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3D simulation Of Extensive Air Showers at Pierre Auger Observatory

3D simulation Of Extensive Air Showers at Pierre Auger Observatory. Santiago de Compostela 3 rd IDPASC school. Auger LIP Group. João Espadanal , Patricia Gonçalves , Mário Pimenta. 24-01-2013. 1. Motivation. Pierre Auger Observatory : Motivation. Cosmic Ray spectrum.

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3D simulation Of Extensive Air Showers at Pierre Auger Observatory

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  1. 3D simulation Of Extensive Air Showers at Pierre Auger Observatory Santiago de Compostela 3rd IDPASC school Auger LIP Group JoãoEspadanal, Patricia Gonçalves, MárioPimenta 24-01-2013

  2. 1. Motivation Pierre AugerObservatory: Motivation Cosmic Ray spectrum Study of Cosmic Rays at ultra high Energies many challenges What is the shape at the end of the spectrum? What is the composition of cosmic rays? What is the origin of these extremely energetic particles? Are the physical interactions the same? Are there new interactions? ?

  3. 1. Cosmic Rays and The Pierre Auger Observatory Extensive Air Shower Air shower Detection: How to detect a cosmic ray? Hadronic interactions and high energy physics Cherenkov Light Shower development Fluorescence Light Energy Deposited (dE/dX)max Cosmic Ray Primary Energy Quasi calorimetric energy measurement Xmax g/cm2 of crossed atmosphere

  4. 1. Cosmic Rays and The Pierre Auger Observatory Pierre Auger Observatory Pierre Auger Observatory The Pierre Auger Observatory (PAO) was recently completed (3000km2, 1600 Cherenkov tanks and 4 FD facilities, ...) With this experiment we have better quality and higher statistics than ever PAO uses SD and FD detection techniques simultaneously, Hybrid technique. Has a very good atmospheric monitoring to better control the systematic uncertainty Allows studies up to 1021eVevents (lab frame) SD detectors FD detectors (Fluorescence Detectors) (Surface Detectors)

  5. 2. Extensive Air Showers structure Extensive Air Showers structure Fluorescence Light Cherenkov Light Light detected is mostly Fluorescence Light detected dominated by Cherenkov • RayleightScattering • Mie Scattering

  6. 2. Extensive Air Showers structure Light Detected in the Telescope One typical event: Time signal in one pixel Shower Length in Time • Fluorescence rich event • Cherenkov rich event

  7. 2. Extensive Air Showers structure Shower in 3 Dimensions • Shower in 3D space Shower intrinsic width Detector effects Atmospheric effects SDId 3599086 Energy = 1.58x1019 Distance to eye= 3.87 km • Light aberration • Internal reflections • Reflections and detections efficiencies Shower intrinsic width Shower Image width Atmosphere Detector Multi Scattering Multi Scattering

  8. 3. 3D Simulation Method 3D Simulation: motivation We generate the air showers All informationis projected into a line Longitudinal profiles Is Better to have To study interesting lateral information we need to have a 3D simulation, instead of having the information projected into a line( at the generator level)

  9. 3. 3D Simulation Method BinTheSky Framework Solution (at generator) • Bins with Cylindrical geometry at generator level • r : 50 x 20m •  : 24 x 15 deg z : 300 x 100 m • (size: 1000m x 360 degx 30000 m) Relatively easy to implement Fluorescence light emission: Energy Deposit => Isotropic emission • Cherenkov Emission? Energy Deposit for fluorescence emission

  10. 3. 3D Simulation Method BinTheSky: Information for Cherenkov emission • Information for Cherenkov (in generator to be used in Auger Framework): l – length travel by electron in bin 𝚫𝝓 bin = 1º Electron Length distribution N Electron angle distribution bin = 1º direction Electron Length distribution NElectron angle distribution

  11. 3. 3D Simulation Method BinTheSky: In Auger Offline Framework • BinTheSkyembodied in the Auger Offline Framework • (Auger Simulation and reconstruction software) • In ShowerSimulatorLX: • Produce photons: Fluorescence emission Cherenkov emission • Propagate Photons to detector using geometrical information : • solid angle • emission angle • distance to telescope • Attenuate and scatter photons • Cherenkov scattered • Multiple-scattering Propagation time Emission time SkyBin 𝚫𝝓 bin = 1º • for each SkyBinfind andbinsin FoV. • Calculate the solid angle and attenuation for (, ) bin. bin = 1º 1bin in and 𝚫𝝓

  12. 3. 3D Simulation Method BinTheSky: Cherenkov Emission tests • Cherenkov Pool on ground for a shower with θ=63º: • Heat Telescope, Field-of-View ( 30o – 60o) Shower Direction • FD Telescope, FoV ( 0o - 30o)

  13. 4. Fluorescence and Cherenkov Results Fluorescence and Cherenkov Validation • Fluorescence Emission • Cherenkov Emission • Energy distribution • Energy distribution Preliminary • Standard Simulation • 3D Simulation • Data • Xmax distribution • Xmax distribution Preliminary

  14. 4. Fluorescence and Cherenkov Results Future Analyses on Lateral distributions Preliminary Zeta distance Preliminary • Standard Simulation • 3D Simulation • Data

  15. Summary and prospects • We saw that the Fluorescence emission was validated (GAP-2012-039) • Cherenkov emission is being tested • Firsts longitudinal results compatible with standard Simulation • Further validation with a large sample of data events • with Cherenkov and Fluorescence • Future Work: • Study and comprehension of the transverse light profile • Cherenkov studies in HEAT • Implement Scattered Cherenkov • Full implementation of a 3D Simulation and 3D reconstruction • Applications to the Telescopes HEAT + Coihueco

  16. Thank You

  17. 1. Cosmic Rays and The Pierre Auger Observatory Pierre Auger Observatory • Pierre Auger Observatory The Pierre Auger Observatory (PAO) was completed in May 2008 (3000km2, 1600 Cherenkov tanks and 4 FD facilities, ...) Hybrid technique With this experiment we have better quality and higher number of cosmic ray events than ever Malargue, Argentina

  18. 1. Cosmic Rays and The Pierre Auger Observatory FluorescenceDetectors • Fluorescence Detector (FD) • PMT Pixels • 4 stations with 6 telescopes • Each telescope with each with 30º x 28.6º field of view • Camara with 440 PMT pixels (20 x 22) • Several calibrating systems • Laser system, LIDAR stations, Aerosol monitors, clouds and stars monitoring • ~10% duty cycle FD Camera representation FD building design FD Telescope design

  19. 3. 3D Simulation Method BinTheSky: Information for Cherenkov emission • Information for Cherenkov (in generator to be used in Auger Framework): l – length travel by electron in bin xsh 𝚫𝝓 bin = 1º ysh Electron Length distribution N Electron angle distribution bin = 1º direction Electron Length distribution NElectron angle distribution

  20. Final 𝝓 distribution of electrons Final 𝜶 distribution of electrons

  21. The 3D validation procedure Select data Events Generate those events in CORSIKA With BinTheSky Framework 3D Simulation in offline (using the BinTheSky information) + Offline Reconstruction KG Simulation in offline + Offline Reconstruction • Fluorescence emission is validated (GAP-2012-039) • Cherenkov emissionOn progress Compare

  22. 4. Fluorescence and Cherenkov Results Fluorescence Validation • Energy distribution 3D simulation of EAS for the FD: validation with a Fluorescence rich data sample (internal note GAP-2012-039) • dE/dX Sum of the events • Xmax distribution • Standard Simulation • 3D Simulation • Data

  23. 4. Fluorescence and Cherenkov Results Cherenkov Validation in Progress • Energy distribution Preliminary • dE/dX Sum of the events Preliminary • Xmax distribution Preliminary • Standard Simulation • 3D Simulation • Data

  24. SDiD: 4943331 • SDiD: 4943331 • 3D • Data • KG

  25. SDiD: 4943331 • SDiD: 4943331 • 3D Data • KG

  26. SDiD: 4943331 • 3D • Data • KG

  27. SDiD: 4943331 • Data • 3D • KG

  28. SDiD: 4943331 • Data • 3D • KG

  29. A few Results • SDiD: 9721432 • 3D • Data • KG

  30. SDiD: 9721432 • SDiD: 9721432 • 3D Data • KG

  31. SDiD: 9721432 • Data • 3D • KG

  32. SDiD: 9721432 • Data • 3D • KG

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