Contents•Current status of

TA•FD calibration

IKEDA DaisukeICRR, University of Tokyo

( JSPS fellow )

Calibration ofTA Fluorescence Detector

Telescope Array Collaboration

R.U.Abbasi25,T.Abu-Zayyad25,R.Azuma21,J.W.Belz25,D.R.Bergaman19,S.A.Blake25,O.Brusova25,R.Cady25,Z.Cao25,B.G.Cheon6,J.Chiba22,M.Chikawa11,I.S.Cho28,W.R.Cho28,E.J.Cho6,F.Cohen8,K.Doura11,T.Doyle26,T.Fujii17,H.Fujii9,T.Fukuda21,M.Fukushima8,Y.Hayashi17,K.Hayashi21,N.Hayashida8,K.Hibino10,K.Honda27,P.Huenitemeyer13,G.A.Hughes19,D.Ikeda8,N.Inoue20,T.Ishii27,S.Iwamoto27,C.C.H.Jui25,K.Kadota15,F.Kakimoto21,H.S.Kang18,K.Kasahara1,H.Kawai2,S.Kawaka20,S.Kawakami17,E.Kido8,H.B.Kim6,J.H.Kim6,A.Kitsugi8,K.Kobayashi22,Y.Kondo8,Y.Kwon28,J.H.Lim18,K.Martens25,T.Matsuda9,T.Matsuyama17,J.A.J.Matthews24,J.N.Matthews25,M.Mimamino17,K.Miyata22,H.Miyauchi17,M.Mostafa25,T.Nakamura12,S.W.Nam5,T.Nonaka8,S.Ogio17,S.Oh5,M.Ohnishi8,H.Ohoka8,A.Ohshima17,T.Okuda17,J.Ormes23,S.Ozawa1,I.H.Park5,D.Rodriguez25,S.Y.Roh3,D.S,Ryu3,H.Sagawa8,N.Sakurai8,L.M.Scott19,T.Shibata8,H.Shimodaira8,J.D.Smith25,P.Sokolsky25,R.W.Springer25,S.R.Stratton19,G.Sunnis13,S.Suzuki9,M.Takeda8,A.Taketa8,M.Takita8,Y.Tameda21,H.Tanaka17,K.Tanaka7,M.Tanaka9,M.J.Taylor26,M.Teshima14,J.R.Thomas25,S.B.Thomas25,G.B.Thomson19,H.Tokuno8,T.Tomida27

,R.Torii8,Y.Tsunesada21,Y.Tsuyuguchi27,Y.Uchihori16,S.Udo1,H.Ukai27,Y.Wada20,V.B.Wickwar26,L.R.Wiencke25,T.D.Wilkerson26,T.Yamakawa8,Y.Yamakawa8,H.Yamaoka9,J.Yang5,S.Yoshida2,H.Yoshii4

(1) Advanced Research Institute for Science and Engineering, Waseda University (2) Chiba University (3) Chungnam National University (4) Ehime University (5) Ewha Womans University (6) Hanyang University (7) Hiroshinma City University(8) Institute for Cosmic Ray Research, University of Tokyo (9) Institute of Particle and Nuclear Studies, KEK (10) Kanagawa University (11) Kinki University (12) Kochi University (13) Los Alamos National Laboratory (14) Max-Planck-Institute for Physics, (15) Musashi Institute of Technology

(16) National Institute of Radiological Sciences (17) Osaka City University (18) Pusan National University (19) Rutgers University (20) Saitama University(21) Tokyo Institute of Technology (22) Tokyo University of Science (23) University of Denver (24) University of New Mexico (25) University of Utah(26) Utah State University(27) Yamanashi University (28) Yonsei University (29) Institute for Nuclear Research of Russian Academy of Science

～ 30 institutes from Japan, USA, Korea, and Russia

Telescope Array Experiment

•Desert in Utah ,USA•3 stations of Fluorescence Detector•507 Surface Detectors•Full operation was started at Mar/2008

FD

FD (HiRes)

SD

31km

~1400m a.s.l.

Fluorescence Detector

Fluorescence Detector

12telescopes / 1station12telescopes / 1station

F.O.V. :3-18°×18°F.O.V. :3-18°×18°

F.O.V. :17.7-33°×18°F.O.V. :17.7-33°×18°

3300mm3300mm PMT:HAMAMATSU

R9508

PMT:HAMAMATSU

R9508 60mm60mm

256PMTs/camera256PMTs/camera1021mm1021mm

893mm893mm

Middle Drum station (HiRes-1)

FD current status

1417 hours

Observation time of BRM (~ 5/Jan/2009)

Observation(LR 6/12telescope)

TestObservatio

n(BRM)

Full Operationof 3 station

FD -example of event-summation of waveforms

Surface Detector

Surface Detector

Wireless LAN 2.4Ghz

120W Solar panel

GPS

1.2km spacing

Plastic scintillator (AGASA-type)3m2, 1.2cm, 2layer

FADC 12bit 50MHz

SD current status

BR

SK

LR

Live time

Observation as three divided arrays

(504 SD)

Full Operationas one large array

(507 SD)

Add boundary trigger

BRLR

SK

SD monitoring

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 Histograms of 1MIP & pedestal

distributions distributions • Histograms to check PMT linearity Histograms to check PMT linearity • # of satellites used by GPS. Anti-correlation

Characteristics of TA

As a hybrid detector▌ SD►AGASA-type plastic scintillator►Energy can be determined as independent of FD

▌ FD►HiRes-1 was moved as one of the TA FD station.►Absolute calibration by using Electron beam accelerator (TA-LINAC)

▌ The disagreement of AGASA and HiRes can be tested directly.

▌ Fine energy measurement as direct determination by SD, FD with TA-LINAC, and comparison in hybrid event.

FD Calibration

Main items of FD Calibration

▌ Telescope►Absolute gain (photon-to-FADC) measurement by CRAYS

►Relative gain monitor by Xe and YAP►On-site uniformity scanner►Mirror reflectance measurement

▌ Atmospheric►LIDAR►Cloud monitor

▌ End-to-end►CLF►TA-LINAC

The preparation of 1st data set of FD calibration for telescope is almost finished.

PMT Calibration - absolute gain-

•Absolute PMT gain measurement Using N2 laser Rayleigh scattering in N2 gas.

•The absolute gain (photon-to-FADC) of 2 or 3 PMTs in one camera are measured and adjusted by CRAYS.

Peak: 0.5075count/photon(337.1nm)

~1%

N2 Laser

CRAYS

PMT Calibration –relative gain-

YAP (YAlO3:Ce+241Am)

YAP pulsers are installed on the standard PMTs calibrated by CRAYS.2 or 3 PMTs with YAP are installed in each camera.YAP is stable light source for gain monitoring.

Peak 365nm50Hz～ 100Hz

YAP pulser

Xe flusherThe gain adjustment and relative gain monitoring is done by Xe flusher.This measurement is done every 1 hour on observation time.

Result of gain adjustmentAll HV is 850V After adjustment

~1%

PMT Calibration-temperature characteristics of PMT

and YAP-Incubator(-10~40degree)

Optical fibers

Function gen.

Signal Digitizer/Finder

Patch panel

PMTYAP

UV-LED

Splitter

Dark box

Stable room temp. (T±0.5℃)

#0

#1

#2

#3

#4

#5

18

Temperature Coefficientsof PMTs with pre-amplifier

#2 #4 #5

#6 #7 #8 #9

#3

TA ALL meeting

－ 0.6

－ 0.5

－ 0.7

－ 0.8

－ 0.4

%/℃

－ 0.6

－ 0.5

－ 0.7

－ 0.8

－ 0.4

%/℃

－ 0.6

－ 0.5

－ 0.7

－ 0.8

－ 0.4

%/℃

－ 0.6

－ 0.5

－ 0.7

－ 0.8

－ 0.4

%/℃

－ 0.6

－ 0.5

－ 0.7

－ 0.8

－ 0.4

%/℃

－ 0.6

－ 0.5

－ 0.7

－ 0.8

－ 0.4

%/℃

－ 0.6

－ 0.5

－ 0.7

－ 0.8

－ 0.4

%/℃

－ 0.6

－ 0.5

－ 0.7

－ 0.8

－ 0.4

%/℃

－ 10 0 10 20 30 [℃]－ 10 0 10 20 30 [℃]－ 10 0 10 20 30 [℃]－ 10 0 10 20 30

－ 10 0 10 20 30 [℃]－ 10 0 10 20 30 [℃]－ 10 0 10 20 30 [℃]－ 10 0 10 20 30

Average

~ -0.65 %/deg

Temperature Coefficients of YAP

#2 #4 #5

#6 #7 #8 #9

#3

－ 0.2

0

－ 0.4

－ 0.6

+0.2

%/℃

－ 0.2

0

－ 0.4

－ 0.6

+0.2

%/℃

－ 10 0 10 20 30 [℃]－ 10 0 10 20 30 [℃]－ 10 0 10 20 30 [℃]－ 10 0 10 20 30

－ 10 0 10 20 30 [℃]－ 10 0 10 20 30 [℃]－ 10 0 10 20 30 [℃]－ 10 0 10 20 30

－ 0.2

0

－ 0.4

－ 0.6

+0.2

%/℃

－ 0.2

0

－ 0.4

－ 0.6

+0.2

%/℃

－ 0.2

0

－ 0.4

－ 0.6

+0.2

%/℃

－ 0.2

0

－ 0.4

－ 0.6

+0.2

%/℃

－ 0.2

0

－ 0.4

－ 0.6

+0.2

%/℃

－ 0.2

0

－ 0.4

－ 0.4

+0.2

%/℃~ -0.2 %/deg

Other items (filters,QE,CE,uniformity)

PMTPMT

paraglasparaglas

BG3BG3

HITACHI U-1100SpectrophotometerHITACHI U-1100Spectrophotometer

XY-ScannerXY-Scanner

ParaglastransparencyParaglas

transparency

BG3transparency

BG3transparency

Q.E.(HAMMATSU)

Q.E.(HAMMATSU)C.E. (HAMAMATSU)

0.909 +0.005 -0.020C.E. (HAMAMATSU)0.909 +0.005 -0.020

PMT uniformityPMT uniformity

PMT uniformity (XY Scanner)

•We create typical uniformity by using 253PMTs (256 – 3 with YAP).•Because of position and direction of each LED is difference, we can obtain the fine uniformity map better than the resolution of XY Scanner. We get the uniformity map of 1mm×1mm resolution.•Comparison with HAMAMATSU measurement

→ Consistent!

XY Scanner•8LED•Spot: 4mm•Step: 4mm

XY Scanner•8LED•Spot: 4mm•Step: 4mm

Mirror reflectance

e.g.) BRM,camera10,mirror3(most dirty mirror)

Mirror washing→Mirror washing→

•In most dirty term, reflectance is affected byLower telescope： ~-10%Upper telescope： ~-5%

•But each reflectance was almost recovered by mirror washing

Measurement pointMeasurement point

KONICA MINOLTA CM-2500d

Atmospheric - LIDAR and cloud monitor -

IR CameraIR Camera

LIDARLIDARLASER: 5mJ,355nm30cm telescope

The 14 pictures is taken every 1 hour.12 picture is corresponded the F.O.V. of each 12 telescope.

LIDAR is operated every start & end time of observation

Central Laser Facility

Long Ridge

Black Rock Mesa

June 13, 2007, 05:45 (UTC)

frame head (sec)=

01.0000630

frame head =

01.0000630

Central Laser Facility (CLF)

Steerable Nd:YAG laser 355 nm, 5 mJ

Shooting every 1 hour.

Atmospheric monitoring, “Test beam”

Central Laser Facility (CLF)

Steerable Nd:YAG laser 355 nm, 5 mJ

Shooting every 1 hour.

Atmospheric monitoring, “Test beam”

Peak time diff. < 100nsPeak time diff. < 100ns

TA-LINAC

▌ Linacの絵

TA-LINAC –motivation-

10km

FD

Air shower

100m

Linac Beam

Absolute energy calibration!

Uncertainties of FD (design report of TA)•Fluorescence yield 15%•Transparency of Air 11%•Telescope Calibration 10%•Reconstruction 6%

We can get integrated calibration constant except for air.

End-to-end calibration!(We can connect energy deposit to FADC count directly.)

More than 20%

100m

FD

Linac

vertical

horizontal

TA-LINAC -Basic specs-

Specs of TA-LINAC•Particle： e-•Energy： 10, 20, 30, 40 MeV

(variable)•Pulse width： 1μsec •Peak current： 0.16mA

(109e-(=160pC)/pulse)•Frequency： ~1Hz•Distance from FD： 100m

Simulated by geant4 (40MeV)

　　： F.O.V.(upper camera)　　： F.O.V.(lower camera)

@KEKConstruction : finishedBeam test : finished(08/Feb/22 – 08/Dec/10 716hours)

TA-LINAC –Result of beam test-

Beam Charge w/ Faraday Cup(

pC/pulse/q)

Core Monitor Output (mV×μs/pulse )

● Data Set 1

● Data Set 2

● Data Set 3

Reference value = 160pC

Output beam

RF

EGUN

WaveformsWaveforms

Beam Energy SpectrumBeam Energy Spectrum

Peak=39.7MeVSpread < 1%Peak=39.7MeVSpread < 1%

Beam Current MeasurementsBeam Current Measurements

+ Data set#1( ‘08 Nov.11th )+ Data set#2( ‘08 Nov.12th )+ Data set#3( ‘08 Nov.20th )+ Data set#4( ‘08 Nov.21th )+ Data set#5( ‘08 Nov.25th )

Mon1 : Faraday Cup (absolute)Mon2 : Core Monitor (relative)Mon1 : Faraday Cup (absolute)Mon2 : Core Monitor (relative)

Diff. btw each Data : less than 5%Diff. btw each Data : less than 5%

TA-LINAC –Current Status-

Feb/06 @KEKFeb/06 @KEK

•Beam Test @KEK•Beam test was finished at Dec/10.

•Transport to Utah from KEK•Preparation for carrying : almost finished.•Shipping from YOKOHAMA : Mar/1(?)•TALinac will be arrived at Utah on end of Mar

•Shooting at Utah•We can start shooting at next Apr-May !!.

▌ Linacの絵

Conclusion

FD Calibration•The 1st data set of telescope calibration was almost prepared.•TA-LINAC calibration will be started at next Apr-May.

TA•TA will present the first result at ICRC09 with data equivalent of about 1 AGASA.

Grazie mille

note

TA-LINAC –for fluorescence yield

measurement-▌ TA-FD can be calibrated end-to-end by TA-LINAC▌ The difference btw LINAC beam and Air shower►The height of the emission the photon

◘ Air shower (XMAX) ~ a few km◘ LINAC beam ~70m

►Atmospheric condition◘ Pressure, temperature has systematic difference.◘ The variation of humidity is bigger than high atmosphere.

◘ (affected by the rain of before days.

►Our countermeasure◘ Use result of yield measurement◘ Use the result of only dry days.

►Of cause, we can measure this dependence by using daily difference of atmospheric condition.

Mirror reflectance 1

KONICA MINOLTA CM-2500d(360～ 740nm,10nm pitch)

2, In this variation of reflectance, We can see•Height dependence•No wavelength dependence

2, In this variation of reflectance, We can see•Height dependence•No wavelength dependence

1, The measured data is consistent with maker data except for short wavelength.

1, The measured data is consistent with maker data except for short wavelength.

2008/06 (before washing)LR upper telescopeVariation from installation

So we useMaker data•spectrum•Absolute reflectance at installation.

Measured data by CM-2500d•Relative variation of reflectance

Mirror reflectance 2

e.g.) BRM,camera10,mirror3(most dirty mirror)

•We prepared data mirror by mirror.•250nm-740nm•Mean ± standard deviation.•1nm supplement with natural cubic spline.•10 days supplement with linear approximation.

Mirror washing→Mirror washing→

•In most dirty term, reflectance is affected byLower telescope： ~-10%Upper telescope： ~-5%

•But each reflectance was almost recovered by mirror washing

Measurement pointMeasurement point

PMT uniformity (XY Scanner)

Method of analysis•We adjust position of each PMTs by center of gravity.•After normalization, we add data of each PMTs. (intensity of each LEDs)•This data is normalized by “The average value of each bins inside circle (dia. 36mm) will be 1”. This condition is determined by CRAYS.

XY Scanner•Spot: 4mm•Step: 4mm•8LED

XY Scanner•Spot: 4mm•Step: 4mm•8LED

Comparison with HAMAMATSU measurement → Consistent !

XY Scanner PMT境界

PMT境界

•PMTごとの中心距離は62mm•全体の積分値に対する境界の外の Binの積分値の割合は

境界線の外のBin→ 0.1%境界線上の Bin→ 0.9%

Uniformity:ratio of deviation in each bins

•Evaluation of characteristics of each PMTs.•sigma/mean ratio plot.•Peak value is about 4%. High sensitivity area has this value.•The edge area (low sensitivity) has bigger error ratio.•Inside 90% circle area (dia. 27.5mm), maximum value is 33%, and 95% is less than 10%.

2007/11の鏡洗浄前後のデータ追加

反射率の時間変化による系統誤差の見積もり

時間変化の絵の描き方①, 全データ使用②, 2007/11は一個前の測定データを使用

BRM camera4

赤：①青：②

全ての鏡ごとに①と②を比較し、差が最大となる値を求める。

反射率の時間変化による系統誤差の見積もり 2

BRM,LRの全 432枚の鏡についてのデータ。全データ使用の場合を測定結果とし、 2007/11の補正を入れた場合に対してどの程度反射率が減少するのかを見積もった。

ピークは～ -2%、最大で -7%程度

通常のイベントに対する影響をさっくり見積もる。通常のイベントによる光スポットは、 18枚の鏡を大体均等に使っていると仮定。

→ 18枚の平均値が影響下のカメラで最大 -3.5%、上のカメラで最大 -2%程度。正確な値はシミュレーションで。

反射率の分布

それぞれ 6 点しか測定していないので分布が分からない。各列毎の鏡測定データを集めて、分布を見る。2008/06,LR,上下のカメラ下の図は 360nmの物まぁまぁガウス分布で合っている。→とりあえずガウス分布それぞれの測定値は平均値、標準誤差、標準誤差 /(測定点数 )^0.5の 3 つとする。

100m

FD

Linac

vertical

horizontal

TA-Linac -Basic specs-

Specs of TA-Linac•Particle： e-•Energy： 10, 20, 30, 40 MeV

(variable)•Pulse width： 1μsec •Peak current： 0.16mA

(109e-(=160pC)/pulse)•Frequency： 1Hz•Distance from FD： 100m

Simulated by geant4 (40MeV)

40MeV×109e- @100m → ~1016eV⇔1020 eV @10km

We install this systems in two containers.(movable?)

　　： F.O.V.(upper camera)　　： F.O.V.(lower camera)

We have to prepare power generator and cooling water by ourselves.

Mirror calibration

Image scanner

Light source

mirror

TAMED

Curvature radiusSpot size at curvature radius measured by TAMED

Reflectance (λ dependence)

measured by Spectrophotometer

(Konica-Minolta CM-2500d)

360nm ～ 740nm

Num

ber

of

mir

rors

Num

ber

of

mir

rors

Curvature radius [mm] Spot size @ curvature radius [mm]R

eflect

an

ce [

%]

90

85

360 420Wavelength [mm]

Mirror alignment

All mirrors were adjusted using BANANA-3

BANANA-36067mm

LED

Spot

Laser(center axis)

LED

Spot~20mm

Current 1mip gain distribution

gain distribution(detector): 45±5 count

At under 4*10^6 gain 1mip peak are around 70,(some PMT is more higher).

E. Kido

Typ 570m

Maximum Number of particle

Hit in 20 nsec time bin

as function of distance from core

Typ： at up to 570 m from coreTA can measure with less non-linearity than 5%.

Slide : by M. Chikawa (2007)

TA IR camera

IR data taking sequence

123456

7 8 9 10 11 12

13 14

Once per 50min (3000 sec) 14 pictures in a sequence

•12 directions : 6 lower (12 deg) and 6 upper (30 deg)•Vertical, horizontal

(vertical)(horizontal)

Sometimes there are missing pictures of some directions

•(Instructions (PC -> camera) did not received correctly)•By analyzing PC logs and time stamps of the IR data, missing parts identified.

Year Month Days # Pictures #/day Total

2007 12 2 123 62 123

2008 1 17 1641 97 1764

2 13 1320 102 3084

3 12 1174 98 4258

4 12 1970 164 6228

5 12 2084 174 8312

6 9 537 60 8849

7 7 406 58 9255

8 20 1500 75 10755

9 15 1423 95 12178

10 16 1651 103 13829

11 15 1246 83 15075

12 12 1535 128 16610

2009 1 2 238 119 16848

Statistics2007/Dec/29 - 2009/Jan/04

“Happy Night”Gallery

2008/Nov/06

08:02

08:59

10:03

Fitting result

0 50 100 150 [FADC count]

Fitting result (log arithmetic)

0 100 200 300 [FADC count]