1 João Espadanal, Patricia Gonçalves, Mário Pimenta Santiago de Compostela 3 rd IDPASC school Auger LIP Group 3D simulation Of Extensive Air Showers at Pierre Auger Observatory

3 rd IDPASC School João EspadanalJanuary 2012 /15 Pierre Auger Observatory: Motivation Cosmic Ray spectrumStudy 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? new interactions Are there new interactions? ? 1. Motivation 2

3 rd IDPASC School João EspadanalJanuary 2012 /15 Extensive Air Shower 3 Air shower Detection: (dE/dX)max Hadronic interactions and high energy physics Shower development Cosmic Ray Primary Energy Quasi calorimetric energy measurement g/cm 2 of crossed atmosphere Xmax Energy Deposited Fluorescence Light How to detect a cosmic ray? Cherenkov Light 1. Cosmic Rays and The Pierre Auger Observatory

3 rd IDPASC School João EspadanalJanuary 2012 /15 Pierre Auger Observatory Pierre Auger Observatory 4 The Pierre Auger Observatory (PAO) was recently completed (3000km 2, 1600 Cherenkov tanks and 4 FD facilities,...) With this experiment we have better quality and higher statistics than ever Hybrid technique PAO uses SD and FD detection techniques simultaneously, Hybrid technique. control the systematic uncertainty Has a very good atmospheric monitoring to better control the systematic uncertainty studies up to eV Allows studies up to eV events (lab frame) Pierre Auger Observatory SD detectorsFD detectors (Surface Detectors) (Fluorescence Detectors) 1. Cosmic Rays and The Pierre Auger Observatory

3 rd IDPASC School João EspadanalJanuary 2012 /15 Extensive Air Showers structure 2. Extensive Air Showers structure Cherenkov Light Fluorescence Light Light detected is mostly Fluorescence Light detected dominated by Cherenkov 5  Rayleight Scattering  Mie Scattering

3 rd IDPASC School João EspadanalJanuary 2012 /15 Light Detected in the Telescope 6 One typical event: Time signal in one pixel  Fluorescence rich event  Cherenkov rich event Shower Length in Time 2. Extensive Air Showers structure

3 rd IDPASC School João EspadanalJanuary 2012 /15 Shower in 3 Dimensions Shower in 3 Dimensions 7 SDId Energy = 1.58x10 19 Distance to eye = 3.87 km Shower intrinsic width  Shower in 3D space Detector effects Atmospheric effects Shower Image width Shower intrinsic width DetectorAtmosphere 2. Extensive Air Showers structure  Light aberration  Internal reflections  Reflections and detections efficiencies Multi Scattering

3 rd IDPASC School João EspadanalJanuary 2012 /158 We generate the air showers All information is projected into a line 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) Is Better to have 3. 3D Simulation Method 3D Simulation: motivation Longitudinal profiles

3 rd IDPASC School João EspadanalJanuary 2012 /15 BinTheSky Framework Solution (at generator) BinTheSky Framework Solution (at generator) 9 Energy Deposit for fluorescence emission 3. 3D Simulation Method r : 50 x 20m  : 24 x 15 deg z : 300 x 100 m (size: 1000m x 360 deg x m)  Relatively easy to implement Fluorescence light emission: Energy Deposit => Isotropic emission  Bins with Cylindrical geometry at generator level  Cherenkov Emission?

3 rd IDPASC School João EspadanalJanuary 2012 /15 BinTheSky: Information for Cherenkov emission  Information for Cherenkov (in generator to be used in Auger Framework): Electron Length distribution NElectron angle distribution Electron Length distribution N Electron angle distribution bin = 1º l – length travel by electron in bin D Simulation Method

3 rd IDPASC School João EspadanalJanuary 2012 /15 BinTheSky: In Auger Offline Framework Propagation time Emission time bin = 1º  BinTheSky embodied in the Auger Offline Framework (Auger Simulation and reconstruction software) SkyBin 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 D Simulation Method

3 rd IDPASC School João EspadanalJanuary 2012 /15 BinTheSky: Cherenkov Emission tests 12  Cherenkov Pool on ground for a shower with θ=63º: Heat Telescope, Field-of-View ( 30 o – 60 o ) FD Telescope, FoV ( 0 o - 30 o ) 3. 3D Simulation Method Shower Direction

3 rd IDPASC School João EspadanalJanuary 2012 /15 Fluorescence and Cherenkov Validation 13 Energy distribution Xmax distribution 4. Fluorescence and Cherenkov Results Energy distribution Xmax distribution Preliminary  Standard Simulation  3D Simulation  Data  Fluorescence Emission  Cherenkov Emission

3 rd IDPASC School João EspadanalJanuary 2012 /15 Future Analyses on Lateral distributions 14 Zeta distance 4. Fluorescence and Cherenkov Results Preliminary  Standard Simulation  3D Simulation  Data

3 rd IDPASC School João EspadanalJanuary 2012 /15 Summary and prospects 15  We saw that the Fluorescence emission was validated (GAP )  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   Applications to the Telescopes HEAT + Coihueco  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

3 rd IDPASC School João EspadanalJanuary 2012 /1516 Thank You

3 rd IDPASC School João EspadanalJanuary 2012 /15 Pierre Auger Observatory 17 The Pierre Auger Observatory (PAO) was completed in May 2008 (3000km 2, 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  Pierre Auger Observatory Malargue, Argentina 1. Cosmic Rays and The Pierre Auger Observatory

3 rd IDPASC School João EspadanalJanuary 2012 /15 Fluorescence Detectors  PMT Pixels 18 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  Fluorescence Detector (FD) FD building design FD Telescope design FD Camera representation 1. Cosmic Rays and The Pierre Auger Observatory

3 rd IDPASC School João EspadanalJanuary 2012 /15 BinTheSky: Information for Cherenkov emission  Information for Cherenkov (in generator to be used in Auger Framework): Electron Length distribution NElectron angle distribution x sh y sh Electron Length distribution N Electron angle distribution bin = 1º l – length travel by electron in bin D Simulation Method

3 rd IDPASC School João EspadanalJanuary 2012 /1520 Final distribution of electrons

3 rd IDPASC School João EspadanalJanuary 2012 /15 The 3D validation procedure 21 Select data Events Generate those events in CORSIKA 3D Simulation in offline (using the BinTheSky information) + Offline Reconstruction 3D Simulation in offline (using the BinTheSky information) + Offline Reconstruction KG Simulation in offline + Offline Reconstruction KG Simulation in offline + Offline Reconstruction CompareCompare With BinTheSky Framework  Fluorescence emission is validated (GAP )  Cherenkov emission On progress

3 rd IDPASC School João EspadanalJanuary 2012 /15 Fluorescence Validation 22 3D simulation of EAS for the FD: validation with a Fluorescence rich data sample (internal note GAP ) Energy distribution Xmax distribution dE/dX Sum of the events 4. Fluorescence and Cherenkov Results  Standard Simulation  3D Simulation  Data

3 rd IDPASC School João EspadanalJanuary 2012 /15 Cherenkov Validation 23 in Progress Energy distribution Xmax distribution dE/dX Sum of the events 4. Fluorescence and Cherenkov Results Preliminary  Standard Simulation  3D Simulation  Data

3 rd IDPASC School João EspadanalJanuary 2012 /15 SDiD:  SDiD: Data 3D KG

3 rd IDPASC School João EspadanalJanuary 2012 /15 SDiD: Data 3D KG  SDiD:

3 rd IDPASC School João EspadanalJanuary 2012 /15 SDiD: Data 3D KG

3 rd IDPASC School João EspadanalJanuary 2012 /15 SDiD: Data 3D KG

3 rd IDPASC School João EspadanalJanuary 2012 /15 SDiD: Data3D KG

3 rd IDPASC School João EspadanalJanuary 2012 /15 A few Results 29  SDiD: Data 3D KG

3 rd IDPASC School João EspadanalJanuary 2012 /15 SDiD: SDiD: Data 3D KG  SDiD:

3 rd IDPASC School João EspadanalJanuary 2012 /15 SDiD: SDiD: Data3D KG

3 rd IDPASC School João EspadanalJanuary 2012 /15 SDiD: SDiD: Data3D KG