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 25 - 75 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