R&D for Radio Detection Ad M. van den Berg
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Transcript of R&D for Radio Detection Ad M. van den Berg
8-Jan-2008 ASPERA R&D Lisbon AMvdB 1
R&D for Radio DetectionAd M. van den Berg
R&D and Astroparticle Physics meeting
8 January 2008
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OutlineOutlineOutlineOutline
• Introduction• Cosmic Rays in Air• Cosmic Rays in Dielectric Solids• R&D next years
To make further progress, particularly in the field of cosmic rays,it will be necessary to apply all our resources and apparatus simultaneously and side-by-side
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Physics MotivationPhysics MotivationPhysics MotivationPhysics Motivation
• Sources of UHE cosmic events
• Energy spectra of selected (point) sources
• Multi-messenger detection (cosmic rays, high-energy photons, neutrinos)
• Interactions of UHE particles with nuclei (HEP)
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IntroductionIntroductionIntroductionIntroduction
• Radio detection of UHE cosmic events goes back to the 1960’s– Askaryan (Cherenkov radiation)
• dielectric solids: rock salt, ice, lunar regolith– Allan, Jelley, Kahn, and Lerge (geo-synchrotron radiation)
• atmosphere of the Earth
• Coherent at frequencies where the shower thickness is comparable to the wavelength of the emitted radiation– solids 10 cm -» GHz– air 10 m -» 10 MHz
• Signal amplitude ≈ E2
• Large penetration depth of EM radiation• “Simple” detection technique
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Other TechniquesOther TechniquesOther TechniquesOther Techniques
• Bremsstrahlung– molecular Bremsstrahlung;
will be tested at Pierre Auger Observatory: AMBER
• Active and Passive Radar– knowledge on lifetime of
free electron required at a height of many 10’s of km; tested at various places (USA, Europe)
Terra Incognita; efforts should continue along these lines
Sch
arf
, R
WTH
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Large volumes (~10Large volumes (~1099 kg sr) kg sr)Large volumes (~10Large volumes (~1099 kg sr) kg sr)
• EeV CR ~ 100/(km2 yr 2 sr)– Auger Observatory with z < 60o
– S 3,000 km2 & E > 1 EeV: 105 / yr– N 10,000 km2 & E > 10 EeV: 6x103 / yr
• EeV GZK < 300/(km2 yr 2 sr)– Interaction probability ~ 0.2% / km– KM3NeT / Ice3: 1 km3 water; < 90o
– 0.5 / yr
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Present StatusPresent StatusPresent StatusPresent Status
• Air-shower observations are becoming “standard”; coincidences with EAS arrays !!– data: energy, pointing, horizontal showers; understanding:
absolute normalization, signal shapes, dependence on composition, polarization
– application to a large scale: design studies are being made (pitch between stations, triggering algorithms)
• Dielectric solids have only p.o.p. in the laboratory– data: energy and polarization (SLAC, ANL)– understanding: no correlation (yet) with any cosmic event
simultaneously detected in another detector– application to a large scale: design studies have been made,
new target sites being investigated
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air - CODALEMA (F)- LOFAR (NL,D,UK) - LOPES and LOPES* (D) - Pierre Auger (Argentina)- IceCube (Antarctica)
moon- GMRT (India)- LORD (in orbit)- LRX (on surface)- NuMoon (NL,D,UK)
ice and salt- Anita (Antarctica)- Arianna (Antarctica)- FORTE (Greenland) - RICE (Antarctica)- Salsa (USA)
Different “Targets”Different “Targets”Different “Targets”Different “Targets”
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Radio with Air as TargetRadio with Air as TargetRadio with Air as TargetRadio with Air as Target
DirectionalOmnidirectional
24/7, statistics !!
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Radio with Air as Target Radio with Air as Target Radio with Air as Target Radio with Air as Target
• Existing arrays– CODALEMA, LOPES, LOFAR
• Upcoming arrays– IceCube, Pierre Auger
• Strategy is to develop solitary systems with intelligence at the front end to remove background noise (RFI) predominantly from transients
• Keywords:– theory & simulations (signal development, LDF)– engineering (power, wireless, self-triggering, calibration)– physics (pointing, composition, efficiency)
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Radio R&D @ AugerRadio R&D @ AugerRadio R&D @ AugerRadio R&D @ Auger
• Auger South is perfect radio test bed for EAS (E > 0.1 EeV)– Low RFI levels (compared to
rural areas)– Co-locate about 120 antennas
inside the baseline SD array
– Reduce Eth to .1 EeV using infill tanks (AMIGA)
– Add additional FD telescopes for nearby showers (HEAT)
– Add muon
• Expertise as input to engineer a very large array (many 1000 km2; e.g. Auger North)
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Example of 2 EeV eventExample of 2 EeV eventExample of 2 EeV eventExample of 2 EeV event
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Long-term Behavior (~3 m)Long-term Behavior (~3 m)Long-term Behavior (~3 m)Long-term Behavior (~3 m)
UTC LST
Events recorded with radio @ Auger
SDSD + Plastic ScintillatorsSD + PS + radio
Long-term behavior of noise
3 antennas separated by 100 m1 event / 2 days
Tim
merm
ans,
RU
2 months
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Event reconstructionEvent reconstructionEvent reconstructionEvent reconstruction
• Beam forming• Radio signals come from the direction as determined from
SD• Our signals are from real Cosmic-Ray events !!
Tim
merm
ans,
RU
NS
EW
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Filtering TechniquesFiltering TechniquesFiltering TechniquesFiltering Techniques
Events recorded with radio @ LOPES*
reduction of RFI using- median filtering techniques- number of zero crossings- ratio width and height- wavelet analysis
Gem
meke
, FZ
K
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Self-triggered EventsSelf-triggered EventsSelf-triggered EventsSelf-triggered Events
Dalli
er,
Su
bate
ch
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Radio with Solids as TargetRadio with Solids as TargetRadio with Solids as TargetRadio with Solids as Target
Westerbork Synthesis Radio Telescope
moon
Alv
are
z N
uñez,
Santi
ago d
e C
om
post
ela
rock salt
ice
$$$$salt mines ?
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Radio with Solids as Target Radio with Solids as Target Radio with Solids as Target Radio with Solids as Target
• Existing experiments– ANITA, (FORTE & GLUE), GMRT, NuMoon/WSRT, (RICE)
• Upcoming infrastructures– ARIANNA, LORD, NuMoon/LOFAR/SKA, SalSA
• Strategy is to use existing infrastructures (WSRT, GMRT, LOFAR); to use & develop dedicated systems (Anita, LORD, Salsa)
• Keywords:– theory & simulations (signal development and attenuation)– engineering (self-triggering, calibration, space)– physics (efficiency, neutrino versus cosmic ray)
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Dielectric MaterialsDielectric MaterialsDielectric MaterialsDielectric Materials
MaterialIceIce
Rock SaltRock SaltLunarLunar
RegolithRegolith
Density (g/cm3) 0.92 2.2 1.8
Radiation Length (cm) 39 10 13
Cherenkov Angle (o) 56 66 55
Attenuation Length (m)at 250 MHz
1000 250 ? 10
Experiment (done, running, proposed)
RICEANITA
ARIANNA
SalSA GLUEFORTE
NuMoonLORD
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ResultsResultsResultsResults
em shower in sandSalt
zberg
, U
CLA ANITA
@ SLAC
power (a.u.)
4 hrs WSRT dataPRELIMINARY
Sch
olt
en,
Univ
ers
ity o
f G
ronin
gen
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Salt DepositsSalt DepositsSalt DepositsSalt Deposits
Mt/y
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Exclusion LimitsExclusion LimitsExclusion LimitsExclusion Limits
• AGN PR M(B)
• GZK ESS PJ KKSS
• TD PS
• GRB WB
Kra
vch
en
ko,
MIT
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Exclusion LimitsExclusion LimitsExclusion LimitsExclusion Limits
SalSA 1 km3 365 d LORD h = 250 km365 d WSRT
20 d
LOFAR 30 d
SKA LFB 365 d
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R&D effortsR&D effortsR&D effortsR&D efforts
• Radio from Air
• Radio from Solids
• Other R&D
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R&D for Radio from AirR&D for Radio from AirR&D for Radio from AirR&D for Radio from Air
• Comparison between theory and data– efficiency and pitch for antenna grid– resolution for energy, arrival direction, and composition – optimization of simulations
• Development of low-power (5 W), radio-quiet solitary stations– optimization of electronics (system integration)– band width and sampling rate– cost engineering
• Development of first and second level trigger– hard- and software filtering
• Monitoring procedures– atmosphere, system health
• Deploy engineering array at Southern Site Auger Observatory
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R&D for Radio from SolidsR&D for Radio from SolidsR&D for Radio from SolidsR&D for Radio from Solids
• Further develop theory– separate signals induced by neutrinos and cosmic rays– shower near surface of dielectric material – emission via transition radiation
• Hybrid detection systems– Antarctica (IceCube) or Acoustic + Radio in salt/ice (ARIANNA)
• Measure attenuation lengths– Ice, salt, regolith (Lunar Radio Astronomy Explorer)
• Develop efficient trigger algorithm for observatories with streaming data (LOFAR, SKA)
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Further R&DFurther R&DFurther R&DFurther R&D
• Continue efforts– development of radar detection of cosmic rays (Eurocosmics?)– explore properties of salt (mines) in Europe
• Laboratory (Frascati?) measurements (together with acoustic?)– high intensity pulsed beams to test
• radio intensity as function of angle wrt Č and frequency
• radar reflection (life time free electron)• pulse shape• yield of molecular Bremsstrahlung as function of frequency
• Connection to other Fields and Industry– radio astronomy– event detection in noisy environment (digital trigger, signal
analysis)– low-power electronics, solitary systems
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SummarySummarySummarySummary
• Radio detection of cosmic rays and neutrinos– complementary technique– contained event (energy determination)
• Last 5 years progress has been substantial– air showers: theory and experiment– dielectric solids: proof of principle
• Next 5 years– extension to highest energy and larger scales (many km2)– cross check with other techniques– Europe plays an important role (air showers & lunar regolith)– involve SME’s
• Continued exploring R&D– salt layers, radar detection