Pierre Auger Observatory for UHE Cosmic Rays Gianni Navarra (INFN-University of Torino) for the...
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Transcript of Pierre Auger Observatory for UHE Cosmic Rays Gianni Navarra (INFN-University of Torino) for the...
Pierre Auger Observatory for UHE Cosmic Rays
Gianni Navarra (INFN-University of Torino)for the Pierre Auger Collaboration
XXXXth Rencontres de MoriondElectroWeak Interactions and Unified TheoriesLa Thuile 5-12th March 2005
•• Science CaseScience Case: the need for Auger: the need for Auger•• Principles and Advantages ofPrinciples and Advantages of aa Hybrid DetectorHybrid Detector•• Present StatusPresent Status of the Observatoryof the Observatory•• First First preliminary preliminary DataData•• PerspectivesPerspectives
Pierre Auger Collaboration
Spokesperson: Alan Watson
16 Countries 50 Institutions~350 Scientists
Italy ArgentinaCzech Republic Australia France BrazilGermany Bolivia* Greece MexicoPoland USASlovenia Vietnam* Spain United Kingdom
*Associate Countries
UHE Cosmic Rays
Eo >1020 eV: 1 part / (km2 century sr) 102 – 103 km2 collecting areas
Surface particle detectors
atmosphericfluorescence detectors
UHE Cosmic Rays
Eo >1020 eV: 1 part / (km2 century sr) 102 – 103 km2 collecting areas
Atmospheric fluorescence detectors
HiRes vs AGASA
AGASA
HiReS
D. Bergmann
~ 30 %Syst. Error
Atmospheric fluorescence detectors
Surface particle detectors
GZK?
pair production energy loss
pion production energy loss
pion production rate
eV1044
2 192
th
mmm
E N
Cosmic ray sources are close by (<100 Mpc)
1021 eV
3 Gpc
B = 1 nG
B intergalactic
-
~ degree Sources !!!
Astrophysics?
Relic Particles in Galactic Halo ?
Mrelic = 1022 eV; SUSY evolution, n-body decay
2
8
16
+ Composition (p,…Fe)+ Astronomy (point sources)
Sakar & Toldrà, Nucl.Phys.B621:495-520,2002Toldrà, astro-ph/0201151
Fundamental
Physics ?
Required to solve EHECR-Puzzle:
• • Better understanding of Syst. ErrorsBetter understanding of Syst. Errors• • Better Resolution in Energy and DirectionBetter Resolution in Energy and Direction
• • Much more StatisticsMuch more Statistics
Hybrid Approach:Hybrid Approach: Independent EAS-observation techniquesIndependent EAS-observation techniques Shower-by-Shower Shower-by-Shower in one Experimentin one Experiment
Much larger ExperimentMuch larger Experiment
Atmospheric fluorescence detectorsAtmospheric fluorescence detectors
UHE Cosmic Rays with Auger
Eo >1020 eV: 1 part / (km2 century sr) 102 – 103 km2 collecting areas
Surface particle detectorsAtmospheric fluorescence detectors
70 km
Southern SitePampa Amarilla; Province of Mendoza3000 km2, 875 g/cm2, 1400 m
Lat.: 35.5° southSurface Array:1600 Water Tanks1.5 km spacing3000 km2
Surface Array:1600 Water Tanks1.5 km spacing3000 km2
Fluorescence Detectors:4 Sites6 Telescopes per site (180° x 30°)24 Telescopes total
Fluorescence Detectors:4 Sites6 Telescopes per site (180° x 30°)24 Telescopes total
LOMA AMARILLA
Schmidt corrector ring
2
.2 m
opt. Filter(MUG-6)
UV optical filter(also: provide protectionfrom outside dust)
Camera with 440 PMTs (Photonis XP 3062)
Schmidt Telescope using 11 m2 mirrors
Coihueco(fully operational)
Lomo Amarilla(in preparation)
Moradoshanded to Collaboration 1.9.04
Los Leones(fully operational)
Water Tank in the Pampa
Solar PanelElectronics enclosure40 MHz FADC, local triggers, 10 Watts
Communication antenna
GPS antenna
Batterybox
Plastic tank with 12 tons of water
three 9”PMTs
receiving tanks
Tank Preparation and Assembly
Transportation into fieldWater deployment
installation of electronics
Installation Chain
650 Water Tanks (out of 1600)
+ 12 Telescopes
Los Leones
Coihueco
AGASA
> 10 x AGASA
Southern Site as of Febr. 2005
SD Calibration by Single Muon Triggers
Agreement with GEANT4 Simulation up to 10 VEM (Vertical Equivalent Muons).
VEM ~ 100 PE /PMT
Huge Statistics!Systematic error ~5%
VEMPeak
Sum PMT 1
PMT 2 PMT 3
Local EM Shower
SD calibration & monitoringsingle muons
Noise
Base-Temperaturevs Time
Signal-Height vs Time
Signal-Height vs Base-Temp
Single tank response
Huge Statistics!Systematic error ~5%
± 3%
All agreed within 10%for the EA
Alternative techniques for cross checks• Scattered light from laser beam• Calibr. light source flown on balloon
FD Calibration Absolute: End to End Calibration
A Drum device installed at the aperture uniformly illuminates the camera with light from a calibrated source (1/month)
Relative: UV LED + optical fibers (1/night)
N Photons at diaphragm FADC
counts
MirrorCamera Calibrated
light source
Diffusely reflective drumDrum from Drum from outside telescope outside telescope buildingbuilding
Atmospheric Monitoring
Balloon probes (T,p)-profiles
LIDAR at each FD building
Central laser facility (fibre linked to tank)
light attenuation lengthAerosol concentration
steerable LIDAR facilities located at each FD eye
• LIDAR at each eye
• cloud monitors at each eye
• central laser facility
• regular balloon flights
Young & Old Shower‘‘young’ showeryoung’ shower
‘‘old’ showerold’ shower
density falls by factor ~150
… by factor ~4
Vertical vs Horizontal Showers
‘young’ showers • Wide time distribution• Strong curvature• Steep lateral distribution
‘old’ showers• Narrow time distribution• Weak curvature• Flat lateral distribution
Only a neutrino can induce a young horizontal shower !Only a neutrino can induce a young horizontal shower !
~ 0.2 µs
(m)
~11020eV~1020eV
Lateral Distribution Function
~ 14 km
~ 8 km
A Big One: ~1020 eV, ~60°34 tanks
~60°~60°
propagation time of 40 µs
EAS as seen by FD-camerasEAS as seen by FD-cameras
Only pixels with ≥ 40 pe/100 ns are shown(10 MHz FADC ≤ 4 g/cm2; 12 bit resol., 15 bit dynamic range)Pixel-size = 1.5° ; light spot: 0.65° (90%)1019 eV events trigger up to ~ 30 km
Two-Mirror event
EAS as seen by FD-cameras
Energy Reconstruction
Integral ofLongitudinal Shower Profile
Energy
preliminarypreliminary
~ 4.8 Photons / m / electron(~ 0.5 % of dE/dx)
A Stereo Hybrid; ~70°
CoihuecoFluores. Telescope
Los LeonesFluores. Telescope
~8·1019eV
Lateral Distribution Function
~37 km
~24km
~70°~70°global view
…zoom
The Power of Hybrid Observations
y
yx
SD times
FD times
Mono vs Hybrid: uncertainties ofShower core & angle of incidence
Verified by using central laser facility
monohybrid
Mono 26.15 ± 0.55 km
Hybrid 25.96 ± 0.02 km
Some numbers:data taking from Jan. 2004
SD: number of tanks in operation 650fully efficient above ~ 3.1018 eVnumber of events ~ 120,000 reconstructed ( > 3fold, >1018 eV) ~ 16,500at present ~ 600 events/day
FD: number of sites in operation 2SD+FD: number of hybrids 1750
~ 350 “golden”
Two Candidate Sites
UtahColorado
“Standard”3,100 km2
10,000km2
15,000km2
TA(800km2)
Auger North(3,100 km2)
AUGER NORTH
CONCLUSIONS
Auger construction in rapid progress in southAuger construction in rapid progress in south Physics data taking since January 2004Physics data taking since January 2004
Stable operation, excellent performance
Hybrid approach is a great advantage!
Neutrino sensitivity
First physics results by summer 2005First physics results by summer 2005Energy spectrum
Sky map
Auger North proposal in progressAuger North proposal in progress