Telescope Array experiment

1
Telescope Array experiment

• Hiroyuki Sagawa
• (ICRR, University of Tokyo)
• on behalf of TA Collaboration
• at BNL
• 10 April, 2008

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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 )

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1020(eV)
4
Energy spectra of extremely high energy cosmic
rays
Japan

• Akeno Giant Air Shower Array (AGASA)
• 100 km2
• 111 scintillator detectors
• Size 2.2 m2
• Spacing 1 km
• Once per year above 1020 eV

( scintillator particle detectors )
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AGASA
E gt 10 19.6 eV
Distribution of arrival directions
distributions of separation angles ? clusters
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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 ).
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Energy spectra of extremely high energy cosmic
rays
Japan
Utah, USA
( fluorescence telescopes)
( scintillator particle detectors )
gtNext generation ( Telescope Array, Auger
) Verify whether the GZK cutoff exists or not.
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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 ) )

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The Mission of phase-1 TA

• Mission
• Confirm/Refute Super-GZK ( energy spectrum )
• Cluster
• Composition
• Method
• By 10 times of AGASA
• Hybrid ( FD, SD )

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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

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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
• AUGERs SDs cannot determine energy scale
  independently. Basically FD-based energy scale.

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Xmax Auger and HiRes
HiRes
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Highest energy cosmic rays are still very
mysterious !
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The LHCf Experiment
TA LHCf workshop on March 15
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?????MC?????????????
2008?3?15?(?) Air Shower MC Mini Workshop _at_ ICRR
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?????
TA LHCf workshop on March 15
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Where is TA ?
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Salt Lake City
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Experiment
Original plan
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FD stations
Middle Drum
Long Ridge
Black Rock Mesa
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Pair Creation DipV.Berezinsky
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Auger Spectrum x 1.5M.Teshima
ICRC07
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Specification of LINAC
Air Shower
40MeV e-
Height (m)
Made by
Geant4
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View of lower FD Camera
Shower Development
Shower Max 0.35X/X0
100m far from FD station
View of upper FD Camera
100m
40MeV109 1016eV
Horizontal (m)
Energy Max40MeV( Continuous adjust )
10km far from FD station
Repetation 1Hz(Max)
1016eV1041020eV
Beam power 6.4mJ/pulse(109e-/pulse)
Pseudo EHECR events
Pulse width 1µsec
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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
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Surface detector (SD)
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Phase-I TA project
Millard County, Utah, USA Altitude 1400 m
Surface Detector (SD)
5034 (700km2)
3 FD stations (atmospheric fluorescence
telescopes)
30 km
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Trigger Efficiency vs Eo
100 (gt1019eV) for q lt 45o
Detector configuration square deployment
1.2km spacing 3m2 size
Triggering condition In the case of adjacent
4fold coincidence of SDs ( gt1 particle/SD )
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Surface Detectors ( SD )
Wireless LAN antenna (2.4GHz)
Solar panel (120W)
GPS antenna
Scintillator Detector
roof
stand
Electronics box Main board with FADC / GPS /
wireless LAN modem / charge controller
battery
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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
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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.

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SD electronics
Main board 12bit 50MSPS FADC
Wireless LAN modem
ADLINK 540F
Charge Controller
GPS Time stamp ( resolution lt 20 ns )
DYNASTY DCS-100L (12V 100Ah) Power consumption
of 6W
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Communication Towers for FD, SD Completed
surveys for animals, vegetation, and heritage in
TA site requested by Burea of Land Manager
(BLM)After the bird habitation conservation
season, Three towers were built in Sep, 2006.
colinear antenna
DM
LR
BRM
30 km
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Final assembly of SDs
Cosmic Ray Center in DELTA in Utah
Install scintillator box ( from Japan ) on the
stand ( fabricated in Utah ) Attach PMT ( tested
in Japan ), solar panel, battery,
electronics, Electronics box
DELTA
SD assembly
Transport SDs by 2 trailers
Deploy SD by helicopter
Staging Area
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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. We deployed 503 SDs by last December.
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Example (A) of Air shower event by surface array

• Trigger condition
• At least three SDs
• more than 3MIPs

9 particles
4 particles
2ms
The radius is proportional to log of deposited
energy
123 particles
57 particles
11 particles
late
early
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Example B
Datagt0.3MIPs
10ms
late
early
Triggergt3MIPs
Log(EeV)19.1 Zenith36.3deg Azimuth241.2deg

Very preliminary
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• TA surface detector has
• been fully operated since
• March 20, 2007.

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Trigger and DAQ flow chart
HOST
local
Send command
Send 3MIPS table (time and charge)
Search 3fold (8us)
Send triggered time and position
Search waveform (gt0.3MIP, 48us)
Send command
Send waveform
store
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Fluorescence Telescope (FD)
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FD Stations
3rd FD Station
HiRes Telescopes was moved
_at_ Middle Drum
s
2nd FD Station
_at_ Long Ridge
1st FD Station
_at_ Black Rock Mesa
MD
LR
BRM
35km
Millard county, Utah, USA
All three FD stations are operating since last
November.
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FD Station Fluorescence telescopes
12 Telescopes/station
Fluorescence Telescope
(Upper 6
Lower 6)
Segment mirror18
256PMTs
1160mm
Camera
1010mm
Camera
FD Station _at_BRM
f3.3m
FOV
Hex PMTBG3 Filter
Azimuth 186108
(Hamamatsu R9508)
Elevation
Upper 318
Lower17.733
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FD Electronics
Signal Digitizer and Finder (SDF)
Patch Panel
Pre-amp
16/camera
1st level trigger
(signal-finding process)
Recorded waveform 51.2 ms
PMT
Dynamic Range 8k p.e./100 ns
Camera
VME PC
Track Finder (TF) 1/camera
VME
Run Control PC
2nd level trigger
track-find process
Partial track on border
5.4 ms for track-finding process
Data Storage
Central Trigger Distributor (CTD) 1/station
VME
Inter-mirror trigger, External trigger
Distribute Final Trigger to all the telescopes
Slow Control PC
Total triggering process time 9.8 ms
CTD PC
GPS, System clock, Reset/Interrupt
HV PS individual HV
WEB PC
HV PC
LAN
Internet
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Stereo event
Taken in June 14, 2007, 0949(UTC)
Black Rock Mesa
Long Ridge
frame head 50.0017877
frame head (sec) 50.0017877
peak time diff. 10ms 3km
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Stereo-hybrid event
On August 13th UTC 071636 SD UTC614030
us BRMFD UTC614054 us LRFD UTC614106 us
LRFD
BRMFD
SD
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LIDAR system
FD event display of a LIDAR event
Laser Telescope
Shot!
100 m
LIDAR Doom
Mirror 30cmf
NdYAG laser 355nm, 4mJ(max) 5ns pulse
Site BRM
In future, New One will be built at
LR
LIDAR system is operating at BRM, now!
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CLF system
Central Laser Facility Steerable NdYAG laser 355
nm, 5 mJ Atmospheric monitoring, Test beam
Long Ridge
Black Rock Mesa
CLF event were Observed at BRMLD.
Event Time June 13, 2007, 0545 (UTC)
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Linear Accelerator
designed and assembled with the collaboration of
ICRR and KEK
Recycle of used or spare parts of KEKB
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Calibration using by LINAC
Uncertainties in Fluorescence Telescope
Fluorescence Yield
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Calibrate all calibration constant except
atmospheric parameters?
Attenuation in Atmosphere
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Detector (Q.E.,C.E.,PMT Gain)
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Reconstruction
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 !!!
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Beam test_at_KEK In February
Beam current measured with core monitor
Flash of beam measured with screen monitor
Accelerated electron beam (mA)
Electron gun beam (mA)
Flash by beam
The LINAC will be sent in May.
Time (ns)


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The configuration of TA now
The current configuration of TA (mostly final)
503 SDs
To be deployed next autumn
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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.