 2007 2008 2009 2010 2011 2012 2013 EUSO A B C/D LAUNCH 2010 ESA-EUSO STARTED A PHASE A STUDY FOR ISS PHASE A UFFICIALLY CLOSE IN JULY 2004 on June 2004 ESA ‘SCIENCE DIRECTORATE’ DID NOT INCLUDED EUSO IN THE PRIORITY LIST OF CANDIDATE EXPERIMENT UP 2012 . (“wait AUGER results”) The possibility to mantain the time schedule is under investigation #24

  25. Conclusion • EUSO is a pioneering experiment for studying EAS from space: • An instantaneous aperture of 6×105km2sr with a duty cycle ~20% is a technically achievable goal with up-to-date technology; • The acceptance reduction due to cloud effect has been evaluated to be ~0.5. 50.000km2sr effective acceptance • ~103 events/year can be expected according to AGASA findings; • ~102 events/year can be expected according to GZK-suppressed spectrum due to uniform source distribution. • for n with E>5*1019eV EUSO will have a competitive sensitivity (50 km3 we effective) TOP DOWN MODELS CAN BE SEEN IF THEY EXISTS • TIME SCHEDULE 2010 ??????? #25

  26. A proposed large mirror system Design of a mirror optics, based on the Schmidt camera principle, with FOV up to 25° light shield mirror correcting plate and/or filter FEATURES 3 identical DETECTORS ASSEMBLED INSIDETHE ISS ? Solid state detectors ? 5-7 m focal plane

  27. S. Bottai, P. Spillantini, “ FROM THE EXTREME UNIVERSE SPACE OBSERVATORY (EUSO) TO THE EXTREME ENERGY NEUTRINO OBSERVATORY “ prooceedings of the XIth Lomonosov Conferenceq AUGER EUSO WB q.e=50% Eth=3EeV D=7.5m FOV= EUSO X 3 GZK(A)~ 40 events/year GZK(A)~0.3 events/year in EUSO

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