Experimental Status of Astroparticle Physics with Radio Antennas

Transcription

1 Forschungszentrum Karlsruhe in der Helmholtzgemeinschaft Experimental Status of Astroparticle Physics with Radio Antennas SALSA GLUE Codalema LOPES RICE ANITA Andreas Haungs December 2006 Bucharest Andreas Haungs 1

2 High Energy Cosmic Rays Radio detection? G.Sigl, astro-ph/ December 2006 Bucharest Andreas Haungs 2

3 Charged Cosmic Rays direct Air shower measurements Radio detection? - The cosmic ray energy spectrum is not fully understood - Above ev primary energy: only air-shower measurements possible More and better experiments needed: new detection techniques? December 2006 Bucharest Andreas Haungs 3

4 Radio Emission from Cosmic Ray Air Shower Charged particles in the geomagnetic field produce radio emission! (Jelley et al. 1965, Allan 1971) coherent emission from electron-positron pairs moving through the geomagnetic field or from charge excess in the shower. December 2006 Bucharest Andreas Haungs 4

5 Emission Mechanism Falcke & Gorham, Astroparticle Physics 19, 2003, 477: Characteristic energy for electrons to disappear through strong ionisation loss is MeV Charge separation in Earth s magnetic field classical electric dipole Gyration of electrons along a small arc emission of synchrotron radiation Electrons are in a shower disk of small thickness (2 m < one wavelength at 100 MHz) coherent emission, beamed into propagation direction Timescales for pulses are relativistically shortened (but with microsecond delay across radial distances) pulse ns December 2006 Bucharest Andreas Haungs 5

6 LOFAR = LOw Frequency ARray Large radio telescope ( MHz) 100s of antennas at an area of > km 2 ; Setup H.Röttgering et al., astro-ph/ , astro-ph/ ) sources and epoch of re-ionisation (via 21cm line at z=5-15) -) formation and evolution of AGN -) transient sources (SNR, GRB, galac. Black Holes, etc.) -) solar physics -) cosmic rays LOPES = LOFAR PROTOTYPE STATION dedicated to the study of radio emission from cosmic ray December 2006 Bucharest Andreas Haungs 6

7 LOPES: goals 30 dipole antennas at KASCADE-Grande justification of radio emission and it s correlation with EAS parameters theory of radio emission and implementation in CORSIKA improvement/optimisation hardware (for application in Auger/LOFAR) December 2006 Bucharest Andreas Haungs 7

8 Theory and Simulations 1. analytical calculation of emission processes 2. Monte Carlo simulations of radio signals with input of parameterized air showers 3. Monte Carlo simulations of radio signals with input of CORSIKA simulated air showers θ = 40 ο θ = 50 ο 40 MHz, ev θ = 60 ο θ = 70 ο ev expectations on frequency spectrum lateral distribution polarization T. Huege & H. Falcke Astrop. Phys. 24 (2005) 116 December 2006 Bucharest Andreas Haungs 8

9 Hardware of LOPES LOPES-Antenna Receiver Module Memory Buffer Clock and Trigger Board short dipole beamwidth (parallel/ perpendicular to dipole) direct sampling with minimal analog parts: amplifier, filter, ADconverter sampling with 80MSPS in the 2nd Nyquist domain of the ADC uses PC133- type memory up to 6.1 s per channel pre- and post-trigger capability generates and distributes clock and accepts and distributes trigger December 2006 Bucharest Andreas Haungs 9

10 First step: 10 antennas at KASCADE 10 antennas at KASCADE array frequency band MHz trigger: >10/16 cluster of KASCADE ( E 0 > ev) 2004: 7 months runtime ~ triggered events (and correlated EAS information) sufficient sample of events for detailed analyses December 2006 Bucharest Andreas Haungs 10

11 KASCADE-Grande = KArlsruhe Shower Core and Array DEtector + Grande Measurements of air showers in the energy range E 0 = 100 TeV - 1 EeV December 2006 Bucharest Andreas Haungs 11

12 KASCADE-Grande: Status and Results Knee by light primary cosmic rays Knee position primary particle dependent Tests of hadronic interaction models Grande extension for detection of heavy knee Radio detection? December 2006 Bucharest Andreas Haungs 12

13 December 2006 Bucharest Andreas Haungs 13

14 LOPES 10 analysis: Proof of principle + + sum beamof raw electric forming data fields energy ev EAS core inside antennas Θ = 25.5 o, Φ = 42.5 o signal is coherent data analyses: EAS analyses KASCADE radio signal analyses sky mapping LOPES collaboration, Nature 425 (2005) 313 December 2006 Bucharest Andreas Haungs 14

15 LOPES 10: analysis of central, distant and inclined events LOPES 10 is triggered by KASCADE: central event But most have also trigger in Grande higher energies, larger statistics and larger distances (lateral extension) December 2006 Bucharest Andreas Haungs 15

16 LOPES 10 Results: energy dependence of radio signal distant events central events Radio signal (electric field) scales with primary energy: ε ν E 0 ~1 Power of electric field scales approximately quadratically with primary energy! Apel et al. LOPES collaboration, Astrop.Phys. 26 (2006) 332 December 2006 Bucharest Andreas Haungs 16

17 LOPES 10 Results: lateral profile and angular dependence of radio signal Radio signal scales with core distance: ε ν exp (-R/R 0 ) (R 0 ~230m) Apel et al. LOPES collaboration, Astrop.Phys. 26 (2006) 332 Radio signal scales with geomagnetic field: ε ν 1 cos α Horneffer et al. LOPES collaboration, 29th ICRC, Pune, 2005 December 2006 Bucharest Andreas Haungs 17

18 LOPES 10 analysis of inclined showers and of events during thunderstorms inclined showers reconstruction of shower by particle detectors difficult -larger lever arm to geomagnetic angle -neutrino sensitivity? Downward electric field during thunderstorms asymmetry in trajectories enhanced radio emission Thunderstorm events control sample Petrovic et al. LOPES collaboration, A&A (2006) in press Buitink et al. LOPES collaboration, A&A (2006) in press December 2006 Bucharest Andreas Haungs 18

19 LOPES 30 Extension 30 antennas at KASCADE-Grande Maximum baseline: ~300 m Absolute Calibration Environmental monitoring Trigger: KASCADE and KASCADE-Grande Polarization measurements December 2006 Bucharest Andreas Haungs 19

20 LOPES STAR : large scale application radio technique has great potential for large scale application: - LOFAR will measure CRs - R&D for use in the Pierre Auger Observatory has started LOPES continues to contribute experience and physics results application in Auger needs a different detector concept: - self-triggered by radio signals only - low power consumption - decentralized array organization LOPES develops LOPES STAR December 2006 Bucharest Andreas Haungs 20

21 LOPES STAR : test setup at Auger flexible setup define setup measure background test trigger system test hardware installation in 2006 close to the Balloon Launching Station additional tank December 2006 Bucharest Andreas Haungs 21

22 Summary LOPES Successful cooperation of Radioastronomy and Astroparticle Physics groups LOPES 10: large sample of radio detected showers detailed analyses: results are in agreement with simulation Proof of Principle LOPES 30 absolute calibrated, higher energies, longer maximum baseline, polarization direct comparison of simulations with measurements Precision measurements for energies up to ev LOPES STAR autonomous system, self-trigger system, test facility for Auger application Optimization for large scale application LOPES will calibrate the radio signal in EAS (all the correlations with cosmic ray parameters) December 2006 Bucharest Andreas Haungs 22

23 LOPES Collaboration ASTRON, Dwingeloo, The Netherlands L. Bähren H. Butcher G. de Bruyn C.M. de Vos H. Falcke G.W. Kant Y. Koopman H.J. Pepping G. Schoonderbeek W. van Capellen S. Wijnholds Department of Astrophysics, Nijmegen The Netherlands S. Buitink A. Horneffer J. Kuijpers S. Lafebre A. Nigl J. Petrovic K. Singh National Institute of Physics and Nuclear Engineering Bucharest,Romania A. Bercuci I.M. Brancus B. Mitrica M. Petcu A. Saftiou O. Sima G. Toma Universität Wuppertal, Germany J. Auffenberg R. Glasstetter K.H. Kampert J. Rauthenberg Universität Siegen, Germany M. Brüggemann P. Buchholz C. Grupen Y. Kolotaev S. Over W. Walkowiak D. Zimmermann Max-Planck-Institut für Radioastronomie, Bonn, Germany P.L. Biermann J.A. Zensus Institut für Kernphysik, Forschungszentrum Karlsruhe, Germany W.D. Apel A.F. Badea K. Bekk J. Blümer H. Bozdog F. Cossavella K. Daumiller P. Doll R. Engel A. Hakenjos A. Haungs D. Heck T. Huege P.G. Isar H.J. Mathes H.J. Mayer C. Meurer J. Milke S. Nehls R. Obenland J. Oehlschläger S. Ostapchenko T. Pierog S. Plewnia H. Rebel M. Roth H. Schieler H. Ulrich J. van Buren A. Weindl J. Wochele Istituto di Fisica dello Spazio Interplanetario, Torino, Italy P.L. Ghia C. Morello G.C. Trinchero Institut für Prozessdatenverarbeitung und Elektronik, FZK, Germany T. Asch H. Gemmeke O. Krömer Soltan Institute for Nuclear Studies, Lodz, Poland P. Luczak A. Risse J. Zabierowski Dipartimento di Fisica Generale dell'universita, Torino, Italy M. Bertaina A. Chiavassa F. di Pierro G. Navarra Institut für Experimentelle Kernphysik Universität Karlsruhe, Germany E. Bettini M. Deutsch A. Hakenjos J.R. Hörandel M. Stümpert December 2006 Bucharest Andreas Haungs 23

24 Competitive experiment: CODALEMA Use existing radio astronomical instrument Circular polarized antennas, effective MHz Recently some scintillators as trigger Particle detectors W N S E Acquisition room Antennas R. Dallier 87 m December 2006 Bucharest Andreas Haungs 24

25 CODALEMA : Results Lateral distribution on single events: nearly exponential fall-off, as expected in geo-synchrotron theory Good absolute calibration of the radio signal but bad air-shower parameters R. Dallier et al. R. Dallier et al. Non-Radio Events December 2006 Bucharest Andreas Haungs 25

26 Another idea: RADAR reflections Small meteors generate dens ionization channel in the atmosphere Reflects radio waves for some seconds Characteristic time signals Does UHE cosmic rays generate similar channels?? Detectable with passive or active RADAR? Large volume Some activities: Experiments: e.g. MARIACHI Theory: e.g. P. Gorham P. Gorham December 2006 Bucharest Andreas Haungs 26

27 UHE neutrino detection P. Gorham Motivation to search neutrinos: Gammas: >30 TeV interaction with IR background Charged particles: Low energies: deflection in magnetic fields High energies: GZK effect with CMB There are particles with E > 3 x ev where do they come from? UHE neutrinos are byproducts of GZK and hadronic acceleration But: needs huge detector volumes December 2006 Bucharest Andreas Haungs 27

28 Advantages of radio technique Strong emission process given in nature by the so-called Askaryan-effect Large attenuation lengths (up to ~km) for radio emission in different dense media like Antarctic ice or salt in salt domes Large detector volumes can be equipped with relatively small detector sampling Different concepts for the detection of highenergetic neutrinos by their radio emission in dense media are available December 2006 Bucharest Andreas Haungs 28

29 Askaryan mechanism G.A. Askaryan Neutrino interacts with detector material and generates an electromagnetic shower The electromagnetic shower has more electrons than positrons Charge enhancement propagates in the medium with v > c med Radio-Cherenkov emission Dominant mechanism in dense media December 2006 Bucharest Andreas Haungs 29

30 Askaryan mechanism Coherent up to GHz frequencies (small, but dense showers) Different geometry and polarization than geomagnetic mechanism GEANT4 simulations J. Alvarez-Muñiz, E. Marqués, R.A. Vázquez, E. Zas December 2006 Bucharest Andreas Haungs 30

31 Askaryan mechanism: proof at accelerators Saltzberg et al. Large bundle of photons in a 3,6 t sand-target (also ice) measures 2 GHz radio emission experimental proof of the Askaryan-effect December 2006 Bucharest Andreas Haungs 31

32 Experiment: AMANDA RICE: 17 receiver and 5 transmission antennas in 200 x 200 x 200 m 3 above AMANDA Frequency-range MHz DAQ since 1999 Limits from 1,5 years data Planned: AURA Radio measurements in ICECUBE Kravchenko et al, Astrop Phys 20(2003)195 D. Besson et al. December 2006 Bucharest Andreas Haungs 32

33 Experiment: ANITA Balloon experiment watching a huge detector volume ( MHz) first test: ANITA Lite 45 day flight planned for end of 2006 December 2006 Bucharest Andreas Haungs 33

34 Accelerator Test of ANITA 2006: original, full experiment tested at SLAC Bundles of ~10 9 GeV electrons Barwick et al, hep-ex/ December 2006 Bucharest Andreas Haungs 34

35 Experiment: FORTE Records Cherenkov emission of particle cascades in ice Large detector volumes Frequency MHz Event examples (not neutrinos, due to length of pulse 10µs) No results, only limits Lehtinen et al, Phys Rev D 69(2004) December 2006 Bucharest Andreas Haungs 35

36 Experiment: GLUE Detection surface P. Gorham et al. Use moon as detector volume for neutrino detection >10 20 ev Frequency 2.2 GHz Radio-attenuation length is only ~10 m at 2,2 GHz Only events which interacts close to the moon surface All together ~123 hours observation time No results, only limits Gorham et al, Phys Rev Let 93(2004) December 2006 Bucharest Andreas Haungs 36

37 Experimental Limits Limits for ANITA lite Limits for GLUE Limits for FORTE Limits for RICE Expected limits for ANITA P. Gorham et al. Gorham et al, Phys Rev Let 93(2004) December 2006 Bucharest Andreas Haungs 37

38 Planned Experiment: ARIANNA Antarctic Ross Ice shelf ANtenna Neutrino Array Ice thickness ~500 meters Enough ice for interactions Thin enough for detecting reflections Salty sea water below ice High Reflectivity Array of antennas atop the Ross Ice Shelf looking down No deep holes Very competitive predicted sensitivity ν Ice shelf Direct Ray Reflected Ray Conolly et al, ARENA workshop 2006, Newcastle, UK December 2006 Bucharest Andreas Haungs 38

39 Planned Experiment: NuMoon Moon observation at MHz with WSRT, later LOFAR At these frequencies attenuation length ~100 m and broader emission pattern larger detector volume than GLUE Detection of extreme high energetic neutrinos (and Cosmic Rays) >10 21 ev GZK induced flux Topol. defects Scholten et al. (NuMoon Collab.) 2006, Astropart. Phys., in press December 2006 Bucharest Andreas Haungs 39

40 Planned Experiment (Concept): SALSA (Saltdome Shower Array) 1 2 Salt domes are extremely transparent for radio waves (as well as Antarctic ice) Factor ~2,4 more dense than ice Simpler environment conditions Easier for installation and operation But: unexpected high drilling costs Antenna array Halite (rock salt) L α (<1GHz) > 500 m w.e. Depth to >10km Diameter: 3-8 km V eff ~ km 3 w.e. No known background >2π steradians possible P. Gorham et al. December 2006 Bucharest Andreas Haungs 40

41 Concept SALSA: Salt Domes D. Saltzberg et al. Qeshm Island, Hormuz strait, Iran, 7km diameter Isacksen salt dome, Elf Ringnes Island, Canada 8 by 5km December 2006 Bucharest Andreas Haungs 41

42 Concept SALSA: Salt Domes In situ measurements (Hockley salt mine, TX, USA) Attenuation length >~250m No bi-refringence observed K noise D. Saltzberg et al. 05 More detailed measurements necessary!! (before full proposal) December 2006 Bucharest Andreas Haungs 42

43 Concept SALSA: Salt Domes A. Connolly et al. 06 Transmitting end Test measurements at salt mines in the US Dipole antennas ( MHz band in air) Antennas in boreholes up to their base Clear signal seen through salt from 100 ft. borehole From 200 ft.,300 ft. signal through salt corrupted Less good and less simple as expected (may depend on mine) Receiving end 150 MHz 50 ns/div 1 mv/div 100 ft. borehole December 2006 Bucharest Andreas Haungs 43

44 Concept SALSA: Test experiment HASRA Hawaii Askaryan in Salt Radio Array target material: kg of synthetic rock salt Rock salt block weight 22.7 kg cm thick layer of lead as additional target mass (12 x 1.2 x 0.8 m) two rows of dipole antennas ( MHz band in air) in boreholes 3 MACRO (liquid scintillator) counters track charged particles and serve as a trigger for antenna readout Radovan et al. ARENA 06 No clear radio signal from salt 2007: relocation: Farther away from RF pollution and Higher altitude for increased cosmic ray flux December 2006 Bucharest Andreas Haungs 44

45 Summary Neutrino Detection By Radio Radio technique allows covering very large detector volumes for the detection of UHE neutrinos Needed statistics in principal reachable in short time Different activities Radio in ice Radio in salt Radio in the moon Presently very active field, but yet no positive detection December 2006 Bucharest Andreas Haungs 45

46 But we will hear it!! December 2006 Bucharest Andreas Haungs 46