3D simulation Of Extensive Air Showers at Pierre Auger Observatory

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João Espadanal, Patricia Gonçalves, Mário Pimenta

24-01-2013

Santiago de Compostela3rd IDPASC school

Auger LIP Group

3D simulation Of Extensive Air Showers at Pierre Auger Observatory

3rd IDPASC School João Espadanal January 2012 /15

Pierre Auger Observatory: 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?

?

1. Motivation

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Extensive Air Shower

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Air shower Detection:

(dE/dX)max

Hadronic interactions and high energy physics

Shower development

Cosmic Ray Primary Energy

Quasi calorimetric energy measurement

g/cm2 of crossed atmosphere

Xmax

Energy Deposited

Fluorescence Light

How to detect a cosmic ray?

Cherenkov Light

1. Cosmic Rays and The Pierre Auger Observatory


Pierre Auger Observatory

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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 1021 eV events (lab frame)


SD detectors FD detectors(Surface Detectors) (Fluorescence Detectors)



Extensive Air Showers structure2. Extensive Air Showers structure

Cherenkov Light

Fluorescence Light

Light detected is mostly

Fluorescence Light detected dominated by

Cherenkov

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Rayleight Scattering Mie Scattering


Light Detected in the Telescope

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One typical event:

Time signal in one pixel

Fluorescence rich event

Cherenkov rich event

Shower Length in Time

2. Extensive Air Showers structure


Shower in 3 Dimensions

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SDId 3599086Energy = 1.58x1019

Distance to eye= 3.87 km

Shower intrinsic width

Shower in 3D space

Detector effectsAtmospheric effects

Shower Image width

Shower intrinsic width DetectorAtmosphere

2. Extensive Air Showers structure

Light aberration Internal reflections Reflections and detections

efficiencies

Multi ScatteringMulti Scattering


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


BinTheSky Framework Solution (at generator)

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Energy Deposit for fluorescence emission


r : 50 x 20m : 24 x 15 deg z : 300 x 100 m (size: 1000m x 360 deg x 30000 m)

Relatively easy to implement Fluorescence light emission:

Energy Deposit => Isotropic emission

Bins with Cylindrical geometry at generator level

Cherenkov Emission?


BinTheSky: Information for Cherenkov emission

Information for Cherenkov (in generator to be used in Auger Framework):

Electron Length

distribution

NElectron angle distribution

Δ𝜙

𝚫𝝓

𝜶

Electron Length

distribution

N Electron angle distribution

𝚫𝝓 bin = 1º

bin = 1º

direction

l – length travel by electron in bin

𝑁𝑝ℎ = 𝑛𝐸𝑙𝑒𝑐𝑡𝑟𝑜𝑛𝑠 .𝒍𝛂 𝒍𝛟𝒍𝐓𝐨𝐭𝐚𝐥 𝑐𝑘൬1− 1𝑛2൰൬1𝜆2 − 1𝜆1൰

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BinTheSky: In Auger Offline Framework

Propagation time

Emission time

𝜶

𝚫𝝓

1bin in and 𝚫𝝓

𝚫𝝓 bin = 1º

bin = 1º

BinTheSky embodied in the Auger Offline Framework(Auger Simulation and reconstruction software)

for each SkyBin find and bins in FoV. Calculate the solid angle and attenuation for

(, ) bin.

SkyBin

In ShowerSimulatorLX:Produce photons: Fluorescence

emission Cherenkov emission

Propagate Photons to detector using geometrical information :

solid angleemission angledistance to telescope

Attenuate and scatter photonsCherenkov scattered Multiple-scattering

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BinTheSky: Cherenkov Emission tests

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Cherenkov Pool on ground for a shower with θ=63º:Heat Telescope, Field-of-View ( 30o –

60o)

FD Telescope, FoV ( 0o - 30o)


Shower Direction


Fluorescence and Cherenkov Validation

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Energy distribution

Xmax distribution

4. Fluorescence and Cherenkov Results

Energy distribution

Xmax distribution

Preliminary

Preliminary

Standard Simulation3D SimulationData

Fluorescence Emission Cherenkov Emission


Future Analyses on Lateral distributions

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Zeta distance


Preliminary

Preliminary



Summary and prospects

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We saw that the Fluorescence emission was validated (GAP-2012-039)

Cherenkov emission is being tested Firsts longitudinal results compatible with standard SimulationFurther 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 HEATImplement Scattered Cherenkov Full implementation of a

3D Simulation and 3D reconstruction


Thank You



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The Pierre Auger Observatory (PAO) was completed in May 2008 (3000km2, 1600 Cherenkov tanks and 4 FD facilities, ...)

Hybrid techniqueWith this experiment we have better quality

and higher number of cosmic ray events than ever


Malargue, Argentina



Fluorescence Detectors

PMT Pixels

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4 stations with 6 telescopesEach telescope with each with 30º x 28.6º field of

viewCamara with 440 PMT pixels (20 x 22)

Several calibrating systemsLaser system, LIDAR stations, Aerosol monitors,

clouds and stars monitoring~10% duty cycle

Fluorescence Detector (FD)

FD building design

FD Telescope design

FD Camera representation



BinTheSky: Information for Cherenkov emission

Information for Cherenkov (in generator to be used in Auger Framework):

Electron Length

distribution

NElectron angle distribution

Δ𝜙

𝚫𝝓

𝜶𝚫𝝓

𝝓xsh

ysh

Electron Length

distribution

N Electron angle distribution

𝚫𝝓 bin = 1º

bin = 1º

direction

l – length travel by electron in bin

𝑁𝑝ℎ = 𝑛𝐸𝑙𝑒𝑐𝑡𝑟𝑜𝑛𝑠 .𝒍𝛂 𝒍𝛟𝒍𝐓𝐨𝐭𝐚𝐥 𝑐𝑘൬1− 1𝑛2൰൬1𝜆2 − 1𝜆1൰

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Final distribution𝝓 of electrons

Final distribution𝜶 of electrons


The 3D validation procedure

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Select data Events Generate those events in CORSIKA

3D Simulation in offline

(using the BinTheSky information)

+Offline

Reconstruction

KG Simulation in offline

+Offline

Reconstruction

Compare

With BinTheSky Framework

Fluorescence emission is validated (GAP-2012-039)

Cherenkov emissionOn progress


Fluorescence Validation

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3D simulation of EAS for the FD: validation with a Fluorescence rich data sample

(internal note GAP-2012-039)

Energy distribution

Xmax distribution

dE/dX Sum of the events




Cherenkov Validation

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in ProgressEnergy distribution

Xmax distribution

dE/dX Sum of the events


Preliminary

Preliminary

Preliminary



SDiD: 4943331

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SDiD: 4943331

Data

3D

KG


SDiD: 4943331

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Data

3D

KG

SDiD: 4943331


SDiD: 4943331

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Data

3D

KG


SDiD: 4943331

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Data 3D

KG


SDiD: 4943331

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Data

3D

KG


A few Results

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SDiD: 9721432

Data

3D

KG


SDiD: 9721432

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Data

3D

KG

SDiD: 9721432


SDiD: 9721432

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Data

3D

KG


SDiD: 9721432

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Data

3D

KG

3D simulation Of Extensive Air Showers at Pierre Auger Observatory

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