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“Phase A study” final report

EUSO. E. U. S. O. xtreme. niverse. pace. bservatory. Simulation Subsystem. Status Report. Vincent Van Gogh, “The starry night”. An Innovative Space Mission doing Astronomy by looking downward from the Space Station at the Earth Atmosphere. “Phase A study” final report.

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“Phase A study” final report

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  1. EUSO E U S O xtreme niverse pace bservatory Simulation Subsystem Status Report Vincent Van Gogh, “The starry night” An Innovative Space Mission doing Astronomy by looking downward from the Space Station at the Earth Atmosphere “Phase A study” final report Giacomo D’Alì Staiti, München, November 19, 2003 EUSO: Extreme Universe Space Observatory

  2. EUSO EUSO : Extreme Universe Space Observatory Event Simulation Strategy • Simulate the Physics processes • Simulate the experimental conditions • Work out the expected signal • Test the reconstruction algorithms (SDA/SIM) • Work out the expected acceptance and resolution for the physics parameters • Check the compliance with overall scientific requirements • Set the scientific requirements as far as: • Detector performances • Allowed background level, • Atmospheric sounding accuracy Giacomo D’Alì Staiti, München, November 19, 2003

  3. EUSO EUSO : Extreme Universe Space Observatory Giacomo D’Alì Staiti, München, November 19, 2003 The End-to-End Simulation Approach Physics Process Simulation Housekeeping, calibration ancillary and atmospheric sounding data • Event generators: • fast generator, bulk event generator, 2nd order effect simulation • EECRs, EEn, Meteors, Lightning) Event by event Correction factors Active target Simulation Fluorescence yield Cerenkov light production Atmosphere description Absorption and Transmission Pressure, temperature, Clouds effect Event Reconstruction Event (EECR, EEn, Meteor,..) Direction Reconstruction Energy Reconstruction Particle identification Raw-like data Raw data Detector Simulation Geometry description Optics description Focal surface description Electronics description Trigger simulation Physics Event Analysis

  4. EUSO No fluctuation on results Fast overlook Large scale fluctuations(0.1km) Bulk simulation Detailed physics and fluctuation description Cross-check, 2nd order effects EUSO : Extreme Universe Space Observatory UHECR Event Generator and Shower Simulator E>1019 eV, Nmax>1010 particles GL J. Linsley’s work to adapt Greisen’s formula to hadron-initiated showers CORSIKA, (AIRES) The UHECR standard for shower simulation UNISIM The hybrid method Florence Paris CdF, SLAST, Annecy Worldwide standard, Pa, Fi, Ge, Paris, Leeds Giacomo D’Alì Staiti, München, November 19, 2003

  5. EUSO The Event Generators GIL (SLAST/Fly) .vs. CORSIKA UNISIM .vs. CORSIKA EUSO : Extreme Universe Space Observatory Giacomo D’Alì Staiti, München, November 19, 2003

  6. EUSO Giacomo D’Alì Staiti, München, November 19, 2003 EUSO : Extreme Universe Space Observatory The Light to EUSO The Fluorescence yield, the diffusion process of the Čerenkov photons at ground and the light transmission through the atmosphere determine, for a given shower, the amount of light received by EUSO. The simulation S/W handles the most relevant effects, and their dependence upon the atmospheric parameters. In standard situation and “clear sky” life would be relatively easy…

  7. EUSO Giacomo D’Alì Staiti, München, November 19, 2003 EUSO : Extreme Universe Space Observatory The Real Atmosphere Unfortunately the real atmosphere is non standard,… non uniform… C.Berat, D.Lebrun, A.Stutz, SIM-REP-012

  8. EUSO Giacomo D’Alì Staiti, München, November 19, 2003 EUSO : Extreme Universe Space Observatory The Real Atmosphere …and life becomes more complicate. The fluorescence yield can vary, the primary mass gets confused C.Berat, D.Lebrun, A.Stutz, SIM-REP-012 …and the real atmosphere has to be known for retrieving the shower features

  9. EUSO Giacomo D’Alì Staiti, München, November 19, 2003 EUSO : Extreme Universe Space Observatory The Real Atmosphere …nor it is clear E. Plagnol,2003 Clouds are present most of the time and modify the scenario seen by EUSO and the 3D target where the shower develop.

  10. EUSO Giacomo D’Alì Staiti, München, November 19, 2003 EUSO : Extreme Universe Space Observatory Atmosphere Simulation summary • Different models and the modification of atmosphere parameters can be handled; • Cloud presence has been taken into account from a statistical point of view; • According to the review panel reccomandation the “scientific requirements” for the knowledge of atmosphere have to be given:  study of experimental resolution (direction, energy, Xmax) as a function of  the accuracy on atmospheric transmission coefficient  the precision on the cloud height determination  the cloud topology ISSUE TREATED AT LENGTH DURING ATMOSPHERIC SOUNDING SESSION

  11. EUSO Giacomo D’Alì Staiti, München, November 19, 2003 EUSO : Extreme Universe Space Observatory The signal collected by EUSO And for low energy “Auger”protons E. Plagnol, S. Bottai, 2003 For a typical 1020 eV event

  12. EUSO Giacomo D’Alì Staiti, München, November 19, 2003 EUSO : Extreme Universe Space Observatory The EUSO trigger efficiency The trigger efficiency in the low end of the energy region, in a “clear sky” environment… …and in the ISCCP cloudy environment , in different zenith angle regions. S. Bottai, 2003 Green curve: requirements see RedBook. Red curve: simulation with 2.3 EPD and baseline optics See RedBook. All curves refer to 2.3 EPD and baseline optics

  13. EUSO Giacomo D’Alì Staiti, München, November 19, 2003 EUSO : Extreme Universe Space Observatory The EUSO acceptance E. Plagnol, 2003

  14. EUSO Giacomo D’Alì Staiti, München, November 19, 2003 EUSO : Extreme Universe Space Observatory The Expected number of events after 3 years data taking …normalised to a duty duty cycle of ~19% (new estimate by F. Montanet, November 2003)

  15. EUSO Giacomo D’Alì Staiti, München, November 19, 2003 EUSO : Extreme Universe Space Observatory DOWNWARD NEUTRINO ACCEPTANCE FOR EUSO ( RedBook ) • 2 * 1018 g is the total target mass under the FOV • reduction due to trigger efficiency is calculated by full simulation of nover 2p. Clouds distribution is considered • reduction due to selection efficiency needed for 10-4 proton rejection has been calculated from full simulation • results show a sensitivity around 10 times AUGER for neutrino in the1020eV energy region golden Fluorescence only Xmax Select. P+ n Shape Select. n S. Bottai P+ Rejection > 10-4

  16. EUSO Giacomo D’Alì Staiti, München, November 19, 2003 EUSO : Extreme Universe Space Observatory EUSO SENSITIVITY Red line is the flux resulting in 1 event/year/decade in energy Blu line ‘ the same ‘ for Auger [1] Oleg E. Kalashev, Vadim A. Kuzmin, Dmitry V. Semikoz, Gunter Sigl. “ULTRAHIGH-ENERGY NEUTRINO FLUXES AND THEIR CONSTRAINTS” Phys.Rev.D66:063004,2002 ZBURST (>100 events/year in EUSO ) GZK(B) (~10 events/year in EUSO ) (both GZK and ZBURST here are the most intense of their category allowed in ref [1] ) TD (A,B,C) (~5 events/year ) ; MR (~ 10 events/year) are topological defect and massive relic fluxes of typical intensity ! S. Bottai EUSO IS SENSITIVE TO TOP DOWN, ZBURST FLUXES AND HIGH INTENSITY GZK FLUXES

  17. EUSO Giacomo D’Alì Staiti, München, November 19, 2003 EUSO : Extreme Universe Space Observatory The Angular Resolution M.C. Maccarone, 2003 J. Dolbeau, 2003 At high energy, without Cerenkov footprint information At 1020 eV, using the Cerenkov footprint position

  18. EUSO 20 ? q(deg)\En.(10 eV) <1,5 1,5 to 3 3 to 4,5 4,5 to 6 6 to 7,5 7,5 to 9 >9 72,50 0,15 0,19 0,17 0,15 0,17 0,18 0,19 77,50 0,18 0,17 0,19 0,15 0,16 0,19 0,17 82,50 0,19 0,2 0,18 0,17 0,18 0,2 0,2 87,50 0,21 0,18 0,21 0,19 0,22 0,18 0,19 Giacomo D’Alì Staiti, München, November 19, 2003 EUSO : Extreme Universe Space Observatory The energy resolution Golden Events Preliminary Fluo_only events D. Naumov, 2003

  19. EUSO Giacomo D’Alì Staiti, München, November 19, 2003 EUSO : Extreme Universe Space Observatory The Xmax reconstruction capability (preliminary) Preliminary Golden events Fluo_only events The detailed study of the composition sensitivity will be done during next phase, only the separation neutrino/hadron have been exploited at this level

  20. EUSO Giacomo D’Alì Staiti, München, November 19, 2003 EUSO : Extreme Universe Space Observatory End-to-end Simulation – The ingredients Conclusions • At the end of phase A the ingredients are there: • Event generators(GIL-Fast parametric, UNISIM- Bulk hybrid, CORSIKA- Full (to be improved) • Fluorescence yield (energy dependence, humidity dependence under development) • Atmosphere transmission (standard and MSISE-based models, adjustable parameters, cloud optical depth present, multiple scattering under study) • Detector Description (ESAF detailed description designed, see next talk) • Reconstruction algorithms – shower directions, first release for energy and Xmax reconstruction. • Priorities: • Detail the “scientific requirements” for the atmospheric sounding device(i.e. the sensitivity of the reconstructed shower features/ of the flux measurement to the precision with which the atmospheric parameters (including cloud altitude, coverage, optical depth) have to be known (STARTED). • Complete the frame design to “cook the ingredients” in the “ESAF Kitchen” in order to connect them into a real “End-to-End simulation chain”; • Include a “signal retrieval” algorithm (feedback from the atmosphere sounding device) for the “event by event reconstruction” in the simulation chain • Improve the confidence and the reliability of the existing “ingredients” (shower generators, atmosphere description, detector performances, reconstruction algorithms) • Address the mass resolution issue for the shower primaries.

  21. EUSO and ATMOSPHERIC SOUNDING • Features of EUSO (positive andnegative) • EUSO will detect showers above the clouds • - Shower maxima are ~7 km • - 63% of the sky is clear above 3.2 km • The distance to the EAS is well known • Measurements of the EAS tail can be neglected • - minimizing dependence on MIE scattering corrections • - less mixing of Cherenkov and fluorescent signals • The range to the EAS is <1000 g/cm2, half that of typical ground-based measurements • Signals at EUSO are weak, requiring single photon counting • EUSO must use the global atmosphere, not just the desert atmosphere

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