nutel, ashra-1, and nta - institute for cosmic ray … › icrr_seminar › seminars12 ›...
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 1
NuTel, Ashra-1, and NTA
November 9, 2012, ICRR Seminar @ Kashiwa
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 2
I. Introduction / Earth-Skimming Method
II. NuTel and Ashra-1
III. Neutrino Telescope Array (NTA)
IV. Conclusion and Discussion
NuTel, Ashra-1, and NTA
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23 + 14 13
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1/26/2010 3George W.S. Hou (NTU) APCosPA School @ NTU
Cosmic Rays and Neutrinos
Cosmic Ray Spectrum
Not Well Understood
CR + X → π± → e±+2νμ+νe
UHECR + γCMB → N + π → GZK ν
~ 0.1 /EeV/year/km2/srGZK νFirm!
~ 1.2 x 103 /PeV/year/km2/sr
AGN ν?
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1/26/2010 4George W.S. Hou (NTU) APCosPA School @ NTU
Window of Opportunity
Conventional νDetector
UHECR νDetector?
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1/26/2010 5George W.S. Hou (NTU) APCosPA School @ NTU
Earth Skimming
νττTelescope
Cross Section~ E1.4
ντ
τ
Earth Skimming + Mountain PenetratingCherenkov vs. fluorescence
Sensitive to ντνe: electron energy mostly absorbed in mountainνμ: no extensive air shower
τ appearanceexperiment!
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3/22/2003 George W.S. Hou @ VHEPA-3
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Acceleration Mechanism
Detection Mechanism
νττTelescope
τ Appearance!
τ Decay: Air Showerns Cherenkov
Cross Section~ E1.4
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What I learned 8/2001▶ Vannucci Visit to NTU
• Earth Center Opaque for E > 1014 eV ν !? • Mountain-Valley ντ Detection Concept
I asked whether he already had funding ...after - checking literature (e.g. Fargion)
- passing it thru NTUHEP PIsI hired Alfred Huang in Fall (start simulations)
(had to convince him ...)
Hawaii Site also came out from Vannucci visit ...from Colloquium 3/2004 @ KIAS
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Hawaii Big Island as Site: happened as gotcha
• Courtesy visit to CosPA-1[Fred Lo]
– Hawaii is known good Astro Site– Stood together in front of Hawaii map– Snap: Big Mountains w/ 40 km sep.
• Mt. Hualalai: M. Alfred HuangGood view of Mauna LoaSituated at dryer west sideMauna Loa provide long base line
~ 90 km wide and 4 km high
from Colloquium 3/2004 @ KIAS
GWS Hou & MA Huang, astro-ph/0204145P Yeh et al., MPLA 19 (2004) 1117 [CosPA 2003 WS]
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1/26/2010 9George W.S. Hou (NTU) APCosPA School @ NTU
Three simulation stages1. Mountain simulation: ντ→τ
ν+N cross-section– inelasticity– energy loss of tau
2. Air shower simulation:τ → Cherenkov photons
– τ decay mode – CORSIKA detailed air shower simulation
vs. fast simulation3. Detector performance simulation
– light propagation + Q.E.– pixelization for triggers – reconstruction
1
2
3
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1/26/2010 10George W.S. Hou (NTU) APCosPA School @ NTU
ντ → τ inside mountain
• SM CC ν+N cross-section• Inelasticity & energy loss calculated by G.L. Lin, J.J. Tseng, T.W. Yeh,
F.F. Lee of NCTU• Range (distance when survival prob = e-1) calculated by M.A. Huang
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1/26/2010 11George W.S. Hou (NTU) APCosPA School @ NTU
Tau flux
• Tau flux:– Fast simulation: single interaction inside target– Full transport eq.: Consider multiple interactions ντ→τ→ ντ→τ ...
• Conversion efficiency:– optimal thickness ~ several times of λτ
– Energy loss decrease conversion efficiency
dE/dxNo dE/dx
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1/26/2010 12George W.S. Hou (NTU) APCosPA School @ NTU
Lateral profile of Cherenkov photonsfor horizontal shower (CORSIKA )
• Similar profile for showers produced by e– and π−
• Cherenkov ring distance ~ (L-Rmax)×Tan θc• Outside ring, photon density ~ exponential decay• Detector can trigger far away from Cherenkov ring
1018 eV
1016 eV
1014 eV
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1/26/2010 13George W.S. Hou (NTU) APCosPA School @ NTU
Photons numbers vs opening angle
Ave. photons vs theta (no att.)
Average photons vs theta
0
1000
2000
3000
4000
5000
0 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18 0.2
0
100
200
300
400
500
600
700
0 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18 0.2
No atten.
Photon density
Opening angle (radian)
1 PeV showerShower core to detector plane30 km awaySerious dropw/ attenuation Atten. = 15km
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1/26/2010 14George W.S. Hou (NTU) APCosPA School @ NTU
The Signal and Background PatternCherenkov: 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 smallCluster-based trigger algorithm
Random Background with NSB flux 1 km away from a 1 PeV e- shower
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1/26/2010 15George W.S. Hou (NTU) APCosPA School @ NTU
Trigger Configuration
• Npe Follows Poisson distribution: Prob(n;μ) = e-μ μn/n!,μ = <Npe> Φ tg A FOV εA εq ,Φ = 200/ns/m2/sr A=1m2 FOV=0.5ox0.5oεA =0.5 εq =0.2 μ =0.039 tg=25ns ; μ=0.076 tg=50nsRange < 0.5 km: Majority of photon arrives within 25 ns
Most photons arrives within 50 ns
H L
H H
H
Hn2n1 n3
n4n5n6n7
n8
• Single Pixel Trigger: One pixel pass energy threshold H
• Duo Trigger: Two neighbouring pixels pass threshold H
• H-L Trigger: Two neighbouring pixels with one passes high threshold Hand the other one passes low threshold L
• Sum Trigger: 1. (3x3) trigger cell2. Central pixel pass high threshold H
Neighbour Npe Sum pass threshold A=n1+n2+…+n8
Night Sky Background:
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1/26/2010 16George W.S. Hou (NTU) APCosPA School @ NTU
Trigger Efficiency for Electron Shower
Sum Trigger giveslargest range1.1 km for εtrig = 90%
Sum 2 trigger similar
Other three triggersSimilar to each other
Conservative estimate: 200 γ needed
90%
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1/26/2010 17George W.S. Hou (NTU) APCosPA School @ NTU
Preliminary Reconstruction• Reconstruction: Minimize χ2 for x,y,θ,φ,
and E– Two Detectors Separated by ~ 100 m
E, x, y, θ, φ
1 2
N1, T1, x1 , y1, θ1, φ1
N2, T2, x2 , y2, θ2, φ2
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1/26/2010 18George W.S. Hou (NTU) APCosPA School @ NTU
Possibility for Reconstruction
– Angular Error within 1°– Energy Error ~ 40%– Reconstruction Efficiency > 90% if triggered
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1/26/2010 19George W.S. Hou (NTU) APCosPA School @ NTU
Sensitivity4.7 ×102Defined as reachable
upper limit of fluxAssume F(En) = F0 En−2
Assume no signal in 2 years of observationFeldman-Cousin methodfor upper limits:
2.44 signal eventsTheo1: ~ 0.5 events/year
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1/26/2010 20George W.S. Hou (NTU) APCosPA School @ NTU
Demands of Optical system
• Smaller image size is better.• Smaller spot size is better. • Wavelength: UV region, because it has more Cherenkov light as 1/λ2.
Aperture~1m2
FOV: 16o horizontally8o vertically
Photo sensor:8 x 8 MAPMTs with512 pixels
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1/26/2010 21George W.S. Hou (NTU) APCosPA School @ NTU
Fresnel lens system not good enough• The spot all isn’t small, ~ 5mm. This is Chromatic issue.
Spot with multi-wavelength is 2~3 times spot with single wavelength.• The main way to lower the chromatic aberration is to use different material. However
there are very few UV transparent material.• Cytop is the best to eliminate dispersion (high Abbe no.), also high T(%)
its spot size ~3mm, but it is expensive and lens will become fatter due to low index.
• To sum up, all spot size are less than the channel size of MAPMTs, it meets the threshold but not good enough. Any possible errors can make spots larger. So we changed to other design.
Cytop PMMA
Refraction index (nd)
1.34 1.49
Abbe’s number
90 55
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1/26/2010 22George W.S. Hou (NTU) APCosPA School @ NTU
Electronics Device of NuTel (schematic)
32events size
distribution board
light collector
light collector
send Interruptevery 16 events
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1/26/2010 23George W.S. Hou (NTU) APCosPA School @ NTU
Schematics of electronics
Trigger
Hamamatsu8x8 MPMT
16-channelspreamplifier
DAQ
PMT Preamp.
32 – channels Data Collection Module in cPCI
10 bit x40 MHzADC
FADC
bufferRAM
Triggerdaisychain
cycleRAM
Signal-sharing plate
2 m cable
HV powersupply
Front-end electronics Inside cPCI (PXI) chassis
16 DCM boards (512 channels) inside one PXI chassisDCM
System (CPU) card
Active cPCI extender for debugging
32-channel Data Collection Module (DCM) in cPCI (PXI) processes signal from 32 channels, with Trigger logic on the module, and memory of 256 ADC clocks. If one event is 8 clocks (200 ns), memory could keep up to 32events.
4 preamp boards and signal-sharing plate connected to one MAPMT
Holes for mechanical purposesin future
16-channels charge sensitive preamplifiertransforms charge into voltage for digitisation bypipelined ADC
“SBS” PCI↔VME adapter
Signal-sharing plate is used for increasing dynamic range of the system in factor of about 10-20 times
Multi-anode PMT (MAPMT) “H7546” of 8x8 pixels iused as photon-sensitive device
Computer-controlled HV power supply “VHQ-202M” in VME is used for MAPMT, 2 channels/module, 1 channel supplies 4 MAPMT (256 pixels)
“SBS” PCI ↔ VME adapter
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1/26/2010 24George W.S. Hou (NTU) APCosPA School @ NTU
Schematics of electronics
Trigger
Hamamatsu8x8 MPMT
16-channelspreamplifier
DAQ
PMT Preamp.
32 – channels Data Collection Module in cPCI
10 bit x40 MHzADC
FADC
bufferRAM
Triggerdaisychain
cycleRAM
Signal-sharing plate
2 m cable
HV powersupply
Front-end electronics Inside cPCI (PXI) chassis
DAQ – in Linux, inside cPCI (PXI) CPU card
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1/26/2010 25George W.S. Hou (NTU) APCosPA School @ NTU
Pre-amp. linearity
• Use attenuation to send decreasing pulses in height.
• Intercept with y axis is 1.025mV.
X10
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1/26/2010 26George W.S. Hou (NTU) APCosPA School @ NTU
Calibration method• Every step taking 96
events. Take peak clock value (usually 5th clock). Calculate every step’s mean and rms.
• Error = rms/ square(N)• Use first order fn (line) to
fit.• intercept with y-axis is
pedestal.
DAC value
Fit result
Fit pedestal
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1/26/2010 27George W.S. Hou (NTU) APCosPA School @ NTU
Single Pulse into Pre-amp
• Output with paw fit, divide by 3 regions. (a) Pre-amp.#37 ch.2(b) fitting function
tau1
tau2
(b)
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1/26/2010 28George W.S. Hou (NTU) APCosPA School @ NTU
tau1 and tau2 over 512 channels
-5% +5%
mean value of tau2=185.9ns
-20% +20%
mean value of tau1=12.26ns
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1/26/2010 29George W.S. Hou (NTU) APCosPA School @ NTU
Event lost rate
-10
0
10
20
30
40
50
0 1000 2000 3000 4000
Trigger rate (Hz)
Los
t R
ate
%
Event lost rate
DAQ Test• Event lost rate =
total lost event / (50000+total lost event)
Event lost Rate
00 0 1 2 2.86.4
24.7
44.7
57.18
65.41
-10
0
10
20
30
40
50
60
70
0 1000 2000 3000 4000 5000 6000
trigger rate (Hz)
lost
rat
e %
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 30
1/2004 up Mauna Loa
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1/26/2010 31George W.S. Hou (NTU) APCosPA School @ NTU
NuTel• NuTel is the first experiment dedicated to earth
skimming for τ appearance• PeV cosmic ντ rate is ~ 0.5 event/year• First set of two telescopes ready • VHECR observation in Taiwan: prototype
deployment in 2009 indicates high light background at Mei-Fong
• But it got cut out in CosPA II in Spring 2004 ...and we could not restore it, after several tries ...so I continued it on a shoestring ...
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1/26/2010 32George W.S. Hou (NTU) APCosPA School @ NTU
Schmidt Mirror System
Aspherical Corrector Lens mainly eliminate spherical aberration.
Curved image surface
D:1.6 m, finally we made 1.8m
D:1.14m
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1/26/2010 33George W.S. Hou (NTU) APCosPA School @ NTU
Measurement of the Aspherical Lens at KEK
An image of a blue laser through the lens is measured on the screen.
Compare with design curve
Result
D:2m
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1/26/2010 34George W.S. Hou (NTU) APCosPA School @ NTU
Foucault test at KEK
RESULT: 1801±2mmDesign value: 1800mm
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1/26/2010 35George W.S. Hou (NTU) APCosPA School @ NTU
Spot size measurement
x
yz
Origin of optical system.
.
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1/26/2010 36George W.S. Hou (NTU) APCosPA School @ NTU
Mountain line of Chi‐Lai
80 ~12KM
F.O.V.
奇萊南峰
F.O.V.
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1/26/2010 37George W.S. Hou (NTU) APCosPA School @ NTU
First NuTel Field Test at Mei-Fong 7/15-7/27
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1/26/2010 38George W.S. Hou (NTU) APCosPA School @ NTU
Set-up of Observational Tent
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1/26/2010 39George W.S. Hou (NTU) APCosPA School @ NTU
Image around the focal plane
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1/26/2010 40George W.S. Hou (NTU) APCosPA School @ NTU
Waiting for sunrise before leaving
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1/26/2010 41George W.S. Hou (NTU) APCosPA School @ NTU
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1/26/2010 42George W.S. Hou (NTU) APCosPA School @ NTU
Calibration of MAPMT
gainWe use purple-UV led to shine on MAPMT in black box.
And we use a photo-diode to check the brightness distribution in MAPMT front window plane.Horizontal
(unit cm)
Vertical(unit cm)
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1/26/2010 43George W.S. Hou (NTU) APCosPA School @ NTU
Calibration of MAPMT
gainWe use purple-UV led to shine on MAPMT in black box.
Left graph shows input charge histogram.
The fitting results shows mean # of photoelectron and gain.
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1/26/2010 44George W.S. Hou (NTU) APCosPA School @ NTU
Noisy environment ?
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1/26/2010 45George W.S. Hou (NTU) APCosPA School @ NTU
NuTel• NuTel is the first experiment dedicated to earth
skimming for τ appearance• PeV cosmic ντ rate is ~ 0.5 event/year• First set of two telescopes ready • VHECR observation in Taiwan: prototype
deployment in 2009 indicates high light background at Mei-Fong
• We learned challenge of mountain operation➙ Tried pair up with CRTNT ... they evolved ...
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1/26/2010 46George W.S. Hou (NTU) APCosPA School @ NTU
NuTel• NuTel is the first experiment dedicated to earth
skimming for τ appearance• PeV cosmic ντ rate is ~ 0.5 event/year• First set of two telescopes ready • VHECR observation in Taiwan: prototype
deployment in 2009 indicates high light background at Mei-Fong
• Pair up with Ashra-1 (M.Sasaki) at ICRR ➙ NTA
• We learned challenge of mountain operation➙ Tried pair up with CRTNT ... they evolved ...
NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 46
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 47
Ashra-1
● Ashra-1 succeeded in demonstrating powerfulness of Earth-Skimming for τ appearance.
[Sasaki’s Presentation @ CosPA 2003-NTU]
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 48
Ashra-1 Light Collector
Total Resolution: ~3 arcmin image in 42 deg FOV
Can Cover Mauna Kea Surface at 35 km Distant
Ashra-1
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 49
PIP & PLI Installation @Mauna Loa
Installation of PLIs20-in Photoelectric Lens Image Intensifier (PLI)
[Y.Asaoka, M.Sasaki NIM, A647:34-38,2011]
Test of PIP
Ashra-1
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 50
Segment Mirror Installation @ Mauna Loa
Mount Seg.Mirrors
Al+Al2O3-coat: Blue = UV -3%
Reflection >85%All Light Collector Optical System on ML Ready
Spot Size RML 0.19mmCorresponds to 0.46 arcmin after adjusting all segments
Ashra-1
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 51
Ashra Observational Site: Mauna Loa
3,300 m a.s.l. 35 km from MK 77% mono. 27% stereo. 2~3 arcmin image
Nice Coverage and Precision as Particle Monitor
Ashra-1
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 52
Advantages of ES Tau Neutrino Detection
Atm-ν & CR BG Free
Image A Fine Tau Shower ➙ Open up Multi-Particle Astronomy
Possible Point ν < 0.1 deg
Ashra-1
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 53
GRB081209A
First Check for PeV-EeV Tau Neutrino from a GRB
Swift GRB Alert during Commissioning
Ashra-1
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 54
Ashra Pipeline Trigger & Readout
Optical 4s
BG 200ns
CR 200ns
Same Fine Image to Multiple Triggers
Multi Messenger Approach with One Detector System
Ashra-1
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 55
Ashra-1 R0000941/E115513 Triggered Real Shower Event vs MC
Real Shower Event
MC
Ashra-1
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 56
Ashra-1 R0000941/E115513 Triggered Real Shower Event vs MC
MC reproduce real event
Real Shower Event MC
Ashra-1
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 57
Observed CR Spectrum
Validation of Sensitivity and Reconstruction
Some Hint for Composition
Ashra-1
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 58
PeV-EeV Tau Neutrino Search Limit
Started Obs03 Runs Approaching to IceCube Area
Even Commisioning 100x Better than Rice
Ashra-1
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 59
GRB Neutrino Search Comparison Complement IceCube:• Methodology• Energy• Self-trigger for Tau Neutrino
1. IceCube, Nature 484 (2012) 351• IC40+IC59 stacked 117+181GRBs• Very strong bias for time window (28s)
around Satellite Triggers to suppresshuge BG
2. Murase et al. ApJ 651 (2006) L5• Nearby Low luminosity (LL) GRB (ex.
GRB 060218/SN 2006aj ) dominate totalneutrino fluxes at Earth
• X or γ Satellites cannot detect
3. Hummer et al. PRL 108 (2012) 231101• Recalculated neutrino flux =>
Ashra Energy Region more important
Plausible: Ashra’s Unbiased Search with BG-free
0.
1.
3.
Ashra-1
0. Auger, PRD 79 (2009) 102001
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 60
Conceptual LayoutCentral Site (Site-0)Peripheral Sites (Site-1, 2, 3)
25 km Triangle Grids
⇒ Huge Target Mass (>100 km3-weq)Huge Atm. Mass (above area >1000 km2)3 Mountains Shield BG
Compound Eyes watching the air from sides and beneath
The air in good weather condition between 3 mountains
Cherenkov & fluorescence images of tau appearance showers
Neutrino Telescope Array (NTA)
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 61
Earth-Skimming τ Shower Imaging Method
Volume > 3,200 km3
Mass > 9.3x1012 ton
Mauna Loa
NTA Site-1 (Ashra-1 ML)
Mauna Kea
Huge Mass!Ice ~ 104 km3
CR BG
Shielding BGDistance suitable forShower development: ~30 km
Fluor. Light
Cherenkov Light
NTASite-0
Ashra-1 really demonstrated this method!(ApJ, 736 (2011) L12)
Neutrino Telescope Array (NTA)
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 62
NTA Light Collector (NTA-LC) mount baseline design (tentative)
Design Review~ 1 yr in NTA collaboration⇒ Technical Proposal
Light Collector (LC)Schmidt Optics with φ1.5m pupilFOV 28〫= focal sphere φ50cm
Detector Unit (DU)4 LCs watching same FOVSuperimposed 4 images
⇒ Effective pupil size = φ3m
⇒ Concept of NTA Light Collector:Ashra-1 x 1.5 scaled-up+same trigger & readout
Neutrino Telescope Array (NTA)
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 63
MC Event Sample (100PeV)
Mauna Loa(Site-1)
Mauna Kea(Site2)
Central (Site0)
Hualalai(Site-3)
Impact PointDecay PointXmax
Central (Site-0): Fluorescence
0.5〫trigger pixel (yellow >5 pe)
Mauna Loa (Site-1): Cherenkov
Neutrino Telescope Array (NTA)
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 64
Acceptance with Water & Muon vs Air & Tau
ANTARES
IceCube
NTA
TA
⇒ ντ Detection in Wide Elevation ~30 deg
Neutrino Telescope Array (NTA)
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 65
GRB Neutrino Search Comparison
NTA Survey Depth: z ~ 0.15 (2 Glyr) for GRBν flux (by Hummer et al.)
Complement IceCube:• Methodology• Energy• Self-trigger for Tau Neutrino
1. IceCube, Nature 484 (2012) 351• IC40+IC59 stacked 117+181GRBs• Very strong bias for time window (28s)
around Satellite Triggers to suppresshuge BG
2. Murase et al. ApJ 651 (2006) L5• Nearby Low luminosity (LL) GRB (ex.
GRB 060218/SN 2006aj ) dominate totalneutrino fluxes at Earth
• X or γ Satellites cannot detect
3. Hummer et al. PRL 108 (2012) 231101• Recalculated neutrino flux =>
Ashra Energy Region more important0. Auger, PRD 79 (2009) 102001
Neutrino Telescope Array (NTA)
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 66
30°
360°
NTA ν Survey Performance FOV Elevation 30°× Azimuth 360°
Duty 10-20% from Ashra-1
For GRBνSurvey Depth z < 0.15 (2 Glyr)
⇔ GW det. KAGRA (0.7 Glyr) x 3
ν pointing accuracy < 0.2°(Cheren. mono)
ハワイ島
Neutrino Telescope Array (NTA)
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 67
Abassi et al., PRD 83 (2011) 092003, H. Johansson Ph.D Thesis (2011)
NTA ντ 3yr(Duty 10%)
Diffuse-ν Sensitivity
Diffuse ν case: Duty 10% × solid angle ratio 0.5 ⇒ competitive w/ IceCube
Neutrino Telescope Array (NTA)
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 68
Conculsion
● Excellent detection sensitivity of Earth-Skimming (ES) τ Shower Imagingmethod in PeV-EeV region to search for ν’s from hadron acceleration inastronomical objects, with good pointing accuracy and negligible BG fromCR and atm-ν’s.
● NuTel and Ashra-1 were developed to detect ντ with the ES method.The optical/electronic systems of NuTel were designed, built and testedat 2100 m on Mei-Fong Mountain in Taiwan, and is ready for physicsobservation. Ashra-1 succeeded in the first search for PeV-EeV ντ fromGRBs with the best instantaneous sensitivity since 2008.
● New collaboration for next-gen. Neutrino Telescope Array (NTA) beginto form. The layout considers three site stations for 25 km-grid triangleand a single site station at the center with full-sky coverage, watchingthe total air mass surrounded by the 3 mountains on Hawaii Island. Thisconfiguration allows tremendous sensitivity ( > 100 Gton weq.) and widesurvey capability with Cherenkov-fluorescence observation for PeV-EeVν’s in essentially background-free conditions.
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 69
Backup
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1/26/2010 70George W.S. Hou (NTU) APCosPA School @ NTU
NuTel at NTU
Gravity center, make rotation easier. Trick of alignment of position & tilt: make incident and reflected light overlapped.
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1/26/2010 71George W.S. Hou (NTU) APCosPA School @ NTU
Kuan-young (3092 m)Lu-Lin Zan Chung (2700 m)
Mei-Fong (2100 m)
Site survey
in summer 2008
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1/26/2010 72George W.S. Hou (NTU) APCosPA School @ NTU
Working in the observational Tent
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1/26/2010 73George W.S. Hou (NTU) APCosPA School @ NTU
Installation of light sensor/readout
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1/26/2010 74George W.S. Hou (NTU) APCosPA School @ NTU
Final adjustment of optics
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1/26/2010 75George W.S. Hou (NTU) APCosPA School @ NTU
Taking shifts for online monitoring
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1/26/2010 76George W.S. Hou (NTU) APCosPA School @ NTU
N.D. filter Transmit rate
By adding N.D. filter in front of window of MAPMT, we can decrease incident photons into MAPMT.
The N.D. filters are reflective type. The transmit rate verse wavelength show as left graphs.
1 N.D. filter
3N.D. filter
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1/26/2010 77George W.S. Hou (NTU) APCosPA School @ NTU
Calibration of MAPMT
gain
We use purple-UV led to shine on MAPMT in black box.
And left picture show the purple led and it shine on grid paper .
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 78
Tau Neutrino Regeneration
ντ τ ντ τ
CC 相互作用ごとに非弾性度分エネルギー損失しながら、レプトン変換を繰り返す⇒ 高いエネルギーの ντ を低いエネルギーの ντ に“変身”させて検出する。⇒ 高いエネルギーの ντ の地球による遮蔽を軽減できる。⇒ 検出視野(俯角)を稼ぐことができる⇒ NTAによる探査範囲が広がる
Regeneration オンRegeneration オフ
Eν=1EeVτ出現時のEτ vs -θelev
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 79
タウシャワー10°吹上げ
シャワー開始は地表面近くVertical
Horizontal
集光器位置を動かす水平シャワーからのチェレンコフ
光は広範囲(~5km)で検出可能
1PeV < Eν < 10PeV ではチェレンコフ光が蛍光より優勢
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 80
タウ伝播長300 m@10PeV
タウ伝播長2 km@100PeV
Tau Propagation Length in Rock (MC study)
地表に現れたτ が
地中を走行した距離のMC平均
(横軸:ντエネルギー)
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NuTel, Ashra-1, and NTA George W.S. Hou (NTU) ICRR Seminar, November 9, 2012 81
Forming International Collaboration
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1/26/2010 82George W.S. Hou (NTU) APCosPA School @ NTU
x
y1 2
3 4
1
2
3 4
Spot size for 0O
RMS diameter: 1.583
0.791435
1.582871.58287
RMS diameter:1.847
RMS diameter:1.382RMS diameter: 1.338
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1/26/2010 83George W.S. Hou (NTU) APCosPA School @ NTU
Θy = 0O,Θx = 10O
Θy=0O ,Θx=-10O
x10
11
9
12
9
10
11y
12
RMS diameter: 1.323RMS diameter: 0.847
RMS diameter: 0.953RMS diameter:1.462
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−θelev
Eν(PeV)
LCCν
(107g/cm2)‐θelev(deg)
1 270 32
10 94 16
100 35 5.9
1000 14 2.3
[M.Sasaki et al., Astropart. Phys. 19 (2003) 37]
地中におけるCC散乱長 (LCCν) に相当する俯角 (‐θelev)
Regeneration ⇒ 低エネルギー化 ⇒ 検出立体角度の拡大
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τシャワーの方向精度(検出方法起源)
• 伝播・反応過程での方向変化
– 素粒子・宇宙線分野で広く用いられ定評あるシミュレーションプログラムにより評価
PeV-EeV領域では、τシャワーはντの方向を覚えている
過程 評価方法 精度@PeV 注釈
ντ荷電相互作用 PYTHIA < 0.3分角 Pt: W質量で制限
τ地中伝播 GEANT4ALLM model < 1分角
輻射プロセス重要
光核反応のみALLMモデルで評価した
τ崩壊 TAUOLA < 1分角 Pt: τ質量で制限
空気シャワー CORSIKA 0.1° AS軸ずれ∝ E‐1/2
Astropart. Phys. in press, arXiv:1202.5656
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• 事象再構成– 到来方向決定精度⇒重要
• 大天頂角宇宙線BG除去
• 超高エネルギーニュートリノ源同定
– Likelihood を用いた再構成精度評価• σ = 0.16°
⇒ Cherenkov モノ観測でも高精度方向決定が可能
ダミーデータ 確率密度分布
(cf.) E>PeV τ シャワーの方向精度良好
10 PeV
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宇宙線BG
• 支配的なバックグラウンド– 大天頂角からの宇宙線シャワー
• 期待されるBG量 (CORISKAにて推定)– Commissioning 観測
• NBG = 1.3x10‐4 (197.1hr) ⇒無視可能
– 本観測 (1LC)• 山際からの距離 0.1° 0.3° 1.0° 3.0°• 期待されるBG頻度 0.082/yr 0.55/yr 4.3/yr 39/yr