Radio detection techniques for cosmic rays
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1 Radio detection techniques for cosmic rays Hartmut Gemmeke on behalf of LOPES Collaboration Motivation What is the physics behind it Learning by simulation Learning by doing LOFAR, LOPES, CODALEMA Future for radio at Auger Super-Hybrid Detection Detection of UHCRs of UHECRs
2 Motivation: Advantages of radio detection of UHECRs Assuming UHECRs emit radio signals f = MHz Antennas are cheap detectors, easy to deploy Duty cycle 24 hours/day Practical no attenuation in air Bolometric measurement (integral of EM-signal over shower evolution) Also useable for neutrino induced showers What is the physics behind it? Hartmut Gemmeke, Hanoi06 2
3 Cerenkov emission for neutrinos or UHECR induced showers in ice, salt, lunar regolith, sand Reason: e - charge excess in ν or CR induced shower Proof of effect in sand: D. Saltzberg et al. at SLAC, 2005 arxiv:hep-ex/ No theoretical prediction in air Growing number of experiments plan to use this effect: RICE, GLUE, ANITA, SalSA, LOFAR, Westerbork (E > ev) Forschungszentrum Karlsruhe Askaryan-effect Soviet Phys. JETP 14(1962) Hartmut Gemmeke, Hanoi06 3
4 Geosynchrotron effect of Cosmic rays in air H.R. Allan started R&D on radio-emission of UHECRs e - and e + accelerated on a circle by magnetic field of the earth synchrotron radiation in forward direction 1965 Allan Hartmut Gemmeke, Hanoi06 4
5 Simulation of Radio Emission from Cosmic Rays coherent geo-synchrotron emission history of simulation 2003: analytical calculations Revisited by Falcke&Gorham Astropart.Phys. 19(2003)477 coherent geosynchrotron emission 2005: Monte Carlo simulations based on parameterized air showers 2006: full Monte Carlo simulations based on CORSIKA by histogramming (Tim Huege FZK-IK) Hartmut Gemmeke, Hanoi06 5
6 Simulation: Scaling with E pp (vertical shower) Nearly linear scaling E EW E pp -> E EW E pp 2 coherent effect Radio is bolometric: atmosphere for h < 8 km transparent Flattening with increasing distance T.Huege, Thesis Hartmut Gemmeke, Hanoi06 6
7 Simulation: lateral profiles f = 10 MHz E =10 17 ev flattening with increasing zenith angle approx. exponential scaling R 0 = m Inclined showers can be seen at large distances Huege & Falcke (2005) Hartmut Gemmeke, Hanoi06 7
8 Comparison of parametrized and histogramming MC arrival times: spectra get somewhat flatter spectra steeper at higher distances low frequencies better for large grid spacings Effect of complete Monte Carlo simulation T. Huege, to be published (vertical shower, ev) Hartmut Gemmeke, Hanoi06 8
9 Experiments: LOw Frequency ARray LOFAR ~10,000 antennas grouped in ~100 stations with 100 antennas (10-90 MHz and MHz) each remote stations out to 2-3 hundred kilometers connected by high-speed internet applications: Cosmology, bursting universe, Cosmic Rays & Neutrinos above ev 1 st station operational 2006/7 See talk of S. Lafebre in PS Netherland-German Collaboration LOPES = LOFAR PrototypE Station at Karlsruhe Hartmut Gemmeke, Hanoi06 9
10 Test bed for LOPES is KASCADE-Grande KASCADE KASCADE + red dots KASCADE Grande Hartmut Gemmeke, Hanoi06 10
11 Field strength [µv/m/mhz] Field strength [µv/m/mhz] time t [µs] Forschungszentrum Karlsruhe RFI Filtering LOPES frequency domain frequency MHz] A.Horneffer 2006, Thesis t [µs] after filtering Hartmut Gemmeke, Hanoi06 11 CalPower [Watt/Bin] Unfiltered data Fourier transformation and filter Filtered data Correlation appears
12 KASCADE-Grande Triggered Pulse Detection Electric field for each dipole after correcting for instrumental and geometric delays. Block-averaged, radio emission as a function of time after beam-forming (Correlation analysis) Nature 2005 A.Horneffer 2006, Thesis Hartmut Gemmeke, Hanoi06 12
13 Calibration of CR Radio Signal with LOPES Dependence on geomagnetic angle UHECR particle energy B-field 1. Proof of geo-synchrotron effect 2. Threshold at Karlsruhe 6*10 16 ev Nature 435, 313 (2005) 3. Radio signal is a good scale for energy A.Horneffer 2006, Thesis 4. Emission is coherent: m Hartmut Gemmeke, Hanoi06 13
14 KASCADE Grande Events: Radial Distribution Radio signal scales with core distance: ε ν exp (-R) Apel et al. LOPES collaboration Astrop.Phys. (2006) submitted Hartmut Gemmeke, Hanoi06 14
15 X-cor [V/m/MHz] Forschungszentrum Karlsruhe Reconstruction of KASCADE-Grande events without LOPES Grande only: AZ = ZE = 41.6 XC = m YC = 40.3 m Radio signal = 0.8 Correlation Gauss-fit Red points t [µs] X-cor [V/m/MHz] Grande + LOPES: AZ = ZE = 41.0 XC = m YC = 30.3 m Radio signal = 2.8!!! t [µs] with LOPES Optimized correlation Improvement in precision of direction and core position!? Hartmut Gemmeke, Hanoi06 15
16 Influence of thunderstorm on radio signals For E > 10 kv/m force by E-field dominates B-field: Fair weather: E 100 V/m Thunderstorms: E 100 kv/m Select thunderstorm periods from meteorological data: Clear radio excess during thunder storms B-field effect dominates under normal conditions > 90% duty cycle possible (KA) Thunderstorm events control sample Buitink et al. (LOPES coll.) 2005 & 2006 in prep Hartmut Gemmeke, Hanoi06 16
17 CODALEMA PM under copper housing Plastic scintillator Particle detectors 1.5 m W N 1.5 m Acquisitio n room Antennas S 87 m E per event lateral profiles fit well with exponential R 0 ~ 100 to 300 m Works and measures real UHECR - but has not a KASCADE-experiment nearby Dallier: Arena2005, Zeuthen Hartmut Gemmeke, Hanoi06 Ardouin et al., astro-ph/
18 Forschungszentrum Karlsruhe Future of Radio? Considered antennas - V-dipole or Tri-pole (LOFAR) - dipole (CODALEMA) - Logarithmic periodic dipole antenna (LOPES*) Hartmut Gemmeke, Hanoi06 18
19 Analog RF Front End ± 0.4 V 20 db NF 1.8dB RG m LNA Supply 40 MHz 8th order 80 MHz 8th order 40 MHz 8th 80 MHz 8th ± 0.4 V 20 db order order 20 db Rectifier radio frequency 1 Vpp 50 Ω BIAS-T 3.3V (22mW/Channel) 50 Ω BIAS-T CH V, 65 mw/channel - envelope Crossed LPDA ADCs 10ns Pulse band-pass filter Simple envelope trigger (quadratic sum of both polarizations) RF-bandpass pulse response Full-wave rectifier fast, only few ripples Hartmut Gemmeke, Hanoi06 19
20 Why driving the trigger with rectified RF? The rectifier is a squaring device: r ( t) = s( t) $ s( t) # R( j! ) = S( j! )" S( j! ) s(t) ( ) 2 r(t) multiplication (time domain) Convolution (frequency domain) CW Carrier Carrier with Modulation Puls spectrum Rectifier output: f f f r e c t. r e c t. r e c t. f f DC Signal Man made RFI turns into DC or low frequency and may be separated from pulse spectrum by high-pass filtering f DC Signal + low frequency wideband triangular spectrum Hartmut Gemmeke, Hanoi06 20
21 Baseband spectrum at rectifier output Man made RFI shifted to DC and low frequency range Hartmut Gemmeke, Hanoi06 21
22 N t NS S h Forschungszentrum Karlsruhe Self trigger: Coincidence of min. 3 antennas a t ES E Pulses from the horizon (interference sources) have a delay of: ΔT h / c problems: if source of interference is inside or near to the triangle!! for curvature of pancake -> we need > 3 antennas Pulses with higher elevation θ Zenith < 80 (e.g. from air showers) reach the antennas more simultaneously: 0 < ΔT < h/c Δθ-sensitivity θ zenith = 60 θ zenith = 90 θ zenith = 30 human made Interference from the horizon scale for a=65m pointing information in plane wave appr Hartmut Gemmeke, Hanoi06 22
23 Forschungszentrum Karlsruhe KASC ADE radiodetector LOPES* in FZK ready + triangle at IPE site, 250 m Hartmut Gemmeke, Hanoi06 23
24 /07: tests antenna performance (4 types), noise immunity, trigger, coincidences with surface detector of Auger : review : if review positive Forschungszentrum Karlsruhe Radio test at Auger-South build an engineering array on 10 km : review and decide on an add-up to Auger South & North test station at balloon launching station of Auger possible geometry in cells of 7 antennas 1.5 km Hartmut Gemmeke, Hanoi06 24
25 Conclusions 1. Angular Resolution: discovery of point sources with Radio: Δθ < 1 with more antennas a resolution of 0.2 seems feasible 2. Bolometric Measurement of Energy correlated with geomagnetic angle 3. Emission is coherent 4. Thunderstorms have an effect, but can be discriminated complementary information to Fluorescence and Surface detectors Polarization, Composition?: working on it Installation of several antennas in Argentina 2006 But much has to be done before you can apply it to Auger-North Auger-South is the necessary test-field for the future of radio Hartmut Gemmeke, Hanoi06 25
26 THANKS Radio on the highway to Auger-North? Hartmut Gemmeke, Hanoi06 26
27 LOPES Collaboration W.D. Apel a, T. Asch b, A.F. Badea a, L. Bähren c, K. Bekk a, A. Bercuci d, M. Bertaina e, P.L. Biermann f, J. Blümer a,g, H. Bozdog a, I.M. Brancus d, S. Buitink h, M. Brüggemann i, P. Buchholz i, H. Butcher c, A. Chiavassa e, F. Cossavella g, K. Daumiller a, F. Di Pierro e, P. Doll a, R. Engel a, H. Falcke c,f,h, H. Gemmeke b, P.L. Ghia j, R. Glasstetter k, C. Grupen i, A. Haungs a, D. Heck a, J.R. Hörandel g, A. Horneffer h, T. Huege a, K.H. Kampert k, Y. Kolotaev i, O. Krömer b, J. Kuijpers h, S. Lafebre h, H.J. Mathes a, H.J. Mayer a, C. Meurer a, J. Milke a, B. Mitrica d, C. Morello j, G. Navarra e, S. Nehls a, A. Nigl h, R. Obenland a, J. Oehlschläger a, S. Ostapchenko a, S. Over i, M. Petcu d, J. Petrovic h, T. Pierog a, S. Plewnia a, H. Rebel a, A. Risse l, M. Roth a, H. Schieler a, O. Sima d, K. Singh h, M. Stümpert g, G. Toma d, G.C. Trinchero j, H. Ulrich a, J. van Buren a, W. Walkowiak i, A. Weindl a, J. Wochele a, J. Zabierowski l, J.A. Zensus f, D. Zimmermann i a Institut für Kernphysik, Forschungszentrum Karlsruhe, Karlsruhe, Germany b Institut für Prozessdatenverarbeitung und Elektronik, Forschungszentrum Karlsruhe, Karlsruhe, Germany c ASTRON, 7990AA Dwingeloo, The Netherlands d National Institute of Physics and Nuclear Engineering, 7690 Bucharest, Romania e Dipartimento di Fisica Generale dell Universita, Torino, Italy f Max-Planck-Institut für Radioastronomie, Bonn, Germany g Institut für Experimentelle Kernphysik, Universität Karlsruhe, Karlsruhe, Germany h Dpt. Astrophysics, Radboud University, 6525 ED Nijmegen, The Netherlands i Fachbereich Physik, Universität Siegen, Siegen, Germany j Instituto di Fisica del lo Spazio Interplanetario, INAF, Torino, Italy k Fachbereich C Physik, Universität Wuppertal, Wuppertal, Germany l Soltan Institute for Nuclear Studies, Lodz, Poland Hartmut Gemmeke, Hanoi06 27
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