the t ianshan r adio e xperiment for n eutrino d etection: an autonomous radio-array for air showers...
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The TIANSHAN RADIO EXPERIMENT FOR NEUTRINO DETECTION:
an autonomous radio-array for air showers detection
Olivier Martineau-Huynh IHEP, 17/02/2011
IHEP (Hu HongBo, Gou QuanBu, Zhang Jilong, Zhang Yi & Olivier Martineau-Huynh)IN2P3 (Ardouin, Carloganu, Charrier, Lautridou, Martineau-Huynh, Niess, Ravel) NAOC (Thomas Saugrin, Wu XiangPing, Zhao Meng)
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Radio detection of EAS
Bgeo
e+e-
F = qvBgeo
• Acceleration of relativistic charged particles in the Earth magnetic field (Kahn & Lerche, 1965): geosynchrotron emission
• Coherent effect
detectable radio emission
LOPES: H. Falcke et al., Nature 435 (2005)CODALEMA:D. Ardouin et al., NIM A 555 (2005)D. Ardouin et al., Astro. Phys. 31 (2009)
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Radio detection of EAS• Why radio?–Measurement of direction of origin, energy (?),
nature of primary (??)– Easiness of deployment & cost!
15k€/unit
3 tons
<1k€/unit (?)
<10kg (?)
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Radio detection of EAS
• Only 2 established setups –<30 antennas: low stat– Slave-triggered to standards EAS detectors
Still a long way ahead!!!
Self-triggering?
Amplitude lateral profile?
Energy measurment?
Primary nature determination?
Threshold?
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The TREND site
• Ulastai, Tianshan mountains, XinJiang autonomous province (2650m asl)
Beijing
Urumqi
Ulastai
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The electromagnetic environementVery clean radio
environement above 20MHz.
AM emitters
AM emitters FM emittersTREND
@ Ulastai
CODALEMA@ Nançay
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The 21cm arraya radio-interferometer for the study of the
Epoch of Reionization (Wu XiangPing, NAOC)
EastWest
North
SouthDAQ
4 km
3 km
127 log periodical antennas
x 80 pods
along 2
baselines
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TREND prototype (2009)N
E
S
W
21CMA pods
TREND antenna
First tests on site in June 2008. 6-antennas prototype running in January 2009.
N
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TREND prototype setup
podDAQ room200MSamples/
s ADC+CPU+dis
k
optical fiber
84
dB
50-200MHz filter
21CMA acquisition
optical fiber
64
dB
50-100MHz filter
TREND acquisition
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TREND prototype performances
• Reconstruction performances
N
- static source (a car inside the array)
ΔSN~1.6 m & ΔWE~1.5 m
4-antennas events5-antennas events6-antennas events
spherical wave analysis
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TREND prototype performances
• Reconstruction performances : plane track
4-antennass = 8°
5-antennass = 5°
6-antennass = 2°
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TREND antenna sensitivity
Major radio source: thermal emission from the Galactic plane.
Visible in Ulastai sky between 15h & 23h LST.
Galactic plane @ 408MHz
CRs@21CMATREND antennas clearly exhibit an increased noise level when the Galactic plane is in the sky
Local sideral time
Sig
nal nois
e level
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TREND EAS search
• Discrimination of EAS from RF background
- short/symmetrical/isolated pulses
- in general, longer & repetitive pulses
- random time & direction of arrivals
- in general, localized sources or tracks
- ~plane wave front
- exponential decrease for lateral amplitude profile
- spherical wave front
- 1/distance decrease for lateral amplitude profile
Background signalsCR signals
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Time [mn]
Azi
muth
[d
eg]
TREND EAS searchNoisy periods rejection
• Select quiet periods (<3evts/3mins)• 69% of 6-antennas prototype data (403h)
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TREND EAS search
«Quiet» periods data: 2259 events in 403 hours
Select events with q<65° only.
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TREND EAS search
• 3 additionnal cuts 25 EAS candidates
2.1s excess towards North (20/25 events)
CODALEMA
Bgeo
see Astropart Phys paper:
arXiv:1007.4359
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EAS shower reconstruction
Shower core position & lateral distribution could be reconstructed for 18 candidates. Not totaly reliable as no satysfying amplitude calibration performed so far.
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TREND 2nd phase (2010)
• 15 antennas • 3 scintillators :
ground array for EAS detection cross-check
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Scintillator array• 50cmx50cmx2cm
plastic scintillator + PMT
• PMT signal directly fed into optical transmiter (20-200MHz)
• Independent trigger for all 15+3 detectors
• Scintillator threshold set for ∼25Hz individual trigger rate. time [μs]
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Scintillator data
• 620 3-fold coincidences found in 19 days of scintillators’data.
The 3-scintillators array is a valid EAS
detector
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Radio data
• Selection of ~15 EAS candidates within the 19 live days (applying selection procedure defined with the prototype)
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Hybrid coincidences
• 3 events with 4+ antennas & 3 scintillators in coincidence
• 2 events with 4+ antennas & 2 scintillators in coincidence
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Hybrid coincidences• Random coincidences?
• Triggers on PMT signals?– Trigger delays not consistent with expected
propagation times.– For 4 hybrid coincs (out of 5), some antennas
triggered before the scintillators.
Expected rate for 2 independent events given by:
fA = 1.6 10-4 Hz rate of 3-folds scintillator eventsfB < 10 Hz rate of radio events (multiplicity≥4)Δt = 2 µs
frdm = 2*fA*fB/(fA+fB)*(1-exp(-(fA+fB)Δt)) Hz
frdm = 0.1/year...
No!
No!
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Hybrid coincidences• Independent reconstruction
for 3 hybrid coincs with 3 scints
Radio recons
Scint recons
CoincAΘ= 52±1°
φ =195±1°
Θ= 49±3° φ
=191±4°
CoincBΘ= 61±3°
φ =359±2°
Θ= 67±5° φ =3±4°
CoincCΘ= 42±1°
φ =55°±4°
Θ= 36±3° φ =56°±5°
Coincidence A
First autonomous radio-detection of EAS!(see Astropart Phys paper: arXiv:1007.4359)
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TREND 3rd phase (2011)• 50 antennas (1.1 km²):
largest EAS radio-detection setup
Numerous EAS candidates expected!Lots of analysis work and physics ahead.
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Next steps
• Improve setup:– Faster ADC (500MHz)– Front end digitization– 2nd level trigger– Upgrade optical
transmetters & receivers
– Move to 20-100MHz frequency range (?)
Need for financial support & expertise!
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Next steps• A hybrid detector?– 24 scintillators (?) for full ground array– Energy calibration, shower reconstruction
comparison, lateral profile studies…– Complementary (?) to CODALEMA & AERA– Financial support?
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TREND long term perspectiveHigh energy neutrinos detection through tau production in rock and decay in atmosphere
ntt
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Neutrino detection at TREND
• High mountains:– Additional target for
n– Screen for CR
showers
• Environment: few RFI sources+very little thunder activity
• Radio optimal for inclined showers detection (?)
UlastaiTREND
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Detection cross sections
En = 1016 eVAveraged over f
En = 1018 eVAveraged over f
TREND site topologyFlat site (close showers)
TREND site topologyFlat site (close showers) Upward going Downward going
Upward going Downward going
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Neutrinos flux limit
TRENDAUGER (PRD 2009)
AUGER integrated
AUGER integrated
Waxmann-Bahcall limit
90%CL limitassuming flux f=f0/E2 and no candidate within 4 years (& 0 background
expected)
Results obtained with optimistic
hypothesis. To be confirmed with final antenna design + radio simulation
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Antenna R&D
• Design for optimal sensitivity along horizon? – On-going work– On-site tests foreseen in 2011
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Conclusion
• TREND project running since 2008.• Autonomous radio detection of EAS
established (arxiv:2010.4359).• At present largest setup for EAS
radiodetection. Attractive physics soon to come!
• System upgrading foreseen (electronics+ ground array?)
• Neutrino search late 2012? (new antenna design)
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谢谢 !Thank you !