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Telescope Array Experiment
ICRR N. Sakurai
for TA collaboration
Concepts
Site & equipments
Observation summary
Future prospects
The XXth Recontres de Blois, "Challenges in Particle Astrophysics"
2
Telescope Array CollaborationK.KASAHARA1, H.KAWAI2, S.YOSHIDA2, H.YOSHII3, T.CHUNG4, S.W.NAM4, S.OH4, I.H.PARK4, J.H. PARK4, J.YANG4, B.G.CHEON5, Y.UNNO5, Y.H.YUN5, K.TANAKA6, F.COHEN7, M.FUKUSHIMA7,N.HAYASHIDA7, K.HIYAMA7, D.IKEDA7,E. KIDO7, Y.KONDO7, T.NONAKA7, M.OHNISHI7, H.OHOKA7,S.OZAWA7, H.SAGAWA7, N.SAKURAI7, T.SHIBATA7, H.SHIMODAIRA7, M.TAKEDA7, A.TAKETA7,M.TAKITA7, H.TOKUNO7, R.TORII7, S.UDO7, Y.YAMAKAWA7, H.FUJII8, T.MATSUDA8, M.TANAKA8,H.YAMAOKA8, K.HIBINO9, T.BENNO10, M.CHIKAWA10, K.DOURA10, T.NAKAMURA11, P.HUENTEMEYER12,G.SINNIS12, M.TESHIMA13, K.KADOTA14, Y.UCHIHORI15, K.HAYASHI16, Y.HAYASHI16, S.KAWAKAMI16,T.MATSUYAMA16, M.MINAMINO16, S.OGIO16, A.OHSHIMA16, T.OKUDA16, N.SHIMIZU16, H.TANAKA16,D.R.BERGMAN17, G.A.HUGHES17, L.M.SCOTT17, S.R.STRATTON17, G.B.THOMSON17, A.ENDO18,N.INOUE18, S.KAWANA18, Y.WADA18, R.AZUMA19, T.FUKUDA19, T.IGUCHI19, F.KAKIMOTO19,S. MACHIDA19, Y. MURANO19, Y. TAMEDA19, Y. TSUNESADA19, J. CHIBA20, K. MIYATA20, J. ORMES21,J.A.J.MATTHEWS22, R.U.ABBASI23, T.ABU-ZAYYAD23, J.W.BELZ23, S.A.BLAKE23, O.BRUSOVA23,R. CADY23, Z. CAO23, C.C.H. JUI23, K. MARTENS23, M. MOSTAFA23, J.N. MATTHEWS23, D. RODRIGUEZ23,J.D.SMITH23, P.SOKOLSKY23, R.W.SPRINGER23, J.R.THOMAS23, S.B.THOMAS23, L.R.WIENCKE23,T.DOYLE24, M.J.TAYLOR24, V.B.WICKWAR24, T.D.WILKERSON24, K.HONDA25, K.IKUTA25, T.ISHII25,T.KANBE25, T.TOMIDA25, I.S.CHO26, Y.KWON26
(1) Advanced Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo, 169-8555 Japan (2) Chiba University, 1-33 Yayoi-cho, Inage-ku, Chiba, 263-8522 Japan(3) Ehime University, 2-5 Bunkyo-cho, Matsuyama, Ehime, 790-8577 Japan(4) Ewha Womans University, Daehyun-Dong 11-1, Seodaemun-Gu, Seoul, 120-750, Korea(5) Hanyang University, Haengdang-Dong 17, Seodaemun-Gu, Seoul, 133-791, Korea(6) Hiroshinma City University, 3-4-1 Ozuka-Higashi, Asa-Minami-ku, Hiroshima, 731-3194 Japan(7) Institute for Cosmic Ray Research, University of Tokyo, University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba, 277-8582 Japan(8) Institute of Particle and Nuclear Studies, KEK, 1-1 Oho, Tsukuba, Ibaraki, 305-0801 Japan(9) Kanagawa University, 3-27-1 Rokkakubayashi, Kanagawa-ku, Yokohama, Kanagawa, 221-8686 Japan(10) Kinki University, 3-4-1 Kowakae, Higashi-Osaka, Osaka, 577-8502 Japan(11) Kochi University, 2-5-1 Akebono-cho, Kochi, 780-8520 Japan. 12Los Alamos National Laboratory, Los Alamos, NM 87545, USA(13) Max-Planck-Institute for Physics, Foehringer Ring 6, 80805 Muenchen, Germany(14) Musashi Institute of Technology, 1-28-1 Tamazutsumi, Setagawa-ku, Tokyo, 158-8558 Japan(15) National Institute of Radiological Sciences, 4-9-1 Anagawa Inage-ku, Chiba, 263-8555 Japan(16) Osaka City University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka, 558-8585 Japan(17) Rutgers University, 136 Freilinghuysen Road, Piscataway, NJ 08854, USA(18) Saitama University, 255 Shimo-Okubo, Sakura-ku, Saitama, 338-8570 Japan(19) Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo, 152-8550 Japan(20) Tokyo University of Science, 2641 Yamazaki, Noda-shi, Chiba, 278-8510 Japan(21) University of Denver, Denver, CO 80208, USA(22) University of New Mexico, Albuquerque, NM 87131, USA(23) University of Utah,115 S 1400 E, Salt Lake City, UT 84112, USA(24) Utah State University, Logan, UT 84322, USA(25) Yamanashi University, 4-4-37 Takeda, Kofu, Yamanashi, 400-8510 Japan(26) Yonsei University, Sinchon-Dong 134, Seodaemun-Gu, Seoul, 120-749, Korea
26 institutes from Japan, USA and Korea
The XXth Recontres de Blois, "Challenges in Particle Astrophysics"
3
Concept of TA Hybrid detector: Ground array + Fluorescence telescopes
Ground array : Plastic scintillator (same as AGASA)
Less sensitive to the hadronic interaction models
Trigger efficiency is 100% above 1018.7eV.
Energy spectra of AGASA should reproduce at TA-SD.
Telescope : 2 new telescopes and 1 HiRes telescope.
3rd TA-FD station is a transfer of HiRes-1
Absolute calibration using LINAC in desert.
Energy spectra of HiRes is compared with TA-FD result directory.
(SD)
(FD)
Area Thickness Readout Electronics Spacing
AGASA 2.2 m2 50 mm Direct PMT Log Amp. 1.0 km
TA-SD 3.0 m2 12 mm x 2 WLS fiber FADC 1.2 km
The XXth Recontres de Blois, "Challenges in Particle Astrophysics"
4
Fluorescence telescope Surface detector Comm. tower
Millard county, Utah, USA
N39.1o W122.9o
1350-1500m a.s.l.
3 Telescopes + 503 SDs
27km
(Google earth)
TA site TA equipments (FD)
Long Ridge Black Rock Mesa
Middle Drum
3.3 m dia.
FOV: 3o – 18o x 18o
Mirrors
1021mm
89
3m
m
PMT: HAMAMATSU R9508
Bleeder circuit with pre-amplifier
camera
60 mm Hex.,
256 PMTs
17.7o – 33o x 18o
Newly developed telescopes ( BRM & LR ) 12 telescopes/station
HiRes-1 system ( Mdddle Drum station )
14 telescopes in this station
The XXth Recontres de Blois, "Challenges in Particle Astrophysics"
5
Fluorescence telescope Surface detector Comm. tower
Millard county, Utah, USA
N39.1o W122.9o
1350-1500m asl
3 Telescopes + 503 SDs
27km
(Google earth)
TA equipments (SD)
Grid with 1.2km spacing
Plastic scintillator detector3m2 x 1.2 cm x 2 layers
Wireless LAN,GPS12bit 50MSPS FADC
The XXth Recontres de Blois, "Challenges in Particle Astrophysics"
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LongRidgeMirror
30cm
Nd;YAG laser 355nm, 4mJ(ma
x) 5ns pulse
100 m
Back scatter LIDAR TA-LIDAR
Height from ground [km]
19 Aug in 2006 : elv90o , azm90o
Horizontal beam data
Vertical beam data
Expectation from the Rayleigh scattering using observed temperature and pressure.E
xtin
ctio
n C
oef
f.
Camera0 Camera2
Camera3Camera1
Camera4 Camera6
BRM
FD event display of a LIDAR event
The XXth Recontres de Blois, "Challenges in Particle Astrophysics"
7
Central Laser Facility
Steerable Nd:YAG laser 355 nm, 5 mJ
Atmospheric monitoring, “Test beam”
Long Ridge
Black Rock Mesa
June 13, 2007, 05:45 (UTC)
frame head (sec)=
01.0000630
frame head =
01.0000630
peak time diff. < 100ns
TA-CLF
The XXth Recontres de Blois, "Challenges in Particle Astrophysics"
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2007
Nov.
Dec.
2008
Jan.
Feb.
Mar.
Observation @ BRM,LR 14/1314/13 nights (76 hours)
MD(Middle Drum) site started observation, 1717 nights
Observation @ BRM,LR 12/812/8 nights (76 hours) , @ MD 2020 nights
SD final massive deployment & communication adjustment.
Observation @ BRM,LR 18/1618/16 nights (120 hours), @ MD 1919 nights
SD test observation with the small sub arrays.
Observation @ BRM 1616 nights (112 hours), @ MD 1515 nights
SD DAQ studies and improvements.
Observation @ BRM,LR 14/1514/15 nights (106 hours), @ MD 1818 nights
SD DAQ started in whole region.
Observation summary
The XXth Recontres de Blois, "Challenges in Particle Astrophysics"
9
Every second # of clock pulse between each 1 PPS from GPS Time stamp of GPS # of trigger above 3 MIP.
Every minute # of trigger above 0.3 MIP Battery voltage, charge current Solar panel output voltage Temperatures of SD equipments Humidity in the detector box
Every 10 minutes Histograms of 1MIP & pedestal distributions Histograms of 1MIP & pedestal distributions Histograms to check PMT linearity Histograms to check PMT linearity # of satellites used by GPS.
SD : Monitors on siteMonitor data : Apr. 30 May 5
>0.3MIP trigger rate: ~ 750Hz
>3MIP trigger rate: ~20Hz
1MIP peak : Up ~50 , Low ~50
# of GPS satellite ~9
Temp. & Humid
Battery Voltage & current
Shower Trigger rate of each branch
BRMLRSK
The XXth Recontres de Blois, "Challenges in Particle Astrophysics"
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Log(E[eV])=19.1Log(E[eV])=19.1Zenith=36.3[deg]Zenith=36.3[deg]Azimuth=241.2[deg]Azimuth=241.2[deg]
1010ss
early late
SD: Event sampleExample of real data
LDF fitting Core position
Very preliminary
Very preliminary
The XXth Recontres de Blois, "Challenges in Particle Astrophysics"
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FD: Observation time
Ratio of Clear night
Jan. 6/18 days
Feb. 7/16 days
Mar. 6/14 days
Total observation time
BRM :629.5 hr
LR : 464.6 hrDead time
10.5% (13% ~ 5%)
The XXth Recontres de Blois, "Challenges in Particle Astrophysics"
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Only data of 2007/Nov. : 76/78 hours, 18 stereo events
FD: Core positions (stereo)
The XXth Recontres de Blois, "Challenges in Particle Astrophysics"
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BRM
LR
Time(UTC) RUN-ID TRIG-ID CAM-ID
BRM07/11/19
09:03:09.753991850111905 107 5
LR07/11/19
09:03:09.753955600111907 4641 2, 4, 5Charge
FD: Stereo event example
The XXth Recontres de Blois, "Challenges in Particle Astrophysics"
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θ[deg]
φ[deg]
core position(x, y) [km]
45.8 -0.5 (-8.2, -7.4)
X1
[g/cm2]Xmax
[g/cm2]Nmax
E0
[eV]
0.0 720.0 2.4*109 3.0*1018
LR BRM
preliminary
FD: Stereo event reconstruction
The XXth Recontres de Blois, "Challenges in Particle Astrophysics"
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Horizontal [m]
Vertical [m]
Specifications of TA-LINAC•e- beam•Energy is variable:10 -> 40 MeV•Pulse width: 1usec •Current: 0.16mA (=109e-/pulse)•Frequency: 1Hz•Distance from FD: 100m
40MeVx109e- @100m away→ Total energy = 4x1016eV⇔1020 eV AS @10km away
TA-LINAC calibration(1)
The XXth Recontres de Blois, "Challenges in Particle Astrophysics"
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After bending mag.
•Current status of LINAC•LINAC will be moved to site in this summer.•Pre-construction and test has done at KEK
Before bending mag.
e-gun Bunching unit 2m acc. tube90deg.magnet
Slit
Window
Faraday cup
Core monitor Screen monitor
B=0.6048T R=220mm→ Beam energy=39.4 MeV
5mm10mm
L R
Down
UpAfter 90o
e-gun683mV
Buncher385mV
acc. tube402mV
output226mV
Core monitor
右L
Down
Up
5mm10mm
Before 90o
R
Hole
TA-LINAC calibration(2)
The XXth Recontres de Blois, "Challenges in Particle Astrophysics"
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Telescope Array experiment We deployed 503SDs and started full observation. All FD stations have been installed and started 3 stereo observation.
Target Confirm/refute super-GZK and cluster in Northern hemisphere.
Understand Surface detector systematic errors (energy scale).
Establish the FD energy calibration by LINAC beam.
Establish FD-stereo, and SD-FD stereo-hybrid measurement and energy calibration.
FutureLINAC for end-to-end calibration will start this summer.
TALE = TA Low energy Extension (1016.5 eV – GKZ energy)
Summary & Future