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Approved by ESA for the “Phase A study” on the International Space Station

EUSO. E. U. S. O. xtreme. niverse. pace. bservatory. Simulation Subsystem G. D’Alì Staiti On behalf of Sergio Bottai. UNISIM and “the hybrid simulation STATUS Report. Vincent Van Gogh, “The starry night”. An Innovative Space Mission doing Astronomy by looking downward

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Approved by ESA for the “Phase A study” on the International Space Station

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  1. EUSO E U S O xtreme niverse pace bservatory Simulation Subsystem G. D’Alì Staiti On behalf of Sergio Bottai UNISIM and “the hybrid simulation 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 Approved by ESA for the “Phase A study” on the International Space Station Giacomo D’Alì Staiti, Huntsville, May 21, 2003 EUSO: Extreme Universe Space Observatory

  2. S. Bottai 05-2003 UNISIM GENERAL CHARACTERISTICS FAST SHOWER SIMULATION HYBRID METHODS : FULL MC SIMULATION FOR E>Eth , PARAMETRIZATION FOR E<Eth. Good reproduction of fluctuations with Eth=1017eV. 3D GEOMETRY AND EARTH CURVATURE LPM EFFECT INCLUDED NEUTRINO SIMULATION OF EHE NEUTRINO INTERACTIONS CC+NC SIMULATION OF CHERENKOV LIGHT EMISSION AND PROPAGATION OF FLUORESCENCE AND CHERENKOV LIGHT using E. Plagnol transport code SIMPLE AND "IDEAL" DETECTOR SIMULATION WITH VARIABILITY OF DETECTOR PARAMETERS INTERFACED WITH ESAF (Note by G. D’Alì Staiti)

  3. S. Bottai 05-2003 UNISIM : THE HYBRID METHOD EHE SHOWERS ( 1011 particles ) full parametrization hybrid full montecarlo ! thinning DESIRED RESULTS large + small scale (m -cm) fluctuations ( AUGER ) large scale (0.1km) fluctuations(xmax,smax...) ( EUSO ? ) no fluctuations on result

  4. S. Bottai 05-2003 the cherenkov light simulation in UNISIM • The generation of Cherenkov light during each step of shower propagation is calculated using the energy distribution of electrons given in : A M Hillas J. Phys. G Nucl. Phys. 8 (1982). • The angular distribution of emitted photons is simulated using the parametrization of electrons angular distribution ( Baltrusaitis et al. J. Phys. G Nucl. Phys. 13 (1987) ) convoluted with Cherenkov cone emission. Good agreement with full simulation approach performed in D.B. Kieda Astr. Phys. 4 (1995) for radial and energy distribution of photons at ground. • Propagation in atmosphere according to Rayleigh scattering and isotropic diffusion at ground

  5. S. Bottai 05-2003 NEW FEATURES OF UNISIM Old version of UNISIM can handle only events whose directions point to the ground (like in Corsika or AIRES ) . But Almost horizontal and upgoing neutrino showers does not match this limitation. A new atmospheric-geometrical package has been added to generalize the code to any possible shower path through the atmosphere. Simulation of Showers having no intersection with ground is now possible. (April 03) + Simulation of cherenkov photons scattered in atmosphere and directed to the EUSO pupil has been added by the interface to the E. Plagnol atmospherich transport code. (March 03)

  6. S. Bottai 05-2003 ON GOING ACTIVITIES ON UNISIM (the core of simulation) A project for a new, updated and mantained hybrid simulation program for EUSO/OWL has started in collaboration with T. Stanev and his collaborators (foreseen for 2004). It will contain new interaction models, new shower libraries precomputed at any depth. INTERACTION MODELS SIMULATE THE INTERACTION OF THE PRIMARY T. Stanev group, at Bartol Res. Institute is mantaining and developing an hybrid shower code with updated interaction models : Phys.Rev D66 2002 An agreement has been reached for a collaboration between EUSO and his group in order to continue the development of the hybrid simulation approach FULL SIMULATION OF SECONDARIES UNTIL THEIR ENERGY BECAME LOWER THAN A MINIMUM ENERGY USE PARAMETRIZATIONS OR PRECOMPUTED SHOWER LIBRARIES TO SIMULATE THE DEVELOPMENT OF SUBSHOWERS

  7. EFFECTIVE ACCEPTANCE FOR PROTONS S. Bottai 05-2003 Trigger: Npix=5 Npers.=3 ; Shower maximum visible M36 with grouping of 2X2 pixel for trigger CLOUDS FREQUENCY AND CLOUDS ALTITUDE DISTRIBUTIONS FROM ISCCP -51o<lat.< 510 (see E. Plagnol doc) M36 CLEAR SKY

  8. Proton – neutrino discrimination S. Bottai 05-2003 Proton spectrum according to E-2.7, 3 years of data taking Neutrino spectrum : E-1 3*1019 – 1021 (arbitrary large statistics) The probability of neutrino interaction in atmosphere is proportional to the atmospheric density. protons neutrinos

  9. S. Bottai 05-2003 Xmax selection for neutrino-proton discrimination (it needs reconstruction of profiles in slant depth) NEUTRINOS 2000 g/cm2 1400 g/cm2 PROTONS

  10. S. Bottai 05-2003 THE DETECTION OF CHERENKOV PEAK WILL GUARANTEE A PRECISE DEPTH RECONSTRUCTION, BUT START TO BE INEFFICIENT FOR NEUTRINOS WITH ZENITH ANGLE GREATER THAN 70 DEG TRIGGERED NEUTRINOS 0.08 ALBEDO TRIGGERED NEUTRINOS HAVING AT LEAST 4 CHERENKOV PE

  11. S. Bottai 05-2003 SHOWER PROFILES 15 SHOWERS WITH E=1020eV, qzen=80o SEE ALSO : EUSO-SIM-REP-003-1 NEUTRINOS CC INTERACTIONS (LPM effect included) PROTONS

  12. S. Bottai 05-2003 EVENTS WITHOUT CHERENKOV PEAK PROTONS AND NEUTRINOS SHOWERS HAVE DIFFERENT SHAPES IN LONGITUDINAL DEPTH , AND EVEN MUCH MORE DIFFERENT SHAPES IN SPACE (km) SINCE THEY DEVELOPS AT DIFFERENT ALTITUDES AND HENCE AT DIFFERENT ATMOSPHERICH DENSITY PROTONS THE DURATION OF THE DETECTED SIGNAL IS A SIMPLE SHAPE (km) DEPENDENT QUANTITY NEUTRINOS BETTER RESULTS ARE EXPECTED WITH A MORE SOPHISTICATED SHAPE ANALYSIS ( see D. Naumov xmax reconstruction)

  13. Identification of the Primary Scientific S I Mulations andData Analysis Proton and electron neutrino shower profiles, as they could appear, in terms of depth…. After E. Plagnol, EUSO Internal Report G. D’Alì Staiti, EUSO General Meeting, November 2002

  14. Scientific S I Mulationsand Data Analysis Identification of the Primary … and in terms of time. After E. Plagnol, EUSO Internal Report 20 nsecs ~100 nsecs G. D’Alì Staiti, EUSO General Meeting, November 2002

  15. EFFECTIVE ACCEPTANCE FOR NEUTRINOS S. Bottai 05-2003 ( selections : trigger, xmax > 1400g/cm2 ) Trigger: Npix=5 Npers.=3 M36 with grouping of 2X2 pixel for trigger CC CC M36 NC CLEAR SKY NC

  16. EFFECTIVE ACCEPTANCE FOR NEUTRINOS S. Bottai 05-2003 Trigger: Npix=5 Npers.=3 CC M36 with grouping of 2X2 pixel for trigger CC M36 NC CLOUD FREQUENCY AND CLOUD ALTITUDE DISTRIBUTIONS FROM ISCCP -51o<lat.< 510 (see E. Plagnol doc) NC

  17. S. Bottai 05-2003 EFFECTIVE ACCEPTANCE FOR NEUTRINOS ( further event selection criterium: shower max above clouds) Trigger: Npix=5 Npers.=3 M36 with grouping of 2X2 pixel for trigger M36 CLOUD FREQUENCY AND CLOUD ALTITUDE DISTRIBUTIONS FROM ISCCP -51o<lat.< 510 (see E. Plagnol doc)

  18. S. Bottai 05-2003 NEW PRODUCTION OF PHP FILES the simulated data set ( 19.000 showers ) • 5000 proton, 5000 iron, 5000 neutrino showers with energy in the range 1019 eV – 1021 eV , E-1 spectrum and expected angular distribution. • 2000 proton showers with E= 5 x 1019 eV • 2000 proton showers with E= 1020 eV Format including definitions in last version of : EUSO-SIM-REP-004-1.1 • New Simulation features : • back scattered cherenkov light • Fully horizontal neutrino events (CC+NC) To be stored at ESAF repository in LYON

  19. EUSO EUSO : Extreme Universe Space Observatory Giacomo D’Alì Staiti, Huntsville, May 21, 2003 Simulation Baseline • DETECTOR • altitude of ISS : 430 km • FOV = +/- 30 deg • area of entrance pupill : 3.14 m^2 • overall optics efficiency including filter (cfr IRB draft by A. Petrolini) • OPTICS • EPS_opt (gamma) = (photons incident on FS)/(photons hitting the pupil), not dependent on wavelenght : • EPS_opt (gamma) = (0.453 -0.000235*gamma*gamma)/(cos(gamma)^3) • where gamma (0.-30 deg) is the arrival angle of the light respect to the central axis of the detecor • spot size of the optics: • S. Bottai plots (cfr IRB draft by A. Petrolini) :2D gaussian at any field angle withsigma_x=sigma_y=4.5/2./SQRT(2.)mm • E. Plagnol plots, it has directly been given by OS people (Ask E. Plagnol for thedetails) • default pixel size : (M36) diameter=4.5mm (0.77 km at ground on the EUSO nadir) • FOCAL SURFACE • overall efficiency of the focal surface (cfr IRB draft, by A. Petrolini) independent on wavelenght :  • EPS_fs= 0.13 S. Bottai, April 2003

  20. EUSO EUSO : Extreme Universe Space Observatory Giacomo D’Alì Staiti, Huntsville, May 21, 2003 Simulation Baseline • ELECTRONICS • GTU lenght = 3*833 ns • trigger : NPE p.e. in any Pixel of a Macrocell , with NPE NTHRpixel in a GTU AND Npers (number of (consecutive) GTUs within the same Macrocell, with NpersNTHRpers • BACKGROUND • 3*1011 ph./(m2×sec×sr), uniform at the PMT level ENVIROMENTAL CONDITIONS • clear sky (unless differntly specified, according to ISCCP statistics) • lowtran7 transmission , standard US atmosphere (see attached doc) • 3 wavelenght fluorescence yield : 337, 357, 391 nm normalized on the entire spectrum content (300-400 nm) and generated according to : altitude, wavelenght (see attached doc) • cherenkov light generated (300-400 nm) according to shower age dependence of electron spectrum and shower age dependence of electrons angular distribution. 8% albedo for the ground. • SHOWER GENERATOR : • UNISIM hybrid generator with shower to shower fluctuations, SYBILL model used for the interactions. lpm effect included (S.Bottai) • GIL parameterisation of longitudinal profile (E.Plagnol) S. Bottai, April 2003

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