cosmic ray measurements with lora - astron · master computer at cs002 300m lofar lora lofar...
TRANSCRIPT
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Cosmic Ray measurements with LORA:LOFAR Radboud Air Shower Array
Satyendra Thoudam(For the LOFAR CR group)
Radboud UniversityNijmegen
M. van den Akker, L. Bähren, A. Corstanje, H. Falcke, W. Frieswijk, J.R. Hörandel, A. Horneffer,C.W. James, J.L. Kelly, R. McFadden, M. Mevius, P. Schellart, O. Scholten, K. Singh, and S. ter Veen
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Outlines
• Introduction: *Detection technique
*Cosmic ray air showers
*Why need LORA?
• LORA details: Experimental set-up
• Results: *Cosmic ray measurements *Simultaneous observation with LOFAR
• Summary
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Cosmic-ray air showers
LORA
LOFAR
⋀ ⋀ ⋀ ⋀ ⋀ ⋀ ⋀
Radioemission
CR
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Operating energy region
Purpose: To support cosmic-ray detection with LOFAR
LOFAR
LORA
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• Primary aim: To complement radio detection of CRs with LOFAR
• 5 stations with 4 detectors each
• At LOFAR stations CS003-007
• Each station is handled by a station computer
• Data processing is done on a central master computer at CS002 300m
LOFAR
LORA
LOFAR Radboud Air Shower Array
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LOFAR Radboud Air Shower ArrayDetectors are plastic scintillators from the KASCADE experiment (Antoni et al. 2003)
Electronics were developed for the HISPARC experiment
e±,µ±
PMT
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LOFAR Radboud Air Shower Array
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Detector calibration
read-out window 10 µsstart 2 µs before trigger12-bit ADC (2.5 ns sampling rate)
Signal produce by a single charged particle Distribution of energy deposition
Fit of Landau distribution to datacalibration: “single-muon“ peak
400 ADC count
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A measured CR air shower
Arrival time Energy depositions
*Arrival time: From the relative time informations between the detectors
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Fitted with NKG function:
Lateral density distribution
A measured CR air shower
Ne=> Shower size (∝Energy)
rM => Moliere radiuss => Age parameterr(X,Y)=> Shower core position
(⊝,⌀)=> Arrival direction
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Results from LORA
• LORA set up completed in May 2011
• Collected over 200,000 cosmic-ray events
• ~40,000 air showers triggered > 7 detectors
• For each air shower, reconstruct the core position (X,Y), arrival direction (⊝,⌀) and the shower size Ne (=> Energy)
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Reconstruction accuracies (from data)using chess-board method (1/2 array vs. 1/2 array)
Core position accuracy Shower size (energy) accuracy
Direction accuracy
< 5m < 25%
< 0.8o
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Results: Average lateral distributions
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Results:
Arrival direction distributions Shower core distributions
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Results: Shower size Ne
Shower size distribution Shower size spectrum
>95% efficiency
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Results: All-particle energy spectrum of cosmic rays with LORA
Preliminary !
Energy=Ne0.93×101.23 GeV (Phd Thesis 2008, KASCADE)
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Simultaneous observations with LOFAR
LORA
*Online processing*Calculate shower parameters*Overall processing time ~ (100+30) ms
*For bright event: Send trigger to LOFAR
CR event
LOFAR
*TBB data stored for 1.3 s
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Simultaneous observations with LOFAR
LORA
*Online processing*Calculate shower parameters*Overall processing time ~ (100+30) ms
*For bright event: Send trigger to LOFAR
CR event
LOFAR
*TBB data stored for 1.3 s
First CR detection with LOFAR !
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Summary of my talk
• LORA performing as expected
• All stations now running
• Started testing LOFAR triggering
• Expecting the 1st CR detection with LOFAR in next few weeks.
• LORA set-up completed in May 2011
• Measured (preliminary) all-particle energy spectrum of cosmic rays
• Started triggering LOFAR
• Led to the 1st detection of CRs with LOFAR in June 2011
Thank you!
We thank the KASCADE collaboration for the detectors. Also, many thanks to Menno Norden, Klaas stuurwold, Jan Nijboer and many others for their support during the LORA installation.