1. RADIO DETECTION of HIGH-ENERGY COSMIC RAYS
at the PIERRE AUGER OBSERVATORY
Aachen, III Physikalisches Institut A of the University of Aachen (RWTH), M. Erdmann, T. Hebbeker, M. Leuthold, T. Winchen
Bonn, MPI für Radioastronomie, P. Biermann
Catania, INFN Sezione di Catania, R. Fonte
Columbus OH, Department of Physics of the Ohio State University, P. Allison, J. Beatty, C. Morris
Dwingeloo, ASTRON, H. Falcke
Grenoble, LPSC, C. Berat, J. Chauvin, D.H. Koang, D. Lebrun, P. Stassi, A. Stutz, O. Zimmerman
Groningen, KVI, S. Harmsma, O. Scholten, A.M. van den Berg
Karlsruhe, FZK-IK, J. Blümer, A. Haungs, T. Huege, H. Schieler, H.O. Klages, R. Engel
Karlsruhe, FZK-IPE, T. Asch, H. Gemmeke, M. Kleifges, O. Krömer
Karlsruhe, IEKP of the University of Karlsruhe, J. Hörandel
Leeds, University of Leeds, P.D.J. Clark
Lodz, Soltan Institute of Nuclear Studies, Z. Ciota, J. Zabierowski
Nantes, SUBATECH, S. Acounis, D. Ardouin, A. Bellétoille, D. Charrier, R. Dallier, T. Gousset, J. Lamblin,
P. Lautridou, L. Martin, O. Ravel, B. Revenu
Nijmegen, NIKHEF and IMAPP of the University of Nijmegen, J. Coppens, S.J. de Jong,
C.W.J.P. Timmermans
Orsay, IPN, E. Parizot, T. Suomijärvi
Orsay, LAL, A. Cordier, S. Dagoret-Campagne, X. Garrido, D. Monnier-Ragaigne
Paris, APC, S. Collonges, B. Courty, Y. Desplanches, L. Guglielmi, C. Lachaud, G. Tristram
Paris, LPHNE, A. Letessier-Selvon
Siegen, Department of Physics of the University of Siegen, T. Bäcker, I. Fleck
Wuppertal, Department of Physics of the University of Wuppertal, J. Auffenberg, K.-H. Becker, K.-H. Kampert, J. Rautenberg
poster size 90*120 = 35.4 * 47.2
20 pts = 7 mm
28 pts = 10 mm
48 pts = 17 mm
for the Pierre Auger Collaboration
Revival for Radio Detection of Cosmic Rays
CODALEMA (Nançay, FR) [1]
LOPES (Karlsruhe, DE) [2]
R&D topics for Radio Detection required for the southern site of the Pierre Auger Observatory
noise levels (sky, transients, broadcasting signals)
influence of thunderstorms
solitary systems (solar power, wireless comms)
“smart” trigger
“animal” and wind proof
optimal bandwidth (analog and/or digital)
Advantages of Radio Detection
no absorption of the signal
bolometric measurement
signal amplitude proportional to energy
good angular resolution
high duty cycle
Start of an R&D project at the Pierre Auger Observatory
using different systems to determine noise levels (sky, atmospheric, human-induced)
correlate radio events with those from the baseline detectors of the Pierre Auger Observatory
energy (pulse height radio ↔ reconstructed energy from base-line detectors)
arrival direction (timing from different antenna stations ↔ reconstructed angle from base-line detectors)
time (true & random coincidences using GPS time stamps)
extend data from CODALEMA and LOPES to 1400 m a.s.l. and E > 0.3 EeV
test bed for a 20 km2 engineering array at the southern site of the Pierre Auger Observatory
SoT = Signal-over-Threshold
T3 = external trigger from baseline detectors
P = external Pulser
present
system
antenna
type
band width
(MHz)
wireless
total gain
(dB)
trigger
pass filter
DAQ
sampling rate
(MS s-1)
dynamic range
(bits) 1
AFDA [3]
0.1 – 200
yes 35
SoT
0.1 – 90
250 8 2
LPDA
35 – 90
<75
SoT/T3
13 – 85
40 (3 parallel receivers) 10 3
LPDA [4] no 63
41 – 79 80 12 4 41
SoT/P
25 – 75
400 5
IVDA [2]
35 – 80
system 1
Active Fat Dipole (AFDA)
Wireless
Solar Power
system 2
Logarithmic Periodic
Dipole
(LPDA)
Initial Results
Wireless
Solar Power
system 3 & 4
LPDA
suppressed by pass filter and by antenna specifications
dominated by Galactic noise
Cabled
system 5
Inverted
V-shaped
Dipole
(IVDA)
Spectral power density measured near the Balloon Launching Station using an LPDA and an Anritsu MS2711D spectrum analyser. The antenna signal was amplified using a low-noise amplifier [4] followed by an RG213 cable with a length of 160 m.
Raw amplitudes of radio signals for a cosmic ray observed with 3 antennas separated by 100 m. The energy of the cosmic ray was 2 EeV, the zenith angle 60o, the azimuth angle -70o, and the distance between the core and the center of the antennas 300 m.
[1] D. Ardouin et al, Nucl. Instr. and Meth. Phys. Res. A555 (2005) 148
[2] H. Falcke et al, Nature 435 (2005) 313, Int. Cosmic Ray Conf, Mérida, July 3- 11, 2007
[3] D. Charrier, IEEE Int. Symp. on Antennas and Propagation, Hawaii, June 10-15, 2007
[4] H. Gemmeke et al, [LOPES collaboration] Proc. ARENA 2005, Int. Mod. Journ. Phys. A21 Suppl. 242 (2006)
Cabled