最高エネルギー宇宙線による極限宇宙観測（研究会 高エネルギーガンマ線で見る極限宇宙２０１４）

野中敏幸
東京大学宇宙線研究所
Ｔｅｌｅｓｃｏｐｅ Ａｒｒａｙ Ｃｏｌｌａｂｏｒａｔｉｏｎ

Highest energy cosmic ray observation
Cosmic ray energy spectrum 1015eV – 1020eVSpectrum index
Composition change

Knee
2nd Knee

Source transition fromgalactic - extragalactic

Dip - Ankle
Cut off

Highest energy
1019eV~
ELHC

1015eV

1017eV

1event /km2・year

1019eV高エネルギーガンマ線で見る極限宇宙２０１４

extragalactic origin.
(larmor radius )2

Candidate of source
Hillas Diagram
Hillas condition.
E∝ BxL
Necessary condition fromcosmic ray energy
several types of objects remainas source “candidate”.

How to infer the source..

Kotera & Olinto, Ann. Rev. Astron. Astrophys (2010)

Direction (anisotropy )Spectrum
Composition…

高エネルギーガンマ線で見る極限宇宙２０１４3

Anisotropy◇ Trajectory of cosmic ray in galactic magnetic field.

1018eV1019eV(Few degree)
1020eV

Using arrival direction, it is possible to searchcorrelation with Source position
Inter galactic magnetic field:
generally random field. B < ~10-9G
Few degree
高エネルギーガンマ線で見る極限宇宙２０１４4

Spectrum
Spectrum modulation from single source

P+γ-> Δ Ｐ+π
ＧＺＫ effect
V.Berezinsky et.al Phys. Rev. D 74, 043005 (2006)

高エネルギーガンマ線で見る極限宇宙２０１４5

TA experiment ,Observation results

Telescope Array Experiment
Location: N39.3°W112.9°
1350-1500m asl

FD station (× 3station)○Surface Array (507 SD)△Communication tower
1.2 km grid SD (3m2 )● 3 sub array :+cross boundary trigger
Total 507 SD● Total detection area ～700ｋ㎡
●FDSD

27Km
高エネルギーガンマ線で見る極限宇宙２０１４7

Observation of highest cosmic ray
Shower development
 N⇔ Energy
maxXmax ⇔ Composition

SD :Lateral Distribution, ⇔ Energy

高エネルギーガンマ線で見る極限宇宙２０１４8Telescope Array Collaboration
T. Abu-Zayyad1, R. Aida2, M. Allen1, T. Arai4, R. Azuma3, E. Barcikowski1, J.W. Belz1,T. Benno4, D.R. Bergman5, S.A. Blake1,O. Brusova1, R. Cady1, B.G. Cheon6, J. Chiba7, M. Chikawa4, E.J. Cho6, L.S. Cho8, W.R. Cho8, F. Cohen9, K. Doura4, C. Ebeling1,H. Fujii10, T. Fujii11, T. Fukuda3, M. Fukushima9􀀀􀀀22, D. Gorbunov12, W. Hanlon1, K. Hayashi3, Y. Hayashi11, N. Hayashida9, K. Hibino13,K. Hiyama9, K. Honda2, G. Hughes5, T. Iguchi3, D. Ikeda9, K. Ikuta2, S.J.J. Innemee5, N. Inoue14, T. Ishii2, R. Ishimori3, D. Ivanov5,S. Iwamoto2, C.C.H. Jui1, K. Kadota15, F. Kakimoto3, O. Kalashev12, T. Kanbe2, H. Kang16, K. Kasahara17, H. Kawai18, S. Kawakami11,
S. Kawana14, E. Kido9, B.G. Kim19,H.B. Kim6, J.H. Kim6, J.H. Kim20, A. Kitsugi9, K. Kobayashi7, H. Koers21, Y. Kondo9, V. Kuzmin12,Y.J. Kwon8, J.H. Lim16, S.I. Lim19, S. Machida3, K. Martens22, J. Martineau1, T. Matsuda10, T. Matsuyama11, J.N. Matthews1,M. Minamino11, K. Miyata7, H. Miyauchi11, Y. Murano3, T. Nakamura23, S.W. Nam19, T. Nonaka9, S. Ogio11, M. Ohnishi9, H. Ohoka9,T. Okuda11, A. Oshima11, S. Ozawa17, I.H. Park19, D. Rodriguez1, S.Y. Roh20, G. Rubtsov12, D. Ryu20, H. Sagawa9,N. Sakurai9, L.M. Scott5,P.D. Shah1, T. Shibata9, H. Shimodaira9, B.K. Shin6, J.D. Smith1, P. Sokolsky1, T.J. Sonley1, R.W. Springer1, B.T. Stokes5, S.R. Stratton5,S. Suzuki10, Y. Takahashi9, M. Takeda9, A. Taketa9, M. Takita9, Y. Tameda3, H. Tanaka11, K. Tanaka24, M. Tanaka10, J.R. Thomas1,S.B.Thomas1, G.B. Thomson5, P. Tinyakov12􀀀􀀀21, I. Tkachev12, H. Tokuno9, T. Tomida2, R. Torii9, S. Troitsky12, Y. Tsunesada3, Y.
Tsuyuguchi2, Y. Uchihori25, S. Udo13, H. Ukai2, B. Van Klaveren1, Y. Wada14, M. Wood1, T. Yamakawa9, Y. Yamakawa9, H. Yamaoka10,J. Yang19, S. Yoshida18, H. Yoshii26, Z. Zundel1
1University of Utah, High Energy Astrophysics Institute, Salt Lake City, Utah, USA

14Saitama University, Saitama, Saitama, Japan

2University of Yamanashi, Interdisciplinary Graduate School of Medicine and15Tokyo City University, Setagaya-ku, Tokyo, Japan

Engineering, Kofu, Yamanashi,
Japan
3Tokyo Institute of Technology, Meguro, Tokyo, Japan
4Kinki Unversity, Higashi Osaka, Osaka, Japan
5Rutgers University, Piscataway, USA
6Hanyang University, Seongdong-gu, Seoul, Korea
7Tokyo University of Science, Noda, Chiba, Japan8Yonsei University, Seodaemun-gu, Seoul, Korea
9Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba, Japan
10Institute of Particle and Nuclear Studies, KEK, Tsukuba, Ibaraki, Japan
11Osaka City University, Osaka, Osaka, Japan
12Institute for Nuclear Research of the Russian Academy of Sciences, Moscow,Russia
13Kanagawa University, Yokohama, Kanagawa, Japan

16Pusan National University, GeumJeong-gu, Busan, Korea
17Waseda University, Advanced Research Institute for Science and Engineering,
Shinjuku-ku, Tokyo, Japan
18Chiba University, Chiba, Chiba, Japan
19Ewha Womans University, Seodaaemun-gu, Seoul, Korea
20Chungnam National University, Yuseong-gu, Daejeon, Korea
21University Libre de Bruxelles, Brussels, Belgium
22University of Tokyo, Institute for the Physics and Mathematics of the Universe,Kashiwa, Chiba, Japan
23Kochi University, Kochi, Kochi, Japan
24Hiroshima City University, Hiroshima, Hiroshima, Japan
25National Institute of Radiological Science, Chiba, Chiba, Japan
26Ehime University, Matsuyama, Ehime, Japan高エネルギーガンマ線で見る極限宇宙２０１４

9Telescope Array Collaboration
T. Abu-Zayyad1, R. Aida2, M. Allen1, T. Arai4, R. Azuma3, E. Barcikowski1, J.W. Belz1,T. Benno4, D.R. Bergman5, S.A. Blake1,O. Brusova1, R. Cady1, B.G. Cheon6, J. Chiba7, M. Chikawa4, E.J. Cho6, L.S. Cho8, W.R. Cho8, F. Cohen9, K. Doura4, C. Ebeling1,H. Fujii10, T. Fujii11, T. Fukuda3, M. Fukushima9􀀀􀀀22, D. Gorbunov12, W. Hanlon1, K. Hayashi3, Y. Hayashi11, N. Hayashida9, K. Hibino13,
K. Hiyama9, K. Honda2, G. Hughes5, T. Iguchi3, D. Ikeda9, K. Ikuta2, S.J.J. Innemee5, N. Inoue14, T. Ishii2, R. Ishimori3, D. Ivanov5,S. Iwamoto2, C.C.H. Jui1, K. Kadota15, F. Kakimoto3, O. Kalashev12, T. Kanbe2, H. Kang16, K. Kasahara17, H. Kawai18, S. Kawakami11,S. Kawana14, E. Kido9, B.G. Kim19,H.B. Kim6, J.H. Kim6, J.H. Kim20, A. Kitsugi9, K. Kobayashi7, H. Koers21, Y. Kondo9, V. Kuzmin12,Y.J. Kwon8, J.H. Lim16, S.I. Lim19, S. Machida3, K. Martens22, J. Martineau1, T. Matsuda10, T. Matsuyama11, J.N. Matthews1,M. Minamino11, K. Miyata7, H. Miyauchi11, Y. Murano3, T. Nakamura23, S.W. Nam19, T. Nonaka9, S. Ogio11, M. Ohnishi9, H. Ohoka9,T. Okuda11, A. Oshima11, S. Ozawa17, I.H. Park19, D. Rodriguez1, S.Y. Roh20, G. Rubtsov12, D. Ryu20, H. Sagawa9,N. Sakurai9, L.M. Scott5,P.D. Shah1, T. Shibata9, H. Shimodaira9, B.K. Shin6, J.D. Smith1, P. Sokolsky1, T.J. Sonley1, R.W. Springer1, B.T. Stokes5, S.R. Stratton5,S. Suzuki10, Y. Takahashi9, M. Takeda9, A. Taketa9, M. Takita9, Y. Tameda3, H. Tanaka11, K. Tanaka24, M. Tanaka10, J.R. Thomas1,S.B.Thomas1, G.B. Thomson5, P. Tinyakov12􀀀􀀀21, I. Tkachev12, H. Tokuno9, T. Tomida2, R. Torii9, S. Troitsky12, Y. Tsunesada3, Y.
Tsuyuguchi2, Y. Uchihori25, S. Udo13, H. Ukai2, B. Van Klaveren1, Y. Wada14, M. Wood1, T. Yamakawa9, Y. Yamakawa9, H. Yamaoka10,J. Yang19, S. Yoshida18, H. Yoshii26, Z. Zundel1
1University of Utah, High Energy Astrophysics Institute, Salt Lake City, Utah, USA

14Saitama University, Saitama, Saitama, Japan

2University of Yamanashi, Interdisciplinary Graduate School of Medicine and15Tokyo City University, Setagaya-ku, Tokyo, Japan

Engineering, Kofu, Yamanashi,
Japan
3Tokyo Institute of Technology, Meguro, Tokyo, Japan
4Kinki Unversity, Higashi Osaka, Osaka, Japan
5Rutgers University, Piscataway, USA
6Hanyang University, Seongdong-gu, Seoul, Korea
7Tokyo University of Science, Noda, Chiba, Japan
8Yonsei University, Seodaemun-gu, Seoul, Korea
9Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba, Japan
10Institute of Particle and Nuclear Studies, KEK, Tsukuba, Ibaraki, Japan
11Osaka City University, Osaka, Osaka, Japan
12Institute for Nuclear Research of the Russian Academy of Sciences, Moscow,Russia
13Kanagawa University, Yokohama, Kanagawa, Japan

16Pusan National University, GeumJeong-gu, Busan, Korea
17Waseda University, Advanced Research Institute for Science and Engineering,
Shinjuku-ku, Tokyo, Japan
18Chiba University, Chiba, Chiba, Japan
19Ewha Womans University, Seodaaemun-gu, Seoul, Korea
20Chungnam National University, Yuseong-gu, Daejeon, Korea
21University Libre de Bruxelles, Brussels, Belgium
22University of Tokyo, Institute for the Physics and Mathematics of the Universe,
Kashiwa, Chiba, Japan
23Kochi University, Kochi, Kochi, Japan
24Hiroshima City University, Hiroshima, Hiroshima, Japan
25National Institute of Radiological Science, Chiba, Chiba, Japan
26Ehime University, Matsuyama, Ehime, Japan

USA Belgium Japan Korea Russia
Total 26Institutes ~140 collaborators.
高エネルギーガンマ線で見る極限宇宙２０１４10

Fluorescence Detectors
From HiRes

Middle Drum

14 cameras/station
256 PMTs/camera

5.2 m2~30km

New FDs
256 PMTs/camera
HAMAMATSU R9508
FOV~15x18deg
12 cameras/station

Long Ridge

Black Rock Mesa

高エネルギーガンマ線で見る極限宇宙２０１４~1 m2

6.8 m21111

FD event example
Energy estimation

光量Ti (αi ,ψ , R)

Use SD timing information
Ψ、R resolution improve (Hybrid analysis)
高エネルギーガンマ線で見る極限宇宙２０１４12TA Surface Detector
3㎡12mm Plastic Scinti.
1mm SS steel plate
Up/Low 2 independent
12mm Plastic Scinti.
layer.
reflector :TyvekWls fiber (475nm ) x5m  PMT ETL9124SA

Solarcell

１０００ｍ － １２５０ｍ

TASD
Energy Dep.(Arb unit)＋ BatteryWireless LAN (2.4GHz)
ＧＰＳ syncronization ~20nsec
Sample rate 50Msps FADC
1.2km square grid array.

Simulated energy deposit
1019eV proton shower (stacked signal)(1μ sec)
高エネルギーガンマ線で見る極限宇宙２０１４time (nsec)
13SD event example
2008/Jun/25 - 19:45:52.588670 UTC

Particle arrival time  shower direction

横方向分布フィットより求める。

S800

S(800)（Primary Energy）

r = 800m

高エネルギーガンマ線で見る極限宇宙２０１４14

Energy spectrum at E>1018.2eV
 Period :2008 May – 2014 May(6 years)◇ 6year TA SD spectrum

 Cut conditions :- # of used detectors >=5- Zenith angle < 45°- Energy > 1018.2eV- w boundary cut Dip energy EdLog10(Ed/eV) = 18.70±0.02
 Break energy Eb
Log10(E b/eV) = 19.74±0.04
 Consistent with GZK cut off Significance of suppression@ E >1019.8eV
Nexp = 85.9
Nobs = 32  6.59 σ
D.Bergman @COSPA 2014
高エネルギーガンマ線で見る極限宇宙２０１４15

Energy spectrum at E>1018.2eV◇ Comparison with Auger spectrum◇ Energy scale shifted artificiallyat Auger x 1.1◇ spectrum shape agree wellat Dip region (1018.5eV)start disagree E> 1019.6eV◇ Plot is from 2013 ICRC.
TA spectrum shape is almost
same in updated data.
◇ Study of Declination dependenceof the spectrum is on going.

ICRC2013 Y.Tsunesada(Collaboration study between Auger-TA)

高エネルギーガンマ線で見る極限宇宙２０１４16

Cosmic ray model E>1018.2eV
5year TA SD spectrum
Composition: Proton.
Evolution index m:ρ ∝ (1+z)m
Spectrum index origin ｐ:
dN/dE ∝ E-PPropagation :Karashev , E.Kido
arXiv:1406.0735
Back gorund photon
CMB, IRB- No magnetic field
E.Kido JPS meeting Sep. 2014

Search best fit parameter-p , m ,Δlog10(E) , Cn*
Cn* (normalization factor)
高エネルギーガンマ線で見る極限宇宙２０１４17

Modeling source distribution E>1018.2eV<Best fit source parameter (*uniform)>
P=2.21m = 6.4
ΔLogE -0.04* (uniform)
Zmin :
Distance of closest source in the model
Increase Zmin to find 95% incompatibility
between model spectrum and data point.

E.Kido JPS meeting Sep. 2014

Data compatible with pure proton model at E>1018.2eV
Under the condition of best fit model , constraint on Zmin:
Zmin < 0.010 (～40 Mpc) in 95% C.L.
高エネルギーガンマ線で見る極限宇宙２０１４18

New result from TA Low energy Extension◇ (TALE SD is under construction)◇ Period : 2013/09/06 - 12/06

TALE detector :High elevation tel + density SD Low energy hybrid

144hr data
◇ SDs are not used ,not hybrid analysis◇ Break @ 1016.2 eV
1017.3 eV found.
 Interesting to see Xmax elongation.
Need more SD
高エネルギーガンマ線で見る極限宇宙２０１４19

Anisotropy of Cosmic Rays E>57EeV
 Period :2008 May – 2013 May(5 years) Cut conditions :- # of used detectors >=4- Zenith angle < 55°- Energy > 57EeV- No boundary cut

72 events

Resolutions

Inner

Outer

Angular

1.0°

1.7°

Energy15%

20%

Full event table is available in the ApJL online journal :http://iopscience.iop.org/2041-8205/790/2/L21/suppdata/apjl498370t1_mrt.txt
20Anisotropy of Cosmic Rays E>57EeV

Count number of event within 20°circle

R.A, Dec =(146.7°, 43.2°) 5.1σ

Random 72 events
assuming isotropy(TA geometrical exposure)
Adopt same analysis &create significance maps
(by five oversampling radius: 15, 20, 25, 30, 35 deg.)
Search for maximum
significance in the FoV

P = 371 / 106 trials= 3.7 x 10-4 (3.4σ)“hotspot”
ApJ 790, L21 (2014)

Figure ‘ｓ comment:
K.Kawata ICRR seminar
21

Anisotropy of Cosmic Rays E>57EeV◇ Eye comparison with 2MASS catalog① Ursa Major Cluster(20Mpc)② Virgo Cluster(20Mpc)③Perseus-Pisces Supercluster(70Mpc)◇ Hot spot is not on SGP orGalaxy cluster◇ “Perseus” close to event cluster
but the area’s
significance is ~2σMore quantitative study
is needed.
John P. Huchra et al.
2012 ApJS 199 26
22

Anisotropy of Cosmic Rays E>57EeV
How it looks at south hemisphere with same analysis?
 No adjustment energy scale
Use original energy at bothexperiment Cen-A region enhancement~3σ Virgo cluster position is notbright at Auger data also.
(~20MPC)

Hotspot cosmic ray comes fromvery close distance like Cen-A?

From Slide H.Sagawa @ JPS symposium 09/22 2014

Is it consist from single source?
or coincidence of two source?
If consist from single source
why very large structure? 20°?

高エネルギーガンマ線で見る極限宇宙２０１４23

Chemical composition from Xmax
 Period :2008 May – 2014 May(5 years)
MD station + TASD (Hybrid analysis) arXiv:1408.1726(pattern recognition cut -> better resolution of Xmax)

Xmax distribution and comparison withProton, Iron MC simulation

Average Xmax along energy◇ Consistent with proton.
◇ Inconsistent with Iron
◇ Hot spot E>10*19.7 eV
Xmax : E>1019.4 eV statistics small！
高エネルギーガンマ線で見る極限宇宙２０１４24

Look for other information
NAGN (vcv12-auger)

More close object“On”

Number of AGNs
In VCV list.
(Z<0.018)

Less colse object”Off”

Lat in SG coordinate
Observation condition:
Distribution of relative exposure
at horizontal
coordinate

Diffence <～4%

◎Divide sky|SGP lat |< 30 and >30(exposure 52 : 48)“ ½, and ½ “◎Observation conditionis almost equal.

Horizontal coordinate ・zenithangle
高エネルギーガンマ線で見る極限宇宙２０１４25

Analysis for spectrum difference b/w Sky area
Preliminary result :Number of Chance events ineach area

SGP 30 deg
Area

Number offraction
cases①41580 0.831766②7996 0.159952

X1(scanpenalty)

6.2x10-4③31④383 0.007662

Data
Off source spectrum:
Break energy is small at off source sky 1019.66 eV

高エネルギーガンマ線で見る極限宇宙２０１４26

Summary
Anisotropy
Hotspot found E>57EeV
 More event to resolve structure of Hot spot.
More spot , Composition study with SD,

TAx4Spectrum shape
Dip at 1018.5eV  e+ e- energy loss - >Dip
Cut off at 1019.7eV  consistent with GZKComparison between Sky area (new)Composition
E>1018.2eV consistent with proton,(E>1019.4eV need more statistics)
TALETALE
Start Data taking ,Obtain spectrum E > 1017eV structure in spectrum .
Need more SD area for good resolution Xmax (w Hybrid)
高エネルギーガンマ線で見る極限宇宙２０１４27

6-Year Data by TA

Out of FoV

5-year data
New 1-year data

Our FoV (Dec>-10°)
Definition in ApJL

Slide K.Kawata @ ICRR seminar

Period:2008 May 11 – 2014 May 11 (87 events)

28Significance Map 6 years
Oversampling with 20°-radius circle

Slide K.Kawata @ ICRR seminar
Max significance 5.55σ (Non = 23, Nbg=5.49)
Centered at R.A=148.4°, Dec.=44.5° (shifted from SGP by 17°)
29
Chance probability of appearing in isotropic sky  4.0σ

TAx4
 Plan to expand TA by 4 times(3,000km2)
1. Add 500 scint. counterswith 2.1 km spacing
2. 10 refurbished HiRes tels
 Science (3-year observation)
1. Anisotropy study
 Expect >>5σ
2. Xmax & E Spectrumat the highest energy region
3. Search UHE photon & neutrino
4. correlation search with Otherobservation. :ex) Fang, Fujii, Linden & Olinto, arXiv:1404.6237(IceCube event x TA Hot spot.)
Slide K.Kawata @ ICRR seminar高エネルギーガンマ線で見る極限宇宙２０１４30

TALE

高エネルギーガンマ線で見る極限宇宙２０１４31

Summary
Anisotropy
Hotspot found E>57EeV
 More event to resolve structure of Hot spot.
Composition study with SD,

TAx4

Spectrum shape
Dip at 1018.5eV  e+ e- energy loss - >Dip
Cut off at 1019.7eV  consistent with GZKComparison between Sky area (new)Composition
E>1018.2eV consistent with proton,(E>1019.4eV need more statistics)
TALETALE
Start Data taking ,Obtain spectrum E > 1017eV structure in spectrum .
Need more SD area for good resolution Xmax (w Hybrid)
高エネルギーガンマ線で見る極限宇宙２０１４32

高エネルギーガンマ線で見る極限宇宙２０１４33

Back up

高エネルギーガンマ線で見る極限宇宙２０１４34

Other type of observation
Fang, Fujii, Linden & Olinto, arXiv:1404.6237

UHECRs + photons  TeV-PeV Neutrinos
TA hotspot
IceCubeν > 30TeV(Circle size:Ang. Resol.)Two IceCube neutrinos among northern 4 events arecoincident with the TA hotspot.  2σ level by chance35銀河系外宇宙線源の進化パラメーターρ 1+z)m1020eVではz=0.05
1018eVではz=11017eVではz=4の宇宙線源が寄与する

D.R. Bergman et al. (2006)

E3J/1024 [eV2m-2sr-1s-1]

進化パラメーター：m

進化パラメーターの違い
m = 2.15
2.55
2.95
γ = 2.384

D.R. Bergman, et al., arXiv:astro-ph/0603.797(2006)

E3J/1024 [eV2m-2sr-1s-1]

log10E[eV] 18

192120スペクトルのベキの違い
m = 2.55
γ = 2.334
2.384
2.434
171819203621

Map ofand Eb at random distribution

Simulation:1)Create On/Off distribution from same population
2) Calculate Eb andat likelihood minimum
collect simulation events

exposure ratio=0.52 (SGP 30)
104 simulation
X : Eb obtained at Off source side
Y : Fraction at off source side+

Our data is around here

Here, Eb is off source Eb
高エネルギーガンマ線で見る極限宇宙２０１４37

Count chance cases
Preliminary Result :Number of Chance events in each area
Total 4.999 x 104

Area

Number offraction
events①41580 0.831766②7996 0.159952
6.2x10-4③31④383 0.007662

高エネルギーガンマ線で見る極限宇宙２０１４

SGP 30 deg
X1(scan penalty)

38