Telescope Array Experiment ICRR N. Sakurai for TA collaboration Concepts Site & equipments...

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


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


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


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


6

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


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


8

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


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


10

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


11

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%)


12

Only data of 2007/Nov. ： 76/78 hours, 18 stereo events

FD: Core positions (stereo)


13

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


14

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


15

TA: Hybrid event sample


16

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)


17

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)


18

Low energy Extension: TALE


19

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


20

Telescope Array Experiment ICRR N. Sakurai for TA collaboration Concepts Site & equipments...

Documents

Transcript of Telescope Array Experiment ICRR N. Sakurai for TA collaboration Concepts Site & equipments...