Recent results from Telescope Array

CosPA 2013 Cosmic Rays 11/14

Takeshi Okuda (Ritsumeikan University)
for Telescope Array Collaboration

Outline• Recent Physics Result• Energy Spectrum• Mass Composition• Photon Limit• Anisotropy• Experiment for Extended Energy Region• TA Low Energy Extension• TA High Energy Extension• TA Affiliate ExperimentTelescope Array Collaboration
T. Abu-Zayyada, M. Allena, R. Andersona, R. Azumab, E. Barcikowskia, J. W. Belza, D. R. Bergmana,S. A. Blakea, R. Cadya, M. J. Chaec, B. G. Cheond, J. Chibae, M. Chikawaf, W. R. Chog, T. Fujiih, M. Fukushimah,i,K. Gotoj, W. Hanlona， Y. Hayashij, N. Hayashidak, K. Hibinok, K. Hondal, D. Ikedah, N. Inouem, T. Ishiil,
R. Ishimorib, H. Iton, D. Ivanova,o, C. C. H. Juia, K. Kadotap, F. Kakimotob, O. Kalashevq, K. Kasaharar, H. Kawais,
S. Kawakamij, S. Kawanam, K. Kawatah, E. Kidoh, H. B. Kimd, J. H. Kima, J. H. Kimd, S. Kitamurab, Y. Kitamurab,V. Kuzminq, Y. J. Kwong, J. Lana, J.P. Lundquista, K. Machidal, K. Martensi, T. Matsudat, T. Matsuyamaj,J. N. Matthewsa, M. Minaminoj, K. Mukail, I. Myersa, K. Nagasawam, S. Nagatakin, T. Nakamurau, H. Nanpeij,
T. Nonakah, A. Nozatof, S. Ogioj, S. Ohc, M. Ohnishih, H. Ohokah, K. Okih, T. Okudav, M. Onon, A. Oshimaj,
S. Ozawar, I. H. Parkw, M. S. Pshirkovx, D. C. Rodrigueza, G. Rubtsovq, D. Ryuy, H. Sagawah, N. Sakuraij,
A. L. Sampsona, L. M. Scotto, P. D. Shaha, F. Shibatal, T. Shibatah, H. Shimodairah, B. K. Shind, T. Shirahamam,J. D. Smitha, P. Sokolskya, R. W. Springera, B. T. Stokesa, S. R. Strattona,o, T. A. Stromana, M. Takamurae,
A. Taketaz, M. Takitah, Y. Tamedak, H. Tanakaj, K. Tanakaaa, M. Tanakat, S. B. Thomasa,G. B. Thomsona, P. Tinyakovq,x, I. Tkachevq, H. Tokunob, T. Tomidaab, S. Troitskyq, Y. Tsunesadab, K. Tsutsumib,
Y. Uchihoriac, F. Urbanx, G. Vasiloffa, Y. Wadam, T. Wonga, H. Yamaokat, K. Yamazakij, J. Yangc,K. Yashiroe, Y. Yonedaj, S. Yoshidas, H. Yoshiiad, R. Zollingera, Z. Zundela
aUniversity of Utah, bTokyo Institute of Technology, cEwha Womans University, dHanyang University, eTokyo University of Science,fKinki University, gYonsei University, hInstitute for Cosmic Ray Research, Univ. of Tokyo,
iKavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, the University of Tokyo,
jOsaka City University, kKanagawa University, lUniv. of Yamanashi, mSaitama University, nAstrophysical Big Bang Laboratory, RIKEN,oRutgers University, pTokyo City University, qInstitute for Nuclear Research of the Russian Academy of Sciences, rWaseda University,sChiba University, tInstitute of Particle and Nuclear Studies, KEK, uKochi University, vRitsumeikan University, wSungkyunkwan University,
xUniversite Libre de Bruxelles, yChungnam National University, zEarthquake Research Institute, University of Tokyo,
aaHiroshima City University, abAdvanced Science Institute, RIKEN, acNational Institute of Radiological Science, adEhime University

2013/11/12

Auger collaboratiom meeting3Telescope Array Collaboration
T. Abu-Zayyada, M. Allena, R. Andersona, R. Azumab, E. Barcikowskia, J. W. Belza, D. R. Bergmana,S. A. Blakea, R. Cadya, M. J. Chaec, B. G. Cheond, J. Chibae, M. Chikawaf, W. R. Chog, T. Fujiih, M. Fukushimah,i,K. Gotoj, W. Hanlona， Y. Hayashij, N. Hayashidak, K. Hibinok, K. Hondal, D. Ikedah, N. Inouem, T. Ishiil,
R. Ishimorib, H. Iton, D. Ivanova,o, C. C. H. Juia, K. Kadotap, F. Kakimotob, O. Kalashevq, K. Kasaharar, H. Kawais,S. Kawakamij, S. Kawanam, K. Kawatah, E. Kidoh, H. B. Kimd, J. H. Kima, J. H. Kimd, S. Kitamurab, Y. Kitamurab,
V. Kuzminq, Y. J. Kwong, J. Lana, J.P. Lundquista, K. Machidal, K. Martensi, T. Matsudat, T. Matsuyamaj,J. N. Matthewsa, M. Minaminoj, K. Mukail, I. Myersa, K. Nagasawam, S. Nagatakin, T. Nakamurau, H. Nanpeij,
T. Nonakah, A. Nozatof, S. Ogioj, S. Ohc, M. Ohnishih, H. Ohokah, K. Okih, T. Okudav, M. Onon, A. Oshimaj,S. Ozawar, I. H. Parkw, M. S. Pshirkovx, D. C. Rodrigueza, G. Rubtsovq, D. Ryuy, H. Sagawah, N. Sakuraij,
A. L. Sampsona, L. M. Scotto, P. D. Shaha, F. Shibatal, T. Shibatah, H. Shimodairah, B. K. Shind, T. Shirahamam,J. D. Smitha, P. Sokolskya, R. W. Springera, B. T. Stokesa, S. R. Strattona,o, T. A. Stromana, M. Takamurae,
A. Taketaz, M. Takitah, Y. Tamedak, H. Tanakaj, K. Tanakaaa, M. Tanakat, S. B. Thomasa,G. B. Thomsona, P. Tinyakovq,x, I. Tkachevq, H. Tokunob, T. Tomidaab, S. Troitskyq, Y. Tsunesadab, K. Tsutsumib,
Y. Uchihoriac, F. Urbanx, G. Vasiloffa, Y. Wadam, T. Wonga, H. Yamaokat, K. Yamazakij, J. Yangc,
K. Yashiroe, Y. Yonedaj, S. Yoshidas, H. Yoshiiad, R. Zollingera, Z. Zundela~120 collaborators in 5 countries
Japan, USA, Korea, Russia, Belgium

aUniversity of Utah, bTokyo Institute of Technology, cEwha Womans University, dHanyang University, eTokyo University of Science,fKinki University, gYonsei University, hInstitute for Cosmic Ray Research, Univ. of Tokyo,iKavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, the University of Tokyo,
jOsaka City University, kKanagawa University, lUniv. of Yamanashi, mSaitama University, nAstrophysical Big Bang Laboratory, RIKEN,oRutgers University, pTokyo City University, qInstitute for Nuclear Research of the Russian Academy of Sciences, rWaseda University,sChiba University, tInstitute of Particle and Nuclear Studies, KEK, uKochi University, vRitsumeikan University, wSungkyunkwan University,
xUniversite Libre de Bruxelles, yChungnam National University, zEarthquake Research Institute, University of Tokyo,
aaHiroshima City University, abAdvanced Science Institute, RIKEN, acNational Institute of Radiological Science, adEhime University

2013/11/12

Auger collaboratiom meeting

4Telescope Array Site

MDFD Utah State in USA

39.3N, 112.9W, Alt 1400[m]

SKCT32.4km
Surface Detector (SD)

CLF

Telecommunication
Tower

27.6kmLRFD LRCTBRCT
507 SDs

Fluorescence Detector (FD)BRFD

5 year SD data

Mass Composition
4 year MD hybrid data

QGSJET-Ⅱ

Mass Composition

5 year BR/LR stereo dataPhoton Upper Limit
The photon likelihood of theobserved shower is evaluated byshower front curvature by SD.
For 5 years SD data, we got thephoton upper limit for which
estimated energy is more than 1019eV.

θ=53.6deg

45deg < θ < 60deg
E>1019eV
45deg < θ < 60deg

Data
PhotonMCCurvatureAnisotropy (Nearby AGN)
AGNs are from VCV 2006 catalog, cut by z (0 ＜ z ≦ 0.18).
There are 465 AGN in our field of view.
Primary Energy ＞ 57EeV, Angular Separation ＜ 3.1°.

17 events correlate out of 42 events.
This probability is 0.014 from chance correlation.

Anisotropy (Auto-correlation)
AGASA reported clustering within 2.5°for energy ＞ 40EeV.
TA found no clustering within 2.5°.
Extended search for larger angles δ and higher energy.

Anisotropy (LSS)
Composition measured by TA
is consistent with proton.

Data (white point)
and Model distribution(shaded region) from LSS
within 100Mpc.

When deflection angle θ
set to 6°, p-value ofisotropy is 0.001 .

Physics Summary

Significance of the five-year
SD spectrum suppression is 5.7σ.
Mass composition is consistent with proton.
Arrival direction at high energy seems
inconsistent with isotropic distribution.

To Extended and Affiliate Experiment

TA Low Energy Extension (TALE)Basically it uses same method as TA, relatively specific for hybrid
observation. The observing energy range is down to 10 17eV (LHC).

Partially installed and operating.
Now, proposing full construction.

Non-Imaging CHErenkov array (NICHE)This is the plan of low
energy extension for TALE,
whose energy range down to1016eV for 200m spacing. The
main purpose is composition
study by Cherenkov pulsewidth, working with TALE.

TA High Energy Extension (TAx4)
Basically it uses same method as TA, with a FD and 3 times larger
coverage area by SDs. SD full area can not be covered by FD field ofview.
This experiment is mainly
for anisotropy study,
This is for detecting
more cosmic rays whichhave energy over GZK. If
they are proton, theirsource is within 50Mpc.
From our current resultof the inconsistency withisotropy at high energy
region, we are halfway tocatching a clue?
Now, proposing construction.

TA Affiliate Experiment
Prototype EUSO at TA

TARA

Reported this morning.

TA Affiliate Experiment
Prototype EUSO at TA

TARA

Reported this morning.
TA Lightning Mapping Array (TALMA)
Test InstallationLMA event display example
LMA can measure the origin of sferics in the lightning
process with high resolution of time and position.

Why TA try to install LMA?

Because TASD observed the bursts of shower like events,
which are correlated with lightning.
From five years TASD data,
there are 10 bursts ofshower trigger. The burst
criteria is 3 shower trigger
in 1 millisecond. The chance
expectation for five years
is less than 10-4.

Because TASD observed the bursts of shower like events,
which are correlated with lightning.
From five years TASD data,
there are 10 bursts ofshower trigger. The burst
criteria is 3 shower trigger
in 1 millisecond. The chance
expectation for five years
is less than 10-4.
Some events in 5 bursts pass
the reconstruction.

datetimeusec
X[m]AS 101004 165842 930565 11356
AS 101004 165842 930612 10478
AS 101004 165842 930835 11142

Y[m]
-7425
-7368
-8159

AS 110727 080615 124319
AS 110727 080615 124543

3447
2897

1952
2232

AS 110916 194056 567481
AS 110916 194056 567566

-3210
-3524

-9285
-9413

AS 120706 014911 184219
AS 120706 014911 184307

9847 -10702
7635 -9674

AS 120907 015545 380684
AS 120907 015545 380755
AS 120907 015545 380881

-8636
-9857
-9450

1254
-337
-961

Because TASD observed the bursts of shower like events,
which are correlated with lightning.
From five years TASD data,
there are 10 bursts ofshower trigger. The burst
criteria is 3 shower trigger
in 1 millisecond. The chance
expectation for five years
is less than 10-4.
Some events in 5 bursts pass
the reconstruction.
These bursts are selected
only by timing, but theircore position is very close.
In addition, thesereconstructed shower front
is very curved compared withnormal shower. They seems
start shower development atlow sky.

datetimeusec
X[m]AS 101004 165842 930565 11356
AS 101004 165842 930612 10478
AS 101004 165842 930835 11142

Y[m]
-7425
-7368
-8159

AS 110727 080615 124319
AS 110727 080615 124543

3447
2897

1952
2232

AS 110916 194056 567481
AS 110916 194056 567566

-3210
-3524

-9285
-9413

AS 120706 014911 184219
AS 120706 014911 184307

9847 -10702
7635 -9674

AS 120907 015545 380684
AS 120907 015545 380755
AS 120907 015545 380881

-8636
-9857
-9450

1254
-337
-961

BurstNormalBurst

Particle Hit Map
Left plots are burst events.
Right plot is a typical (normal)
event whose zenith angle isalmost same as left two eventsand its shower size is middle ofleft two events.

BurstNormalLateral Number of Particle
Burst

Left plots are burst events.
Right plot is a typical (normal)
event whose zenith angle isalmost same as left two eventsand its shower size is middle ofleft two events.

BurstNormalLateral Arrival Timing
Burst

Left plots are burst events.
Right plot is a typical (normal)
event whose zenith angle isalmost same as left two eventsand its shower size is middle ofleft two events.
Left plots’shower front is much
more curved than Right plot.

BurstNormalWaveforms
Burst

Left plots are burst events.
Right plot is a typical (normal)
event whose zenith angle isalmost same as left two eventsand its shower size is middle ofleft two events.
Left plots’waveforms have lesssharp rising edge than Right plot.

Correlation with Lightning Data from NLDN.
National Lightning Detection Network detects lightning by VLF.
The lighting list contains lightning time, 2D coordinates, peakcurrent and flag which indicates whether intracloud lightning or
cloud-ground lightning.

NLDN is somewhat inefficientfor intracloud lightning.

I defined “synchronized”
lightning is the timedifference within ±1[ms]from burst.
I defined “related”
lightning is the timedifference within ±200[ms]from burst excecpt forsynchronized lightning.

TAAS
LG

date
date

time
time

usec
usec

X[m]
X[m]

Y[m]
Y[m]

H[m]
Flag

AS 101004 165842 930565
AS 101004 165842 930612
AS 101004 165842 930835
LG 101004 165842 930608
LG 101004 165842 934058

11356
10478
11142
12480
10619

-7425
-7368
-8159
-5068
-8069

3963
4400
3270
CG

AS 110727 080615 124319
AS 110727 080615 124543
LG 110727 080615 124303
LG 110727 080615 130887

3447
2897
3653
3084

1952
2232
2285
1996

4070
3070
CG

AS 110916 194056 567481
AS 110916 194056 567566

-3210
-3524

-9285
-9413

3253
3134

AS 120706 014911 184219
AS 120706 014911 184307
LG 120706 014911 184122

9847 -10702
7635 -9674
8997 -9670

3770
3361
CAS 120907 015545 380684
AS 120907 015545 380755
AS 120907 015545 380881
LG 120907 015545 380675
LG 120907 015545 390411
LG 120907 015545 409370

-8636
-9857
-9450
-8942
-9635
-8608

4446
4805
3361
CG
G

1254
-337
-961
668
-1952
-1653

Correlation with Lightning
Data from NLDN.
There are 4 correlations in 5reconstructed bursts.
This is good correlation withconsidering NLDN detection
efficiency.
AS line shows TASD event.
LG line shows NLDN event.

ASLG

date
date

timetime

usec
usec

X[m]
X[m]

Y[m]
Y[m]

H[m]
Flag

AS 101004 165842 930565
AS 101004 165842 930612
AS 101004 165842 930835
LG 101004 165842 930608
LG 101004 165842 934058

11356
10478
11142
12480
10619

-7425
-7368
-8159
-5068
-8069

3963
4400
3270
CGAS 110727 080615 124319
AS 110727 080615 124543
LG 110727 080615 124303
LG 110727 080615 130887

3447
2897
3653
3084

1952
2232
2285
1996

4070
3070
CG

AS 110916 194056 567481
AS 110916 194056 567566

-3210
-3524

-9285
-9413

3253
3134

AS 120706 014911 184219
AS 120706 014911 184307
LG 120706 014911 184122

9847 -10702
7635 -9674
8997 -9670

3770
3361
CAS 120907 015545 380684
AS 120907 015545 380755
AS 120907 015545 380881
LG 120907 015545 380675
LG 120907 015545 390411
LG 120907 015545 409370

-8636
-9857
-9450
-8942
-9635
-8608

4446
4805
3361
CG
G

1254
-337
-961
668-1952-1653

Correlation with Lightning
Data from NLDN.
There are 4 correlations in 5
reconstructed bursts.
This is good correlation withconsidering NLDN detection
efficiency.
AS line shows TASD event.
LG line shows NLDN event.

These correlations are taken
only by timing, but thelocations of bursts andlightning are also correlated
very well.

ASLG

date
date

time
time

usec
usec

X[m]
X[m]

Y[m]
Y[m]

H[m]
Flag

AS 101004 165842 930565
AS 101004 165842 930612
AS 101004 165842 930835
LG 101004 165842 930608
LG 101004 165842 934058

11356
10478
11142
12480
10619

-7425
-7368
-8159
-5068
-8069

3963
4400
3270
CG

AS 110727 080615 124319
AS 110727 080615 124543
LG 110727 080615 124303
LG 110727 080615 130887

3447
2897
3653
3084

1952
2232
2285
1996

4070
3070
CG

AS 110916 194056 567481
AS 110916 194056 567566

-3210
-3524

-9285
-9413

3253
3134

AS 120706 014911 184219
AS 120706 014911 184307
LG 120706 014911 184122

9847 -10702
7635 -9674
8997 -9670

3770
3361
CAS 120907 015545 380684
AS 120907 015545 380755
AS 120907 015545 380881
LG 120907 015545 380675
LG 120907 015545 390411
LG 120907 015545 409370

-8636
-9857
-9450
-8942
-9635
-8608

4446
4805
3361
C
G
G

1254
-337
-961
668
-1952
-1653

Correlation with Lightning
Data from NLDN.
There are 4 correlations in 5
reconstructed bursts.
This is good correlation withconsidering NLDN detection
efficiency.
AS line shows TASD event.
LG line shows NLDN event.

79% of the NLDN lightning datahave flag “G(cloud-ground)”.
However, all synchronized 4
lightning strokes have flag“C(intracloud)”. And all
related subsequent strokes
have flag “G(cloud-ground)”.

High Energy Radiation Shower Geometry with Lightning
Color shows the height from ground up to 3000m.
Red point shows shower core hit position.
Circle shows lightning position with 300m radius.
I set “Synchronized(intracloud)” lightning at 3000m,
and “Related(cloud-ground)” lightning at 0m.

We are planing to install our Lightning Mapping Array (LMA) to study
more detail correlation between high energy radiation and lightning.
We need fund for TALMA.

Summary
Some Extended Experiments
andSome Affiliate Experiments
are planned and going on.

EndThank You

BackupSurface Detector
Particle Detection Part:
2 layers of 3m2×1.2cm plastic scintillators.
104 Wave Length Shifting Fibers for each layer.

Electronics:
50MHz FADC
Charge Controller
GPS
Wireless LAN

Data Acquisition:
Shower Trigger is generated by adjacent 3SDs whose signal isover 3MIPs in 8μs.
Waveforms for all SD within 32μs from shower trigger time.

Scatter plot of H with Energy or Zenith (080511-100907)

Events (E>6.36EeV && Zen<55deg)
with H (the altitude of thespherical center for shower front)
less than 6000 are very few.