T h e S t a t u s o f T e l e s c o p e A r r - - PowerPoint PPT Presentation

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S c i e n t i f i c A c t i v i t i e s

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I C R R S c i e n t i f i c A c t i v i t i e s

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I C R R ” ”

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b s e r v a t i

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i g h E n e r g y C

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m i c R a y s h i g h E n e r g y C

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m i c R a y s

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h e S t a t u s

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e A r r a y T h e S t a t u s

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O c t . 1 9 t h , 2 6 @ O c t . 1 9 t h , 2 6 @ K a s h i w a K a s h i w a , J a p a n , J a p a n M . F u k u s h i m a M . F u k u s h i m a

Telescope Array (TA)

Originally planned as a large array of fluorescence telescopes to identify the origin of super-GZK (E > 1020eV) cosmic rays (ICRR review in 2000). HiRes monocular spectrum suggested existence of GZK cutoff (27th ICRC @ Hamburg in 2001). Physics? Method? Statistics? Critical look at systematics of SD (AGASA) and FD (HiRes) measurements became imperative. Phase-1 TA financed in 2003 as SD / FD hybrid detector.

Mechanism of GZK Cutoff Mechanism of GZK Cutoff

2.725 K 411 ph / cm3

Gamma Beam Energy (GeV) Cross Section (mb) 0.1 0.01

γ+ p→Δ（ 1232） → πo p or π+ n

Gamma Beam Energy (GeV) Cross Section (mb) 0.1 0.01

γ+ p→Δ（ 1232） → πo p or π+ n

Gamma Beam Energy (GeV) Cross Section (mb) 0.1 0.01

γ+ p→Δ（ 1232） → πo p or π+ n

0.6 x 10-27 cm2

γ

p n p

π

＋

μ

＋

ν e

＋

ν

γ

E = 1

2 0e

V E . 8 x 1

2 0e

V ̃

The super The super-

• GZK Cosmic Rays must call for a New Physics.

GZK Cosmic Rays must call for a New Physics.

Energy Spectra by AGASA and HiRes (mono) AGASA HiRes

Ground Array (plastic scintillator) Fluorescence Telescope

A G A S A : s t

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p e d i n J a n , 2 4 A u g e r : 1 s t r e s u l t i n A u g . 2 5 H i R e s : s t

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p e d i n A p r . 2 6 T A : w i l l s t a r t D A Q i n A p r i l 2 7 A u g e r

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• u

t h : w i l l b e c

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p l e t e d i n 2 7

SHINOZAKI @WeiHai, 2006

AGASA

Monocular Spectra New “fully efficient” stereo Spectrum - no cloud cuts Most recent Mono spectrum (with cloud cuts)

SOKOLSKY @WeiHai, 2006

HiRes

ZAVRTANIK @WeiHai, 2006

AUGER

ZAVRTANIK @WeiHai, 2006

AUGER

N

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c l u s i

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r e a c h e d

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G Z K . E n e r g y S c a l e i s i n q u e s t i

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. B u t i t m a y n

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b e t h e

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l y c a u s e

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D i s c r e p a n c i e s . E v e n a f t e r e n e r g y r e s c a l i n g , #

• f

e v e n t s w i t h E > 1

2

e Vd i f f e r s a m

• n

g e x p e r i m e n t s .

A G A S A : s t

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p e d i n J a n , 2 4 A u g e r : 1 s t r e s u l t i n A u g . 2 5 H i R e s : s t

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p e d i n A p r . 2 6 p h

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T A : w i l l s t a r t D A Q i n A p r i l 2 7 A u g e r

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t h : w i l l b e c

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p l e t e d i n 2 7

3 x Fluorescence Stations

AGASA x 4

576 Counters

AGASA x 9

Low Energy Extension

TALE TALE Phase Phase-

• 1 TA

1 TA

• Comm. Tower

CLF

Millard County in Utah / USA

Plastic Scintillator

3 m2, 12 mm t

WLSF readout, 2 layers overlaid

1 MI P phot o-elect ron distribut ion

24 pe

• 50 MHz, 12 bit FADC
• GPS time stamp (~20ns)
• Wireless LAN modem
• Solar panel + charge controller
• Battery
• Slow control

U p p e r l a y e r

Spectrum and Rate for Cosmic Muon

628 Hz at 1/3μ 42 Hz at 3μ ~ 1000 Hz. Triggered by lower layer at 1/3μ level Wave form recorded locally at each counter T i m i n g s e n t t

• c
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m . t

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e r f

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C

• i

n c i d e n c e T r i g g e r m u

• n

s p e c t r u m t r i g g e r Integrated over 12 time bins (240ns)

Why Plastic Scintillator ? Conserve AGASA energy scale and check Sample electromagnetic shower (~90% of Eprimary) >>> less dependent on

• primary composition
• hadronic interaction @EHE

Why Two Layers ? trigger and calibration by muon wider dynamic range (PMT Gain H/L) linear upto 60 / 360 MIPs in 20 ns

S(600) for 3 x 1020eV

may vary over GZK energy

• e
• 36o

25o 45o 53o 60o 0o 66o Proton/SIBYLL Proton/QGSJET Iron/SIBYLL Iron/QGSJET

ARISAKA GAP 2004-037

AUGER

Particle density at 540m from shower core vs X - Xmax

Z E N I T H A N G L E

# of particles in upper scintillator # of particles in lower scintillator

Expected Signals from e, γ, μ

b y G E A N T f

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1

1 6

e V p r

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s h

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e r @ 6 g / c m

2

a n d 1 k m a w a y f r

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c

• r

e

2.0 mm t Al 1.2 mm t Fe 1.2 mm t Fe 1.0 mm t Fe 10 mm t Scint.

• 合計５

１ ６ 台を、 ２ ０ ０ ７ 年２ 月までに設置の予定 合計５ １ ６ 台を、 ２ ０ ０ ７ 年２ 月までに設置の予定

○ ○ 80% of 80% of SDs SDs & 3 towers on federal land. & 3 towers on federal land. ○ ○ Took 2.5 years for getting permission from BLM office. Took 2.5 years for getting permission from BLM office.

Surveys of endangered animals and plants, cultural resources Surveys of endangered animals and plants, cultural resources and historical sites, and numerous other administrative w and historical sites, and numerous other administrative works

• rks

done by U of Utah colleagues done by U of Utah colleagues.

.

○ ○ First comm. tower built on Sept.15 First comm. tower built on Sept.15th

th + 16

+ 16th

th

○ ○ First 50 counters will be deployed today (Sept 19). First 50 counters will be deployed today (Sept 19). ○ ○ 516 counters will be in the field by next February. 516 counters will be in the field by next February.

SDs waiting for Deployment near Delta Cosmic Ray Center

From Delta to staging area (~30km) 18 SDs at the staging area 18 SDs deployed in 3 hours

TEST DEPLOYMENT in Dec. 2004

FLUORESCENCE ELESCOPE

• Fixed telescope with spherical mirror
• One telescope with 180 x 150 FoV

seen by mosaic PMT camera

• 6 x 2 telescopes / station
• Field of View 30-330 for elevation

1080 for azimuth

TELESCOPE CAMERA

• 16 x 16 PMT array
• BG3 glass filter (UV transparent)
• Pre-amplifier (x 50)
• 1. 3 PMTs: absolutely calibrated

by standard UV light source (self develop.) & PMT gain monitored by YAP + 241Am.

• 2. All 256 PMTs: relatively adjusted in situ

by diffused light ( Xenon flasher )

• 3. XY-mapping by UV-LED scanner

FADC Track Trig. HV PS LV PC

TELESCOPE ELECTRONICS

1 camera

One of the first events of TA: 2005/07/12, 2:52 am, Utah. 200 ns / step.

top / bottom & left / right of camera view reversed.

Spherical Mirror (3.3m ） , 10 pixel PMT Conserve HiRes optics (30% more light than HiRes) Simple in Optics & Mechanics “Sandwich” configuration for stereo meas..

• less than 20 km to the nearest FD station
• always tagged by the SD
• HV, DC coupled, 40MHz,12-bit sampling

No wave form distortion Direct night sky BG measurement

• “FD as a lidar”

~ms baseline update 5 contiguous PMTs for “track” trigger

• 1st FD station: 8 / 12 telescopes completed
• 2nd station: to be ready by March, 2007
• 3rd station: transfer of HiRes. Ready by June, 2007.

E # of photons

1 . F l u

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e s . E f f . 3 . T e l e s c

• p

e C a l i b . 2 . A t m

• s

p h e r i c C

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r .

loss of photons # of ptotons ADC ch

FD is a Total Absorption Calorimetry for absolute energy measurement

Air Fluorescence Spectrum

Piece to Piece Calibration is needed. We also have Xe flasher, YAP and LED but….

E n e r g y D e p

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i t ＝ F l u

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e s c e n c e E f f i c i e n c y ｘ R a y l e i g h a n d M i e S c a t t e r i n g L

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s ｘ O b s c u r a t i

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（ b y c a m e r a a n d s u p p

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t i n g s t r u c t u r e s ）

ｘ M i r r

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A r e a a n d R e f l e c t i v i t y ｘ T r a n s p a r e n c y

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C a m e r a W i n d

• w

（ U V t r a n s p . l u c i t e ）

ｘ T r a n s m i t t a n c e

• f

B G 3 F i l t e r

（ a g a i n s t N i g h t S k y b g ）

ｘ P M T G a p ｘ P M T Q u a n t u m E f f i c i e n c y ｘ P M T

( d i n

• d

e )

C

• l

l e c t i

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E f f i c i e n c y ｘ P M T G a i n ｘ P r e a m p l i f i e r G a i n ｘ C a b l e A t t e n u a t i

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ｘ S h a p e r / A m p l i f i e r G a i n ｘ F A D C C

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v e r s i

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G a i n ｘ F A D C C

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n t 1 . 2 . 3 . 4 . 5 . 6 . 7 . 8 . 9 . 1 . 1 1 . 1 2 . 1 3 . 1 4 . 1 5 . Energy Deposit FADC count

５ ％? ｘ Ｓ Ｑ Ｒ Ｔ （ １ ５ ） ～ ２ ０ ％ ???

Direct End to End Calibration is wanted.

Inject Electron Linac Beam （ 10 - 40 MeV） into the Sky 20 MeV / particle x 109 ppp = 2 x 1016 eV total energy deposit. Absolutely calibrated Light Source!!

20 MeV 40 MeV

100 m away 100 m away

Telescope FoV PMT pixel

From Energy deposit to ADC ch.

TA-Linac for calibration

Assembly of TA Linac proceeding using KEK B factory injector

• components. Beam test at KEK in March, 2007.

MEADE telescope

• n alto-azimuth mount.

YAG laser (355 nm, 5mJ)

Lidar for Atomospheric Monitoring

Lidar Observation at the BRM station

LOG (photons・ R2) Distance R (m)

Performance of TA

140 km2 sr 25 % 18 % 20 AGASA

• r

b e t t e r

• r

b e t t e r FD

# of Events per Year

SPECTRUM Calibration X -check

Cumulated # of Events

Log（ エネルギー［ eV］ ）

Log ( 流量 x E3)

Expected by GZK cutoff

Result of TA by spring 2010

• AGASA flux
• AGASA Energy x 1 or x 0.8
• TA = SD (516 ctrs) + FD mono

SHINOZAKI @WeiHai, 2006

AGASA

SUMMARY SUMMARY

• Phase

Phase-

• 1 TA approved in 2003:

1 TA approved in 2003: 10 x AGASA + FD 10 x AGASA + FD

• NSF budget approved in 2006:

NSF budget approved in 2006: infra + FD + TALE infra + FD + TALE

TALE: low energy extension of TA TALE: low energy extension of TA

• Start data taking with 516

Start data taking with 516 SDs SDs & 3 & 3 FDs FDs next spring. next spring.

516 516 SDs SDs = 90% of proposal, 3 = 90% of proposal, 3rd

rd FD by

FD by HiRes HiRes transfer transfer

• Confirm

Confirm super super-

• GZK

GZK and cluster in the North by 2010. and cluster in the North by 2010.

• Understand SD

Understand SD systematics systematics. .

• Establish stereo FD method and

Establish stereo FD method and energy calibration energy calibration. . Future: Future: Integrated Giant Ground Detector (> 100 AGASA) Integrated Giant Ground Detector (> 100 AGASA)

Telescope Array Collaboration

H.Kawai a, T.Nunomura a, N.Sakurai a, S.Yoshida a, H.Yoshii b, K.Tanaka c, F.Cohen d, M.Fukushima d, N.Hayashida d, M.Ohnishi d, H.Ohoka d, S.Ozawa d, H.Sagawa d, T.Shibata d, H.Shimodaira d, M.Takeda d, A.Taketa d, M.Takita d, H.Tokuno d, R.Torii d, S.Udo d, H.Fujii e, T.Matsuda e, M.Tanaka e, H.Yamaoka e, K.Hibino f, T.Benno g, M.Chikawa g, T.Nakamura h, K.Kadota j, Y.Uchihori k, Y.Hayashi l, S.Kawakami l, K.Matsumoto l, Y.Matsumoto l, T.Matsuyama l, S.Ogio l, A.Ohshima l, T.Okuda l, D.R.Bergman m, G.Hughes m, S.Stratton m, G.B.Thomson m, N.Inoue n, Y.Wada n, K.Kasahara o, M.Fukuda p, T.Iguchi p, F.Kakimoto p, R.Minagawa p, Y.Tameda p, Y.Tsunesada p, J.W.Belz qs, J.A.J.Matthews r, T.Abu-Zayyad s, R.Cady s, Z.Cao s, C.C.H.Jui s, K.Martens s, J.N.Matthews s, J.D.Smith s, P.Sokolsky s, R.W.Springer s, S.B.Thomas s, L.R.Wiencke s, T.Doyle t, M.J.Taylor t, V.B.Wickwar t, T.D.Wilkerson t, K.Hashimoto u, K.Honda u, T.Ishii u, T.Kanbe u,S.J.Baek v, J.E.Kim v, K.S.Kim v, S.Nam v, I.H.Park v, J.Yang v, B.G.Cheon w, Y.Unno w, Y.H.Yun w, I.S.Cho x, Y.J.Kwon x

(a) Chiba University (b) Ehime University (c) Hiroshima City University (d) ICRR, University of Tokyo, (e) Institute of Particle and Nuclear Studies, KEK (f) Kanagawa University (g) Kinki University (h) Kochi University (j) Musashi Institute of Technology (k) National Institute of Radiological Sciences (l) Osaka City University (m) Rutgers University (n) Saitama University (o) Shibaura Institute of Technology (p) Tokyo Institute of Technology (q) University of Montana (r) University of New Mexico (s) University of Utah (t) Utah State University (u) Yamanashi University (v) Ewha Womans University (w) Chonnam University (x) Yonsei University

80 physicists From Japan, USA and Korea