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The quest for UHECR and ν from space

The quest for UHECR and ν from space. Andrea Santangelo IAAT, Eberhard Karls Universit ä t & IASF-CNR Sez. Palermo. Outline. UHECR and ν in a nutshell (see Monday Afternoon for details) Why from space ? How from space ? The actual idea and proposals  EUSO

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The quest for UHECR and ν from space

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  1. The quest for UHECR and νfrom space Andrea Santangelo IAAT, Eberhard Karls Universität & IASF-CNR Sez. Palermo XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  2. Outline • UHECR and ν in a nutshell (see Monday Afternoon for details) • Why from space ? • How from space ? • The actual idea and proposals  EUSO • The Future: toward a “Cosmic Vision 2015-2025” Mission for Particle Astronomy (?) XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  3. Their origin, nature and even their route to the Earth presents an extraordinary puzzle UHECR E> 5×1019 eV (~1016 keV) XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  4. One Piece of the Puzzle, the GZK feature the GZK effect Greisen (1966) and, independently, Zatsepin and Kuz’min (1966) p + hn → n+p+ p + hn → p+p° (p + hn → p+ e++e- ) Photopion production! Photodisintegration (Puget et al., 1976) Pair production (Blumenthal, 1970) A + hn → (A-1) + N A + hn → (A-2) + 2N A + hn → A+ e++e- E ~2*1020 eV (nuclei) XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  5. Energy (eV) 1 TeV = Fermilab CMB Radio IRB Flux / / / / / / / / / / / Visible e+e- X-rays GeV g-rays Ressell & Turner XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  6. Energy (eV) cosmic rays e+e- n XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe Halzen, Ressell & Turner

  7. Physics with Astroparticles Battiston, 2002 XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  8. The Observational Scenario is still uncertain and still under debate XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  9. Tens of events at energies > 5×1019 eV have been detected so far… Six ground based experiments have reported ~ 20 events at E>1020 eV 3.2X1020eV  Fly’s eye (Bird et al. 1995) 3.4X1020eV  AGASA (M. Teshima, 2000) Flux of 1 particle per km2 per century!! Several Observations… XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  10. HiRes collaboration, astro-ph/0208301 This discrepancies call for a study with a new approach: may need an experiment combining ground array with fluorescence such as the Auger project to resolve this issue.. XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  11. ( ) --- AGASA -10% Statistics ~2.4 σ (~2.0 σ) HiRes AGASA ~3.0 σ (~1.5σ) ~2.3 σ ~ 0σ ~ 0 σ Extended spectrum Super-GZK GZK-Hypothesis M. Teshima, 2002 De Marco et al., 2003 XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  12. 1600 (600 op.) water Cherenkov detectors 4 stations with 24 fluorescence telescope (6+6 op.) The Pierre Auger Observatory (South…) Jan 2005 68% AGASA XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  13. John Linsley in 1979 in the Field Committee Report of NASA “Call for Projects and Ideas in High Energy Astrophysics for the 1980s” The concept to observe, by means of Space Based devices looking at Nadir Nighttime, the fluorescence light produced by an EAS proceeding in the atmosphere In 1995 Yoshi Takahashi of UHA rediscovered the original idea and proposed the MASS program wich later became a reality with the OWL and EUSO studies XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  14. Kakimoto et al. , 1996 A. Bunner, 1967 • Large distance > 400 km • Large FOV XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  15. Large Target Mass of the atmosphere • Large Distance R but small proximity effect • Full sky coverage looking at both North and South sky Large encircled area: A Space Device (…EUSO) Small encircled area: AUGER XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  16. Full sky coverage South and North Sky are very different Great Attractor, Local Void, Galactic Center  South Local Super Cluster  North A. Olinto, 2003 By A.Kravtsov The base of the Scientific Rationale of Auger North Decision June 2005 Matter and Galaxies within 93 Mp XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  17. Comparison of UHECRs Experiments XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  18. Ongoing Studies/Concepts XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  19. The Extreme Universe Space Observatory XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  20. A Main UV Telescope + LIDAR XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  21. XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  22. XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  23. Number of events expected in five years of operation EUSO Red Book, 2004 XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  24. Neutrino Observations in atmosphere FLUORESCENCE CHERENKOV ? Bottai, 2004 XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  25. EUSO Red Book, 2004; Bottai, 2004 Speculative models AUGER Region of ‘safe’ neutrino astronomy EUSO (Kalashek, Kuzmin, Semokov, Sigl) Phys. Rev. D66 2002 GZK gives only granted flux of cosmic neutrinos XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  26. Paolo Lipari, 2004 skimming ~GZK(A) downward XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  27. The trigger efficiency XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  28. The Tracking Ultraviolet Set-up Mission XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  29. TUS main figures R&D to be completed within 2005 Mission is planned for 2007-2009 XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  30. Between Present and future: OWL XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  31. The future XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  32. “Opening Particle Astronomy to probe and understand the evolving Universe”A scientific Theme proposed in response to the ESA D-Sci “Call for themes for Cosmic Vision 2015-2025” XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  33. Opening Particle Astronomy • This will open up the field of "Particle Astronomy" and its correlations with radio, photo, X and g astronomy. • To Search for UHE neutrinos Blasi & De Marco, 2003 A powerful enough detector will allow to study (within the GZK neighbourhood) : • Source densities, • Source intensities, • Individual source spectra. • … 2 Main “Requirements” Effective Aperture 50-100 times Auger 10 times EUSO Energy threshold close to 1018 eV XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe Blasi & De Marco, 2003

  34. Code provided by E. Parizot, 2005 Plagnol, 2005 XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  35. Based on the analysis of Blasi & De Marco, 2003 source density of 10 -5 sources/Mpsec (in fact, 10-4 to 10-6). Plagnol, 2005 Conclusion : A precise study of individual source spectrum (g, Emax) would benefit strongly from an increase of efficiency : UHECR Astronomy XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  36. AUGER EUSO 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 XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  37. XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  38. Task 1: Optics • Large Area (pupil  2m  5-7m) and Large field of view ( 90° full angle) Optical systems • Deployability/Assembling in space • Materials (High Throughput, Light weight, contaminants…) • Filter (coatings multilayers…) XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  39. Piero Mazzinghi, Vojko Bratina (INOA) A proposed 5 m EPD 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 • Entrance pupil MUST be in the mirror centre of curvature • Mirror is then larger than EPD (depending on FOV) • Light shield is anyway necessary for stray light reduction • The correcting plate greatly improves performances • F/# investigated as low as 0.6 • Detector diameter smaller than any other proposed solution • Weight saving solution (both for optics and detector) • Obscuration acceptable for FOV up to 25° • Vignetting almost constant for all FOV • Low sensitivity to misalignment (except decenter) • Optical system design scalable to any dimension focal plane XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  40. 833.33 MM OWL/AIRWATCH Maksutov Type Telescope Scale: 0.03 DJL 17-Mar-99 Fresnel-Maksutov Optics 0.1o Pixel Angular Resolution in UV ~ 104 away from Diffraction Limit D. Lamb et al., NASA/MSFC University of Alabama, Huntsville Maksutov-Mangin (Pitalo-Lamb) makes =0.02 FOV=50, Ro/R = 0.7 XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  41. Assembling in space … On the ISS stay there or move as a free flyer By robots on the launchers XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  42. XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  43. Task 2: Sensors Detectors • High Efficiency Sensors; • Compact and light-weight (solid state ?) • High Efficiency detectors (how high ? The highest…) • Large area, large number of pixels (channels) 106? • Maximizing filling factor, cooling system • Light collector/filter SiPM at MPI R&D goals: increase SiPM size from 1 mm up to (3-5)mm increase in QE up to 70% XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  44. Task 3: Electronics • Front End (fast, low power, miniaturized, mixed analogue/digital) • “Smart” Triggering systems (efficient, highly selective, configurable, adaptive) • OBDH electronics (fast analysis of large amount of data, compliant with usually limited telemetry resources; “interaction” with the Atmosphere Monitoring System) XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  45. Task 4: Mission Concept (?) • Formation flights • Stereo operation • Variable Orbits XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

  46. Conclusions • Space-Based observation of UHECR can provide a breakthrough in the field • EUSO can be consider a pathfinder in the field, and the studies associated have provided unvaluable info for new developments • To succeed, the support of the entire HEAP community is mandatory • A solid and realistic R&D program must be developed, already started… • Convince the High Energy Astrophysics Community that UHECR studies could provide a step forward in our understanding of the Universe… XXXXth Rencontres de MORIOND Very High Energy Phenomena in the Universe

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