ARENA 2005 DESY-Zeuthen Conference Summary 19 May 2005

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ARENA 2005 DESY-ZeuthenConference Summary19 May
2005

• John Learned
• University of Hawaii

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General Comments

• Heroic times for radio and acoustic, a
  renaissance will grand discoveries follow?
• Adventurous field dangerous for careers perhaps,
  but opportunities, and a great training ground
  for students.
• Build on successes of optical Cherenkov in IMB,
  Kam, SuperK -gt SN1987A muon neutrino
  oscillations.
• Long campaign of Baikal, DUMAND-US, AMANDA,
  NESTOR, ANTARES, and NEMO -gtICECUBE (KM3?) Soon
  to bear fruit.
• We had all better wish ICECUBE great success!
• Amazingly all highest energy Nu limits from radio
  and acoust!!
• Limits easier than discoveries knowing what you
  saw is vital.
• But no UHE discoveries yet, though no Xterr
  nus.. Danger lessons of HE and VHE Gamma Ray
  Astron.
• Seek bread and butter results, ties to particle
  physics, creative funding.
• International cooperation vital and natural.

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Several Random Comments on Historyadding to
earlier remarks here and at RADHEP

• M. A. Markov Frederick Reines great
  stimulators of neutrino physics (and nucleon
  decay.), roles perhaps underappreciated.
• Mistakes often forgotten early acoust
  overestimate, other acoustic mechanisms with
  large output progress is a crooked path. Amusing
  how wrong results can initiate later successes.
• Some positive surprises water and ice
  transparency gtgt thought in 1980s.

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Requirements for UHE Rare Particle Detection

• Need natural targets, natural radiation
  mechanisms, detection at large impact parameter
• Aevent (?transverse)2 (?atten/?)2
• Methods
• Particle Sampling
• Fluorescence/Scintillation
• Optical Cherenkov
• Radio Cherenkov
• Radio Geo-Synchrotron
• Thermo-Acoustic Radiation

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Project Summary

• So many projects and talks at this meeting,
  cannot cover all in short summary. Apologies.
• See many wonderful talks on ARENA web.
• Many starting, a few physics results
• See following table

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Methods Projects for UHE Particle Detection
Medium/ Mechanism Atmos Water, Ocean/Lake Deep Ice Salt Domes Lunar Regolith Bulk Earth/ Moon
Particle Sampling EAS Arrays AUGER IMB, Kam, SK x x ?? CWI, KGF,
Fluor/Scint Flys Eye, HiRes, TA, ASHRA, EUSO x x x? x x
Opt Cherenkov Mt. Hopkins,, HESS, ASHRA, MAGIC, Baikal, DUMAND, NESTOR, ANTARES, NEMO AMANDA, ICECUBE ?? x x
Radio Cherenkov ? x RICE, Forte, ANITA SALSA-R GLUE, Kalyazin, Westerbrk LORD x
Radio Geo-Synch LOPES, CODALEMA AUGER x x x x x
Acoustic Radiation x SADCO, SAUND, ACORNE, NEMO, Baikal ICECUBE-A SALSA-A x (Seismic) ??
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Physics Simulations

• Great progress in all areas (GEANT4 Corsika)
  but much to do for solids both acoustic and
  radio.
• Highest energies still not well handled.
  Computing time. LPM. (Dedenko made nice hybrid).
• Time domain in radio needed.
• Need studies of HEP potential crossections,
  flavor separation, composition.
• Have lab demos for radio, need work on acoust.
• HE Physicists need to learn to deal with analogue
  signals interesting new options in signal
  processing
• (Engineers need to learn about non-CW signals).

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Detector Technology

• Much progress in radio antennas, work ongoing
  still some black magic.
• Ongoing problem due to our special need for
  impulse response devices.
• Piezoelectric technology well developed by
  military oil industry commercial devices
  available. Use it.
• Interesting options with fiber optics (Trono).

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On Site Simulators Calibrators

• Pingers (bulbs) and transmitters (sparkers) easy,
  but shower simulation is not.
• Sadly, no physics benchmark.
• Shower simulators under development for acoust
  (zapper, laser).
• Need ideas for ice/salt radio (accel in hole ?).
• Cross calibrate in radio EAS applications.

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Media Properties

• Need work in all areas
• Radio in ice good, lots of variation in salt
  measurements, but probably OK.
• Acoust well known in water, but ice mostly
  theory.
• More work needed in accounting for variable index
  of refraction, in simulations.

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Radio Atten in Salt- lots of spread
Chiba
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Acoustic absorption in ocean Pure water absorbs
due to its viscosity. In sea water, a pressure
wave shifts chemical equilibrium between a
molecule and ions, taking energy from wave
B(OH)3 B3 3 OH-(relaxation freq. 1
kHz)MgSO4 Mg2 SO42-(relaxation freq.
100 kHz)
water B(OH)3 MgSO4
absorptivity dB/km
water MgSO4
water
Ulrich
Frequency Hz
Price
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Summary of Acoustic predictions for ice and
NaCl ?scatt ?abs
104 Hz 3x104 Hz 104
Hz 3x104 Hz Ice (D0.2 cm) 1650
km 20 km 8-12 km 8-12 km
NaCl (D0.75 cm) 120 km 1.4 km
3x104 km 3300 km 1. Clay, liquid
inclusions, and anhydrite in salt domes dominate
scattering and absorption. 2. Scattering in salt
domes is worse than in South Pole ice because
grain size is larger (geometric rather than
Rayleigh). 3. In ideal salt, absorptivity would
be far lower than in ice in real salt it will be
worsened by heterogeneities. 4. Must measure
?scatt and ?abs in South Pole ice and salt domes
Price
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Predicted depth (temperature)-dependent ice
acoustic absorption at 10 kHz
See P.B. Prices talk absorption
frequency-independent but temperature
(depth)-dependent
In simulation, integrate over absorption from
source to receiver
Vandenbroucke
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Ocean Acoustic Arrays Can Compete
not optimized yet
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Acoustic Detection Needs

• Need acoustic noise levels in ocean versus depth,
  direction.
• Realistic ocean propagation modelling.
• Survey of promising locations in ocean (deep,
  calm, salty, warm surface, possibility to work
  below reciprocal depth).
• Acoustic absorption and scattering in ice and
  salt, measured in situ.
• Study of shear wave production in salt and ice.
• Investigate use of surplus telephone (fiber)
  cables for a mid-ocean array.

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LOPES_at_KASCADE-GrandeHeino Falcke

• KASCADE 250 electron muon scintillator
  detector hutsLOPES10 10 radio antennas KASCADE
  Grande expansion of KASCADE (red dots)

KASCADE
KASCADE Grande
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LOPES Summary ConclusionsHeino Falke

• LOPES works, the geosynchrotron effect is real
• Radio is a faithful tracer of air showers
• Radio gives very good energy information and
  arrival directions.
• Inclined showers Excellent prospects for
  composition studies and neutrino hunting
• Next steps Argentina, Moon

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Westerbork Proposed Experiment next 5 slides from
Jose Bacelar
Use Westerbork radio observatory

• Advantages
• 117-175 MHz band
• 25 m diameter dishes
• 5 degree field of view
• 12-14 coincident receivers
• 100 hour observation time
• 40 M samples/sec (PuMa2)
• Polarization information

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Results of calculations for cosmic rays
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Results of calculations for neutrinos
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Calc. limits GLUE
Published limits Rice,GLUE,FORTE
Predicted limits 45 days ANITA
Theoretical predictions Active galactic
nuclei Astro.Phys.3(96)295 GZK induced
flux Phys.Rev.D64(04)93010 Topological
defects AstroPhys. J. 479(97)547
Calc. limits 100 hours Westerbork
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Strong refraction in firn
Acoustic upward
Radio downward D. Besson
Signals always bend toward minimum propagation
speed, but Sound abhors vacuum c 0 Radio
adores vacuum c 3e8 m/s
Vandenbroucke
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Ice Optical, radio, acoustic independent
effective volumes
Preliminary!
Vandenbroucke
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Conclusion

• Wonderful level of activity in AR detection.
• New ideas, ranging from deep ice and salt, to
  earth and sky.
• Exciting rapid progress in radio EAS
• Much work to do in studying media, technology,
  array design, simulations.
• Some projects close to having crucial results
  (ANITA, ICECUBE, AUGER).
• Many thanks to hosts, and looking forward to next
  meeting.
• Advert (MeV) Geonu meeting in Hawaii 14-16 Dec
  2005.

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ARENA 2006Newcastle UK
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Location
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EHE CR NusAndreas Ringwald DESY

• Insert slides limits and spectrum
• SM Crossection uncertainties x2
• New physics x 100 EgtEeV?
• Strongly interacting nus depth of interaction?
• Necessity of seeing something soon or we are in
  trouble.

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GZK NeutrinosDave Seckel

• Show overall spectrum and limits
• ESS benchmark, but could be 10x lower, or 10x
  higher depending upon evolution, spectrum,

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Compare MethodsJulia Becker

• Show plots energy and depth
• What geomoetric volume for ICECUBE?

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Radio Attenuation in Salt and IceChiba

• L 538 /- 171 m in pure salt, cavity method
  1GHz, 1000/- 640 m at 300 MHz
• Hockley 275/- 234 m peculiar spread,
• 156/-112m at 300MHz??
• Show atten vs freq plot
• Questions of water absorption and polycrystaline
  form

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Acoustic Waves in Ice and SaltBuford Price

• Absorption and scattering both look good for ice
  and salt (10 km scale, but salt 1km?)
• Salt needs dome with small (lt1cm) grains
• Need in situ measurements
• Temperature and pressure dependence?

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Acoustics in SaltEisenblatter and Manthei

• Crack monitoring around cavities 10KHz
• Peak attenuation around 0.28db/10m in German
  repository (500m deep).

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Radio Signals in Test Beams at SLAC Dawn Williams
Ped Miocinovic

• 2000 sand, 2002 salt
• photon beam simulated 1015 1019 eV
• Amplitude and polarization agrees with theory
  over large range.
• Measurements of spectrum, phase and deconvolved
  time domain consistent.

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UHE SimulationsL. G. Dedenko

• Hybrid calculations producing results
• 400 m at 1020 eV due to LPM
• Show cascade length vs energy

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Coherent Radio Emission in Solid MediaJaime
Alvarez-Muniz

• ZHS, GEANT4 agree in various media
• Simple scaling model for various media

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Structure Function of Charge Excess in Rock
SaltY. Watanabe

• Model of EM shower with parameters for both
  longitudinal and lateral densities.
• Uses GEANT4 up to few PeV.

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Radio from CR ShowersHuege Falcke

• Geomagnetic effect predominates
• Scales roughly with energy over large range
• Frequencies lt 50 MHz, dists lt 1km
• Not strong variation with azimuth around track
• Show plots

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EAS Radio Simulations with EGSnrcA. Konstantinov

• See diffraction from Cherenkov
• Cherenkov and Geosynchrotron latter dominates by
  x10
• Cherenkov becomes dominant gt100 MHz

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Radio Signal Pulse ShapesDavid Seckel

• Scaled to universal shapes for long and trans
• Uses gamma functions for shower model
• How to handle flcutuations, phases,

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Acoustic Signal ProcessingSean Danaher

• Nice review of various signal analysis
  techniques. See talk.

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Experience from SAUNDJason Vandenbroucke
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Analysis of ITEP Baikal Acoustic DataD. Zaborov

• Doing reconstruction of possible sources of EAS
  generated pulses
• No correlated events with EAS counters
• Threshold maybe 1021 eV?

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Acoustic Detectors in AntaresC. Neumann

• Developing piezo devices
• Deployed recording device
• Have some noise spectra, but peculiar
• Crazy plan to use sensors on glass housing

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Piezoceramics StudiesK. Salomon

• Calculated and measured characteristics of
  hydrophones
• FE calculations

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Fiber laser hydrophone measurementsC. Trono

• Doped fiber laser gives distributed response
• Many sensors on one string with one pump laser
• Sensitivity to levels of hydrophones

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Hydrophone Calibration with a Proton BeamGiulia
de Bonis

• Using commercial hydrophones (Benthos, ITC, ..)
• 100 MeV beam at ITEP into water tank
• See nice acoustic signal, linearity over x10

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GlaciophonesSebastian Boser

• Made various tests and designs for ice use
• Use ring transmitter

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High Frequency Acoustic Noise in BaikalN. Budnev

• No convincing coincidences between counter array
  and hydrophones, but some peculiar impulsive
  noise
• Some lovely bipolar pulses need further
  exploration

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Acoustic Studies at ITEPV. Lyashuk

• Tests with proton beam, exploring 4 deg point

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Acoustic Signals with Proton and Laser BeamsK.
Graf

• Interesting investigation of temp depend with
  laser and with proton beam
• See peculiar business with zero crossing
  differences between protons and laser.

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SAUND I ResultsJustin Vandenbroucke

• Report of first data paper.

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NEMO Acoustic Test FacilityG. Riccobene

• Running on line from 2km deep test site
• 4 hydrophones operating
• Many recordings of surface noises from dolphins
  and whales, ships

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Acoustic Detection in ValenciaM. Ardid

• Just getting started with lots of acoustical
  expertize not only in neutrino business
• Designing and characterizing hydrophones

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Results from Kalyazin RadiotelescopeRustam
Dagkesamanskiy

• Now have results with 55m telescope and set
  limits similar to GLUE with 60hr of data
• Slightly less stringent limit due to more
  conservative assumptions

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Westerbork Observatory to Observe Lunar NusJ.
Bacelar

• Suggests using 100MHz
• Get penetration to 250m, angle to 75 deg
• 5 orders of mag greater acceptance for CRs, down
  to 1E22 eV
• Neutrinos up by 1E4
• 14 telescopes, 5 deg FOV
• Show slide of spectral response

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RICE StatusDave Besson

• Revised (down) volume (show fig)
• Paper out soon on limits on low scale gravity
  under assumptions of GZK flux (various).
• No coinc for GRBs

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Status of ANITA, MCsPed Miocinovic Amy Connolly

• Fly 2006-7
• Rays reflected from bottom may contribute new
  signals over larger solid angle

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Radio Detection of CRsHeino Falcke

• Running LOPES since Jan 2004 with KASKADE, gt1017
  eV
• Radio flashes correl to lt1 deg with EAS
• Nature paper reporting first clean detections
• Sho figures

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LOPESAndreas Horneffer Andreas Haungs

• 40-80 MHz, 10 -gt 30 antennas
• Corr well with N_mu but not so well N_e

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CODALEMA ResultsRichard Dallier

• 7000 m2, 50 PeV threshold
• 7 log periodic antennas, 24-82 MHz
• Demonstrated stand alone capability with impact
  parameter detection, angles, energy
• Program to import antennas to Auger

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