Transcript Telescope Array experiment Hiroyuki Sagawa (ICRR, University of Tokyo) on behalf of

Telescope Array experiment
Hiroyuki Sagawa
(ICRR, University of Tokyo)
on behalf of TA Collaboration
at BNL
10 April, 2008
1
Content

Status of “Telescope Array (TA) experiment”
( Main topics today )
 Explore the origin of highest energy cosmic rays
 Hybrid detector of fluorescence telescopes and a
surface array of particle detectors (~1,000km2) to
detect extensive air shower events from cosmic rays
of energies around/beyond 1020eV

Future ambitious plan of radio detection of
highest energy cosmic rays on the ground

~100,000km2 ( 100 times larger than TA )
2
Energy vs
Flux of cosmic rays
Observed flux
One / year / m2
One / sec / m2
One / year / 100 km2
One / year / km2
1020（eV）
Energy （electron volt）
3
Energy spectra of extremely high energy
cosmic rays
Japan

( scintillator particle detectors )





Akeno Giant Air Shower
Array (AGASA)
~100 km2
111 scintillator detectors
Size: 2.2 m2
Spacing: ~1 km
Once per year above
1020 eV
4
E > 10 19 eV
AGASA
> 10 20.0 eV
> 10 19.6 eV
> 10 19.0 eV
E > 10 19.6 eV
Distribution of arrival directions & distributions
5
of separation angles → clusters
Telescope Array



Research for the
origin of the highest
energy cosmic rays
Originally it was
proposed as an
array of many
fluorescence
telescopes.
But, …
Fluorescence telescope
measures longitudinal
profile ( or composition ).
6
Energy spectra of extremely high energy
cosmic rays
Utah, USA
Japan
( scintillator particle detectors )
( fluorescence telescopes)
=＞Next generation ( Telescope Array, Auger )
Verify whether the GZK cutoff exists or not.
7
TA : Hybrid detector


Hybrid of fluorescence telescopes and
surface detector array
Fluorescence telescopes ( FD )


HiRes-type detector
Surface detector array ( SD )

AGASA-type plastic-scintillator detectors :

sensitive to electromagnetic component

( AUGER : water tank ( sensitive to muons ) )
8
The Mission of phase-1 TA

Mission
Confirm/Refute Super-GZK ( energy spectrum )
 Cluster
 Composition


Method
By ~10 times of AGASA
 Hybrid ( FD, SD )

9
Advantages of TA
As a hybrid detector,
 Surface detector array with plastic
scintillators

AGASA used plastic scintillators


( Auger : water tanks )
Fluorescence detectors (FD)
One of TA FD stations : HiRes mirrors
 Electron-beam LINAC : absolute energy
calibration with electron beams at the site of
TA

10
Surface detectors ( SD )

TA : Plastic scintillators :

sensitive to electromagnetic components




~90% of total energy
Small dependence of hadron interaction model /
composition
SDs can determine energy scale independently of
fluorescence detectors.
Auger : water tanks



Sensitive to muons
Large model dependence and composition
dependence
AUGER’s SDs cannot determine energy scale
independently. Basically FD-based energy scale.
11
12
Xmax Auger and HiRes
HiRes
13
Highest energy cosmic
rays are still very
mysterious !
14
TA LHCf workshop on March 15
The LHCf Experiment
SAKO Takashi (STE Lab., Nagoya University)
for the LHCf collaboration
CONTENTS
1, Physics
2, Detector Concept
3, LHCf Detectors
4, Calibration
5, LHCf Operation
(6, Absolute Cross Section)
Hardwareの話中心。MCベースの話は毛受トークで。
15
2008年3月15日（土） Air Shower MC Mini Workshop @ ICRR
モデル弁別
TA LHCf workshop on March 15
16
Where is TA ?
17
Salt Lake City
18
Experiment
Original
plan
19
ＦＤ stations
Middle Drum
HiRes-1
system
14
telescopes
12telescopes/station
camera
１０２
１ｍｍ
Long Ridge
60 mm
Hex.,
256 PMTs
Black Rock Mesa
FOV: 3o –
18o x 18o
17.7o –
33o x 18o
3.3
m dia.
PMT:
HAMAMA
TSU
R9508
Bleeder
circuit
with preamplifier
Mirr
ors
20
Pair Creation Dip
V.Berezinsky
21
ICRC07
Auger Spectrum x 1.5
+M.Teshima
"Auger.txt"
"Auger1.5.txt"
1e+025
1e+024
1e+023
17
17.5
18
18.5
19
19.5
20
20.5
21
22
Specification of LINAC
40MeV e-
Air Shower
Made by
Geant4
Height (m)
100
View of lower
FD Camera
Shower Development
Shower Max ～0.35X/X0
View of upper
FD Camera
100m far from FD station
100m
40MeV×109 ～1016eV
Horizontal (m)
Energy: Max40MeV( Continuous adjust )
Repetation : 1Hz（Max)
Beam power: 6.4mJ/pulse(=109e－/pulse)
Pulse width: 1μsec
10km far from FD station
～1016eV×104=1020eV
Pseudo EHECR events
23
Telescope Array Collaboration
R.AzumaA, K.IkutaB, T.IguchiA, D.IkedaAB, T.IshiiB, H.IshizukaAB, N.InoueC, S.IwamotoB, Y.UchihoriD,
S.UdoAB, A.EndoC, H.OhokaAB, M.OhnishiAB, A.OhshimaE,S.OgioE, T.OkudaE, S.OzawaAB, F.KakimotoA,
K.KasaharaF, K.KadotaG、H.KawaiH, S.KawakamiE, S.KawanaC, T.KanbeB, E.KidoAB, Y.KondoAB,
H.SagawaAB, N.SakuraiAB, T.ShibataAB, H.ShimodairaAB, S.SuzukiJ, M.TakedaAB, A.TaketaAB, M.TakitaAB,
K.TanakaI, H.TanakaE, M.TanakaJ, Y.TamedaA, M.ChikawaK, J.ChibaL,Y.TsunesadaA, M.TeshimaM,
H.Tokuno, T.TomidaB, R.Torii, K.DouraK, T.NakamuraN, T.Nonaka, K.HayashiA, N.Hayashida, Y.HahashiE,
K.HibinoO, K.HiyamaAB, M.FukushimaAB, T.FukudaA, H.FujiiJ, K.HondaB, S.MachidaA, T.MatsudaJ,
T.MatsuyamaE, M.MinaminoE, K.MiyataL, Y.MuranoA, H.YamaokaJ, Y.YamakawaAB, K.YamamotoAB,
Y.WadaC, N.YoshiiP, S.YoshidaH, R.U.AbbasiQ, T.Abu-ZayyadQ, J.W.BelzQ, D.R.BergmanR, S.A.BlakeQ,
O.BrusovaQ, R.CadyQ, Z.CaoQ, B.G.CheonS, I.S.ChoT, W.R.ChoT, T.ChungU, F.Cohen, T.DoyleV,
P.HuentemeyerW, G.A.HughesR, C.C.H.JuiQ, H.KangX, H.B.KimS, Y.J.KwonT, K.MartensQ, J.A.J.MatthewsY,
J.N.MatthewsQ, M.MostafaQ, S.NamU, J.OrmesZ, S.OhU, I.H.ParkU, J.H.ParkU, D.RodriguezQ, D.RyuAA,
L.M.ScottR, B.K.ShinS, G.SinnisW, J.D.SmithQ, P.SokolskyQ, R.W.SpringerQ, S.R.StrattonR, M.J.TaylorV,
J.R.ThomasQ, S.B.ThomasQ, G.B.ThomsonR, Y.UnnoS, V.B.WickwarV, L.R.WienckeQ, T.D.WilkersonV,
J.YangU
A: Tokyo Institute of Technology, B: Yamanashi Univ., AB: Institute for Cosmic Ray Research, University of Tokyo,
C:
Saitama University, D: National Institute of Radiological Science, E: Osaka City Univ.,
F:
Advanced Research Institute for Science and Engineering, Waseda Univ., G: Musashi Institute of Technology,
H:
Chiba Univ., I: Hiroshima City Univ., J: Institute of Particle and Nuclear Studies, KEK, K: Kinki Univ.,
L:
Tokyo Univ. of Science, M: Max-Planck-Institute for Physics, N: Kochi Univ., O: Kanagawa Univ., P: Ehime Univ., Q:
Univ. of Utah, R: Rutgers Univ., S: Hanyang Univ., T: Yonsei Univ., U: Ewha Womans Univ., V: Utah State Univ., W: Los
Alamos National Laboratory, X: Pusan University, Y: Univ. of New Mexico,
Z: Univ. of Denver, AA: Chungnam National Univ.
USA, Japan, Korea
28 institutes 116 members
24
Surface detector (SD)
25
Phase-I TA project
Millard County, Utah, USA
Altitude ~1400 m
Surface Detector (SD)
503+4 (~700km2)
576 scintillator detectors
3m2 size, 1.2 km interval
3 FD stations
(atmospheric
fluorescence
telescopes)
30 km
26
Trigger Efficiency vs Eo
Detector configuration
square deployment
1.2km spacing
3m2 size
100% (>1019eV)
for q < 45o
Triggering condition
In the case of
adjacent 4fold coincidence
of SDs ( >=1 particle/SD )
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Surface Detectors ( SD )
Solar panel (120W)
Wireless LAN
antenna
(2.4GHz)
GPS antenna
Scintillator Detector
roof
stand
Electronics box
Main board with FADC / GPS / wireless
LAN modem / charge controller
& battery
28
Scintillator Detector
Scintillator
3m2 area 1.2cmt 2 layers
Wave Length shifter Fiber(WLF)
1.0mm diameter 2 cm interval
Outputs from PMTs
2 PMTs (Electrontubes 9124SA)
( PMTs for upper/lower layers )
Scintillator box
stainless steel
230 x 170 x 10(cm3)
( 1.2mm, 1.5 mm thickness)
Total weight ~200 kg
fibers
separated optically
29
Assembly of scintillation detectors


20 SDs as Test Array in 2004
Started mass production in May, 2005 … 348 SDs in 2005
Assembly in ICRR, Japan


Completion of assembly in Oct 2006 … 150 SDs in 2006
Totally 514 SDs were sent to Utah, USA.
30
SD electronics
Main board
12bit 50MSPS FADC
Wireless LAN modem
ADLINK 540F
Charge Controller
GPS
Time stamp
( resolution < 20 ns )
DYNASTY
DCS-100L (12V 100Ah)
Power consumption of ~6W
31
Communication Towers for FD, SD
Completed surveys for animals, vegetation, and heritage in TA
site requested by Burea of Land Manager (BLM)
colinear
antenna
After the bird habitation conservation season,
Three towers were built in Sep, 2006.
DM
LR
BRM
30 km
32
Final assembly of SDs
Cosmic Ray Center in DELTA in Utah
Install scintillator box ( from Japan )
on the stand ( fabricated in Utah )
DELTA
Attach PMT ( tested in Japan ),
solar panel, battery, electronics,
Electronics box
SD assembly
Transport SDs
by 2 trailers
Deploy SD by helicopter
Staging Area
33
28th of February, 2007
deployed 485 SDs
Grid with 1.2km spacing
Three sub-arrays ( ~7x7 SDs for each )
are ( being ) prepared for the
observation and detailed check.
Remaining SD tuning was performed
last October.
34
We deployed 503 SDs by last December
Example (A) of Air shower event
by surface array

Trigger condition :
At least three SDs
 more than 3MIPs

9 particles
4 particles
5
Miles
2ms
The radius is proportional
to log of deposited energy
123 particles
57 particles
11 particles
early
late
35
Example B
Data>0.3MIPs
10ms
early
late
Trigger>3MIPs
Log(E[eV])=19.1
Zenith=36.3[deg]
Azimuth=241.2[deg]
36
• TA surface detector has
been fully operated since
March 20, 2007.
37
Trigger
and DAQ flowlocal
chart
HOST
Send command
Search 3fold (8us)
Send triggered time
and position
Send 3MIPS table
(time and charge)
Search waveform
(>0.3MIP, ±48us)
Send command
Send waveform
store
38
39
40
41
42
43
Fluorescence
Telescope (FD)
44
FD Stations
3rd FD Station
HiRes Telescopes was moved
@ Middle Drum
2nd FD Station
s
@ Long Ridge
1st FD Station
@ Black Rock Mesa
MD
LR
BRM
35km
Millard county, Utah, USA
All three FD stations are operating
since last November.
45
FD Station & Fluorescence telescopes
12 Telescopes/station
(Upper ×6 Lower ×6)
Fluorescence Telescope
Segment
mirror×18
256PMTs
1160mm
1010mm
Camera
Camera
FD Station
@BRM
FOV
Azimuth: 18°×6=108°
Elevation:
Upper: 3°～18°
Lower:17.7°～33°
φ3.3m
Hex PMT+BG3 Filter
(Hamamatsu R9508)
46
FD Electronics
Patch Panel
Pre-amp
Signal Digitizer and Finder (SDF)
16/camera
st
1 level trigger
(signal-finding process)
Recorded waveform: 51.2 ms
Dynamic Range:
PMT
Camera
8k p.e./100 ns
VME PC
Track Finder (TF) 1/camera
2nd level trigger
track-find process
Partial track on
border
5.4 ms for trackfinding process
VME
Run Control PC
Data Storage
Central Trigger Distributor (CTD) 1/station
VME
Inter-mirror trigger, External trigger
Distribute Final Trigger to
all the telescopes
Total triggering process
time: 9.8 ms
GPS, System clock, Reset/Interrupt
HV PS:
individual HV
CTD PC
Slow Control PC
WEB PC
HV PC
LAN
Internet
47
Stereo event
Taken in June 14, 2007, 09:49(UTC)
Long Ridge
frame head (sec) =50.0017877
Black Rock Mesa
frame head =50.0017877
peak time diff. ~10ms ~3km
48
Stereo-hybrid event
On August 13th
UTC 07:16:36
SD:
UTC+614030 us
BRMFD:
UTC+614054 us
LRFD:
UTC+614106 us
LRFD
SD
BRMFD
49
LIDAR system
FD event display of a LIDAR event
Camera0
Camera2
Camera1
Camera3
Camera4
Laser & Telescope
Camera6
Shot!
100 m
LIDAR Doom
Site : BRM
In future,
New One will
be built at LR
Mirror
30cmf
Nd;YAG laser
355nm, 4mJ(max)
5ns pulse
LIDAR system is
operating at BRM, now!
50
CLF system
Central Laser Facility
Steerable Nd:YAG laser 355 nm, 5 mJ
Atmospheric monitoring, “Test beam”
Long Ridge
Black Rock Mesa
CLF event were Observed at BRM&LD.
Event Time : June 13, 2007, 05:45 (UTC)
51
Linear
Accelerator
designed and
assembled with
the collaboration
of ICRR and KEK
Recycle of used
or spare parts of
KEKB
52
Calibration using by LINAC
Uncertainties in Fluorescence Telescope
Fluorescence Yield
～15%
Attenuation in Atmosphere
～11%
Detector (Q.E.,C.E.,PMT Gain) ～10%
～6%
Reconstruction
Calibrate all calibration
constant except
atmospheric parameters。
End-to-End Calibration
(1) Known Primary Energy = Known Energy Loss
(2) We can ignore the attenuation for 100 m in Atmosphere
Calibration with LINAC near from FD is Very Useful !!!
53
Beam test@KEK
In February
Time (ns)
Flash of beam measured with screen monitor
Accelerated electron beam (mA)
Electron gun beam (mA)
Beam current measured with core monitor
Flash by beam
The LINAC will be sent in May.
54
configuration
TheThe
current
configuration
of TA
(mostly final)
503 SDs
of TA now
To be deployed
next autumn
55
Summary of TA

Fluorescence Detectors (FD)
Three stations were completed.
 Fully operated since November, 2007.


Surface Detectors (SD)
We deployed 503 SDs by the end of 2007.
 New SD-DAQ firmware will be installed in
March, 2008 for the full operation.


We have a lot of items towards the
precise measurements.
56