PeV Cosmic Neutrinos from the Mountains Ping Yeh ( 葉平 ) National Taiwan University November 15,...
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PeV Cosmic Neutrinos from the Mountains
Ping Yeh (葉平 )National Taiwan University
November 15, 2002 CosPA 2003 @ NTU, Taipei
Today is the 75th Birthday of NTU!
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Ultra-High Energy Cosmic Rays
Origin
D.J. Bird et al., Ap. J. 511, 738astro-ph/9806096
AGASA4% excess
M. Teshima et al.,27th ICRC p337, 2001
Anisotropy
Fly’s EyeP(fluct) < 0.07
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High Energy Cosmic Neutrinos
Production presumably dominated by and e
Hadronic
Transportation & Oscillation: 1:1:1
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Cosmic Rays and Neutrinos
Cosmic Ray Spectrum
Not Well Understood
CR + X e2e
UHECR + CMB N + GZK
~ 0.1 /EeV/year/km2/sr GZK Firm!
~ 1.2 x 103 /PeV/year/km2/sr
AGN ?
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Observing High Energy Cosmic Neutrinos
Principle: convert neutrinos to observablesLow cross section: need large target volumeSignals development: need large detection volumeMostly use H2O as target and detection volume (Bikal, AMANDA, ANTARES, IceCube)
Energy coverage: H2O, air fluorescence, and the “hole”
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Conventional Detectors: Atm/Solar
Shield from CR & Atmospheric ’s: Underground Under Water/IceVery Large Target Volume = Detection Volume
SuperK
solar deficit/ &
SNO
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Conventional High Energy Detectors
Limited by Target Volume: Maximum Energy ~ 1015 eV
Deployment: 2003 - 2009
Existing
Yoshida’s talk
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IceCube: 1 PeV Limit for
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UHECR Detectors
Detect -induced Air ShowersConversion Efficiency in Atmosphere Small
Auger
Fluorescence Energy Threshold High > 1018 eV
Reflected
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Window of Opportunity
Conventional Detector UHECR Detector?
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AGN Jets, CRs and Protons?
?
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Earth Skimming
Telescope
Cross SectionCross Section ~ E~ E1.41.4
Earth Skimming + Mountain PenetratingCherenkov vs. fluorescence
Sensitive to
e: electron energy mostly absorbed in mountain : no extensive air shower
appearanceexperiment!
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Collaboration Italy: IASF, CNR, Palermo
– N. La Barbera, O. Catalano,G. Cusumano, T. Mineo,B. Sacco
France: Paris, France F. Vannucci, S. Bouaissi
USA: Hawaii J.G. Learned
Japan: ICRR M. Sasaki
Taiwan: – NCTS/CosPA3– G.L. Lin, H. Athar, …
NTUHEP/CosPA2PIs: W.S. Hou & Y.B. HsiungHardware Team:
K. Ueno (Faculty)Y.K. Chi (Electronics)Y.S. Velikzhanin (Electronics)M.W.C. Lin (Technician)
Simulation Team:M.Z. Wang (Faculty)P. Yeh (Faculty)H.C. Huang (Postdoc)C.C. Hsu (Ph.D. student)
NUUM.A. Huang (Faculty)
Formed in Spring 2002
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Rates, Rates? Rates!
Figure of merit for the experimentDiffused source vs point source
Flux: different sources, different modelsAcceptance: Maximizing A(E) within the budget constraint is the design goal
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Feasibility
Feasibility study was done in 2002 (Alfred Huang)Assume: aperture = 1 m2, light collection efficiency = 10%, ~ 40 km wide valley, ~ 2 km high mountainConclusion was O(1) events per yearDeemed feasible, more attractive with a small budget, and was funded that wayMore detailed study in 2003, will be shown
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Acceptance
Figure of merit of the telescope designA = integration of detection efficiency in the phase space (x, y, theta, phi)
Detection efficiency depends on aperture & field of viewlight collection efficiencytrigger logic
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Factors for Acceptance
The chain of conversions
to conversion rate: ~ O(10-5) - O(10-4)Expect O(10) /year/km2/sr flux> O(1) km2 sr acceptance desired
decay: ~ 82% branching fraction for showersLight collection (baseline design): 1 m2 aperture, 8o x 16o field of view, ~ 10% efficiencyTrigger: position dependent
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The Signal and Background Pattern
Cherenkov: ns pulse, angular span ~ 1.5 degreesNight Sky Background (mean)
Measured at Lulin observatory: 2.0 x103 ph/ns/m2/srA magnitude 0 star gives 7.6 ph/m2/ns in (290,390) nm
Cosmic Ray background very small
Cluster-based trigger algorithmRandom Background with NSB flux 1 km away from a 1 PeV e- shower
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Trigger Study
Background Rates vs Signal Efficiency1PeV, 30 km, normal incidence
1PeV, 30 km, 10° incidence
H-L Trigger
Single Trigger
H-H Trigger (Dual trigger)
H threshold
Tri
gg
er R
ate
(Hz)
X
Y
Local coincidence necessary
to kill the background!
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Acceptance Determination
Integration of efficiencies in phase space
Three independent methods for cross-checking
Results are consistent with each other!
Method Efficiency Integration Investigator
MIR Range determined fromSimulation
Monte Carlo Alfred
MIME Modelled Curve Monte Carlo Minzu
NISE Detailed Simulation Numerical Ping
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Acceptance Curve
Estimated with an idealistic vertical plane mountain surface
Acceptance starts at E ~ 1 PeV
Gradually levels off near 1 EeV ( decay length = 50 km @ 1 EeV)
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Preliminary Reconstruction
Reconstruction: Minimize 2 for x,y,,,
and E– Two Detectors Separated by a few 100m
E, x, y, ,
1 2
N1, T1
, x1 , y1, 1, 1
N2, T2
, x2 , y2, 2, 2
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Reconstruction Error
Possible to Reconstruct Events
– Angular Error within 1°– Energy Error ~ 40%– Reconstruction Efficiency 30% ~ 70%
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Sensitivity
Sensitivity :
1 event/year/decade
of energy Great Chance to See
from– AGN– TD– GC
Attenuation is an Issue
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Requirements on the Instrument
Find signal on top of background!Rate >= 0.5 events/year
aperture, light collection efficiency, triggerAngular resolution: 0.5 degrees or smallerTiming (ns pulse)Low budget
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Prototype Telescope
Purpose:– Proof of Concept– Measure Background
Telescope– Commercial Fresnel Lens
(NTK-F300, f30cm, size=30cm,
pitch=0.5mm, PMMA UV),
– UV Filter (BG3)
– Hamamatsu 4x4 (H6568) MAPMT
– Readout Electronics: Preamp, Receiver,
Trigger, ADC and DAQ
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Field Test at Lulin Observatory (2900m)
E
玉山(Mt. Jade)
0°3°7°
15°Sirius
3 elevation angles: 3°, 7°, 15°2 conditions: w/o BG3 filter
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Cosmic Rays
CR tracks seen by prototype telescope– System functions
properly Potential Use:
– Monitor System Health– Calibration by CR events
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The Optics
Want to utilize existing mirrors or lensesFirst concept: EUSO-type Fresnel lens
Note that EUSO is years away
Timely readiness and cost!
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The Optics - revised Current direction: ASHRA-type Mirror + correction len
s Photon Sensor: Multi-Anode Photomultiplier Don’t need arc-min resolution: optics is basically read
y NOW
Sasaki’s talk
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The Electronics
Dynamic Range x4
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Schematics of the Electronics
PMT Preamp.
UV filter
Hamamatsu8x8 MPMT
16-channelspreamplifier
DAQ
PMT Preamp.
UV filter
TriggerDetector pair
Start readout
32 – channels DCM(Data Collection Module) in cPCI
10 bit x40 MHzPipelinedADC
16 RAM x 256 x 16 per 8 channels
Mirror
Trigger FPGA
FADC
bufferRAM
ADC controlFPGA (x4)
To/fromAnother DCM
Trigger
cycleRAM
Start readout10 bit x40 MHzPipelinedADC
FADC
bufferRAM DAQ
cycleRAM
To/fromAnother DCM
Signal-sharing plate
Front-end electronics box 8x8 pixels(1 MPMT, 1 SSP, 4 preamplifiers)
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Calibration: Pointing
Crab Nebula as the standard candleCan we see it?
d J / d E = 0.28 * ( E / 1TeV ) -2.6 km-2 s-1 TeV-1
Integrated flux is not small: 0.3 /km2 /sRandom background > 10 times higher in “stary stary nights” Use neutral density filter + tighter trigger
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Acceptance to the Crab Acceptance ~ around O(0.1) km2 sr Rate ~ 6 events/hr Exposure of several nights would be useful
Photon density (1/m2
)
1 TeV gamma
Distance (m) log E (TeV)
Trigger Range (m)
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Site Primary Site: Mt. Hualalai looking at Mauna Loa
– Good weather condition, less background, GC in FOV
– No electricity, no water, no communication Prototype Site: Mauna Loa looking at Mauna Kea
– Infrastructure ready, on-site help from CosPA1!
– No GC observation
Mt. Hualalai
Mauna Kea Mauna Loa
Still looking for
possible sites!
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Schedule
Detector Design
Construct1024 Ch. Prototype
2003 2004 2005
Prototype Operation
Construct Full-size Telescope
Site Survey / Preparation
Installation & Calibration
Full Telescope Operation
Crab’s itinerary dictates October - December
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Conclusion NuTel is the first experiment dedicated to Earth skim
ming / mountaing watching The PeV cosmic rate is a few events/year
The cost is low: O(1) million US dollars to build it The time is short: prototype deployment in 2004 The window of opportunity is good, both in energy an
d time (Hmm… the uncertainty principle?)
Ashra is a natural continuation for NuTel– Site coincides
– Physics complimentary
– Schedule looks promising