ta実験の結果と ニュートリノ検出の可能性...gps antenna solar panel 120w stainless...
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TA実験の結果とニュートリノ検出の可能性
��ICRR 多米田裕一郎
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Outline
• Ultra High Energy Cosmic Ray
• Telescope Array Experiment
• TA Result
– Energy Spectrum
– Mass Composition
• Summary
11.3.9 第24回「宇宙ニュートリノ」研究会 2
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Ultra High Energy Cosmic Ray
11.3.9 第24回「宇宙ニュートリノ」研究会 3
HiRes
Auger
PRL.104.161101 (2010)
PRL.104.091101 (2010)
UHECR Mass composition
UHECR Energy spectra
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Telescope Array Experiment
• The largest cosmic ray detector in the northern hemisphere• Hybrid detector for UHECRs
– Western desert in Utah, USA
• Surface detector– 507 plastic scintillation counter (AGASA type)– 1.2 km spacing, 678 km2
– Particle density
• Fluorescence detector– Three FD stations– Northern site was transferred from HiRes-I– Longitudinal development
• FD obs. started : Oct, 2007• SD obs. started : May, 2008
11.3.9 第24回「宇宙ニュートリノ」研究会 4
35km
SD array
FD station
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11.3.9 第24回「宇宙ニュートリノ」研究会 5
Scintillator
3m2 1.2cm 2layers
WLSF
1.0mmφ 2cm spacing
Output
2 PMTs (Electrontubes 9124SA)
Stainless steal box
230x170x10(cm3)
( thickness 1.2mm、1.5 mm厚)
Scintillator
3m2x1.2cmx2layers
WLSF
1.0mmf 2cm spacing
2 PMTs
(Electrontubes 9124SA)
GPS antenna
Solar panel
120W
Stainless box
Wireless LAN antenna
2.4GHz
FADC 12bit 50MHz
GPS
LAN-MODEM
Charge Controller
Battery
Surface Detector
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SD Event example
11.3.9 6
r = 800m
AGASA fitting function
S800 : energy estimator
2008/Jun/25 - 19:45:52.588670 UTC
S800
Lateral distribution
air shower front
第24回「宇宙ニュートリノ」研究会
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Fluorescence detector
11.3.9 第24回「宇宙ニュートリノ」研究会 7
Newly developed fluorescence detectors
Middle Drum site
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Middle Drum
MD transferred from HiRes-I
11.3.9 8第24回「宇宙ニュートリノ」研究会
Transferred from HiRes-I
14 telescopes / st.
5.2m2 mirror
256 PMTs / camera
Sample-and-Hold
electronics: 5.6 μs gate
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Long Ridge
Black Rock Mesa
3.3m
1m
PMT
With BG3
60mm
12 telescopes / FD station
F.O.V. 108o x 30o
Spherical mirror
Curvature radius 6067mm
256PMTs / 1camera
F.O.V
PMT 1.1ox1.0o
Camera 18ox15.6o
Fluorescence Detector (FD)
11.3.9 第24回「宇宙ニュートリノ」研究会 9
HAMAMATSU R9508
Hexagonal bialkali photocathode
Borosilicate glass window
8dynodes
Q.E.:30%(350nm)
Gain:8.0x104(800V)
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TA FD Stereo Event
BRM
LR
Date log(E/eV) Xmax zenith azimuth Xcore Ycore
2008/09/04 19.71 890 g/cm2 44.3o -3.0o -3.1 14.2
Dete
cte
d #
of
P.E
.
11.3.9 10第24回「宇宙ニュートリノ」研究会
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TA Results
• Energy spectrum
– TA MD mono
– TA Hybrid
– TA SD
• Mass Composition
– TA FD Stereo
11.3.9 第24回「宇宙ニュートリノ」研究会 11
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TA MD mono energy spectrum
11.3.9 第24回「宇宙ニュートリノ」研究会 12
• Data: 2007/Dec~2008/Sep
• MC: CORSIKA/QGSJET events
• ~1/2 HiRes
PreliminaryPreliminary
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TA FD & SD Hybrid
11.3.9 第24回「宇宙ニュートリノ」研究会
TA Hybrid analysis
• Using signal arrival timing of FD and SD
• Angular resolution ~ 1.1deg (mono : ~4.7deg)
Using SD aperture
Constant above 1019eV
Data set: BR + LR
May/27/2008 – Sep/28/2009 (~1.5 years)
MC: Shower simulation : COSMOS
SD detector response : GEANT4
i
rcoretcore
Showeraxis
tSD
rSD
FD
Primary energy 1018eV ~ 1020.5eV with E-3.1
Zenith angle cosθ=0.65 (≒50degree) ~ 1
Primary particle Proton
Thinning ratio 10-4 (≤1020eV), 10-5(> 1020eV)
Interaction modelQGSJET II (> 80GeV)DPMJET III (<80GeV)
Cut threshold 100keV
Arrival directionPeak: 0.7 degreeResolution(68%):
1.1 deg
Preliminary Preliminary
13
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11.3.9 第24回「宇宙ニュートリノ」研究会 14
TA-Hybrid: Data MC Comparison
# of selected PMT # of clustered SD ψ
Rp χ2 of geom. fit -Log(L)
PreliminaryPreliminary
PreliminaryPreliminary
Preliminary
Preliminary
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TA-Hybrid : Energy Spectrum
11.3.9 第24回「宇宙ニュートリノ」研究会 15
Preliminary
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SD Analysis
• Good data fits:
– c2/d.o.f.: > 4.0
– Pointing direction resolution: < 5o
– Fractional S800 uncertainty: < 25%
• Good shower geometry:
– Border Cut > 1200m
– Zenith Angle Cut: < 45o
• May/2008 –Feb/2010
• 1.75 years, 6264 events (May/2008 –Feb/2010)11.3.9 16第24回「宇宙ニュートリノ」研究会
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SD Analysis:Energy Determination
• Energy determination table is constructed from the fitting results of the Monte Carlo.
• First estimation of the event energy is done by interpolating between S800 vs. secθisoclines.
secq
log1
0(S
80
0)
11.3.9 17第24回「宇宙ニュートリノ」研究会
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SD Analysis: Data/MC Comparisons
S800 Energy11.3.9 18第24回「宇宙ニュートリノ」研究会
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SD Analysis
1.1˚ Zenith
1.2˚ Azimuthal
11.3.9 19第24回「宇宙ニュートリノ」研究会
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SD Analysis: Energy Scale
• Energy scale is determined experimentally by FD without referring to MC.
• Set SD energy scale to FD energy scale using well-reconstructed events detected by both detectors.
• 27% renormalization.
11.3.9 20第24回「宇宙ニュートリノ」研究会
ESD=1.27EFD
ESD=EFD
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TA Surface Detector Energy Spectrum
11.3.9 21第24回「宇宙ニュートリノ」研究会
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SD Energy Spectrum:GZK Feature
11.3.9 22第24回「宇宙ニュートリノ」研究会
Preliminary
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SD Energy Spectrum:Comparison
● TA
SD
▲ TA MD
■ TA Hybrid
11.3.9 23第24回「宇宙ニュートリノ」研究会
Preliminary
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SD Energy Spectrum:Comparison
● TA
SD
▼ HiRes-II
▲ HiRes-I
11.3.9 24第24回「宇宙ニュートリノ」研究会
TA Preliminary
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SD Energy Spectrum:Comparison
● TA SD
▼ HiRes-II
▲ HiRes-I
●AGASA■ Auger
■ TA
Hybrid■ TA
MD
11.3.9 25第24回「宇宙ニュートリノ」研究会
TA Preliminary
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TA Results
• Energy spectrum
– TA MD mono
– TA FD Hybrid
– TA SD
• Mass Composition
– TA FD Stereo
11.3.9 第24回「宇宙ニュートリノ」研究会 26
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Xmax technique
Depth [g/cm2]
Nu
mb
er o
f ch
arge
d p
arti
cle
Shower longitudinal development
Xmax
• Shower longitudinal development strongly depends on their primary particle type.
• FD observes shower development directly.• Xmas is one of the most efficient parameter for
determining primary particle type.
HiRes
Auger
PRL.104.161101 (2010)
PRL.104.091101 (2010)
11.3.9 27第24回「宇宙ニュートリノ」研究会
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CORSIKA v6.9
• Hadronic interaction modelQGSjet-01, SIBYLL
• Primary : P, Fe
• Energy : log(E) = 18.0 – 20.0
• Zenith angle : 0 – 65 deg
• ~1400m a.s.l (Height of TA Site)
• Thinning factor : 10-4
Ecut: EM100keV, hadron100MeV
Air Shower Monte Carlo
1. Distribution of Energy and Xmax2. Systematic study for TA FD stereo3. Expected Energy vs Xmax observed by TA FD
averaged Xmax
11.3.9 28第24回「宇宙ニュートリノ」研究会
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Detector Monte CarloDetector simulation
• Shower generator : CORSIKA
• Shower cores: within 20km from the center of F.O.V. of each station.
• Actual detector configuration
• Typical atmosphere
Aerosol : typical value observed by LIDAR
scale height : 1.0km, mean free path : 29km
• Fluorescence model: Kakimoto et al., Flash (spectrum)
11.3.9 29第24回「宇宙ニュートリノ」研究会
FD Stereo reconstruction
Determination of shower axis by stereo reconstruction is much better than monocular reconstruction.Opening angle by monocular reconstruction is 〜5deg(1σ ).
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TA-FD Stereo analysis @1019-19.2eV
-0.8 ± 7.9%
-6.2 ± 5%
-11 ± 23 g/cm2
-11 ± 15 g/cm2
ΔE/Esim
ΔE/Esim
ΔXmax
ΔXmax
Proton (QGSJET01)
Iron (QGSJET01)
11.3.9 30第24回「宇宙ニュートリノ」研究会
〜 -4%
- Proton
- Fe
Missing energy correction (QGSJET-II)
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Prediction of Averaged Xmax CORSIKA
11.3.9 31第24回「宇宙ニュートリノ」研究会
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Prediction of Averaged XmaxCORSIKA with Detector MC
11.3.9 32第24回「宇宙ニュートリノ」研究会
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MC/Data Comparison
• Data set: 2007/Nov – 2010/Sep
• FD Stereo events
• Comparison with MC
• Quality Cut
Xmax observed
Zenith < 60o
Core within 19.6km circle
Energy > 1018.0eV
χ2 cut
11.3.9 33第24回「宇宙ニュートリノ」研究会
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MC/Data Comparison (QGSJET01)
Xcore Ycore
Zenith Azimuth
log(#of P.E.)
1018.8-19.0eV (47events)
Likelihood
11.3.9 34第24回「宇宙ニュートリノ」研究会
km km
deg deg
- Iron
- Proton
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Preliminary
Preliminary
Preliminary
Preliminary
Xmax Distribution (QGSJET01)1018.2-18.4eV 1018.4-18.6eV
1018.6-18.8eV 1018.8-19.0eV
11.3.9 35第24回「宇宙ニュートリノ」研究会
Iron
Proton
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PreliminaryPreliminary
Preliminary Preliminary
Xmax Distribution (QGSJET01)
1019.0-19.2eV 1019.2-19.4eV
1019.4-19.6eV 1019.6-19.8eV
11.3.9 36第24回「宇宙ニュートリノ」研究会
Iron
Proton
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Averaged Xmax
Preliminary
11.3.9 37第24回「宇宙ニュートリノ」研究会
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Averaged Xmax
11.3.9 38第24回「宇宙ニュートリノ」研究会
HiRes
Auger
PRL.104.161101 (2010)
PRL.104.091101 (2010)
Preliminary
TA
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Neutrino detection @ TA
11.3.9 第24回「宇宙ニュートリノ」研究会 39
TA results : GZK suppression favor
GZK neutrino : expected to be observed
Neutrino search by FD and SD
Earth-skimming tau neutrinos, etc.
Preliminary
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Conclusion
• TA : the largest detector in the northern hemisphere• FD : 2007/Nov. -• SD : 2008/Mar. -
• Energy spectrumMD mono, TA hybrid, SD : Suppression
• Mass CompositionFD stereo : Consistent with proton composition
• TA Result is consistent with GZK suppressionGZK neutrino is expected to be observed.
11.3.9 40第24回「宇宙ニュートリノ」研究会