ta 4 - telescope array projectuhecr14.telescopearray.org/sagawa/20141015-tax4-v5.pdf · ta×4 h....

TA×4

H. SagawaInstitute for Cosmic Ray Research

The University of Tokyofor Telescope Array collaboration

12014/10/13 H. Sagawa@UHECR2014

Outline

2014/10/13 H. Sagawa@UHECR2014 2

Telescope Array (TA)

Recent TA results5- or 6-year data

Outline

2014/10/13 H. Sagawa@UHECR2014 3

Telescope Array (TA)

Recent TA results5- or 6- year data

TA×4extension

Telescope Array Collaboration

4

R.U. Abbasi1, M. Abe13, T.Abu-Zayyad1, M. Allen1, R. Anderson1, R. Azuma2, E. Barcikowski1, J.W. Belz1,D.R. Bergman1, S.A. Blake1, R. Cady1, M.J. Chae3, B.G. Cheon4, J. Chiba5, M. Chikawa6, W.R. Cho7, T. Fujii8,

M. Fukushima8,9, T. Goto10, W. Hanlon1, Y. Hayashi10, N. Hayashida11, K. Hibino11, K. Honda12, D. Ikeda8,N. Inoue13, T. Ishii12, R. Ishimori2, H. Ito14, D. Ivanov1, C.C.H. Jui1, K. Kadota16, F. Kakimoto2, O. Kalashev17,

K. Kasahara18, H. Kawai19, S. Kawakami10, S. Kawana13, K. Kawata8, E. Kido8, H.B. Kim4, J.H. Kim1, J.H. Kim25, S. Kitamura2, Y. Kitamura2, V. Kuzmin17, Y.J. Kwon7, J. Lan1, S.I. Lim3, J.P. Lundquist1, K. Machida12, K. Martens9,

T. Matsuda20, T. Matsuyama10, J.N. Matthews1, M. Minamino10, K. Mukai12, I. Myers1, K. Nagasawa13, S. Nagataki14, T. Nakamura21, T. Nonaka8, A. Nozato6, S. Ogio10, J. Ogura2, M. Ohnishi8, H. Ohoka8, K. Oki8, T. Okuda22, M. Ono14, A. Oshima10, S. Ozawa18, I.H. Park23, M.S. Pshirkov24, D.C. Rodriguez1, G. Rubtsov17,

D. Ryu25, H. Sagawa8, N. Sakurai10, A.L. Sampson1, L.M. Scott15, P.D. Shah1, F. Shibata12, T. Shibata8, H. Shimodaira8, B.K. Shin4, J.D. Smith1, P. Sokolsky1, R.W. Springer1, B.T. Stokes1, S.R. Stratton1,15, T.A. Stroman1,

T. Suzawa13, M. Takamura5, M. Takeda8, R. Takeishi8, A. Taketa26,M. Takita8, Y. Tameda11, H. Tanaka10, K. Tanaka27, M. Tanaka20, S.B. Thomas1, G.B. Thomson1, P. Tinyakov17,24, I. Tkachev17, H. Tokuno2, T. Tomida28,

S. Troitsky17, Y. Tsunesada2, K. Tsutsumi2, Y. Uchihori29, S. Udo11, F. Urban24, G. Vasiloff1, T. Wong1, R. Yamane10, H. Yamaoka20, K. Yamazaki10, J. Yang3, K. Yashiro5, Y. Yoneda10, S. Yoshida19, H. Yoshii30, R. Zollinger1, Z. Zundel1

1 University of Utah 2 Tokyo Institute of Technology 3 Ewha Womans University 4 Hanyang University5 Tokyo University of Science 6 Kinki University 7 Yonsei University 8 ICRR, University of Tokyo

9 IPMU, the University of Tokyo 10 Osaka City University 11 Kanagawa University 12 University of Yamanashi13 Saitama University 14 Astrophysical Big Bang Laboratory RIKEN, Wako 15 Rutgers University

16 Tokyo City University17 INR of the Russian Academy of Sciences 18 Waseda University19 Chiba University 20 KEK 21 Kochi University 22 Ritsumeikan University 23 Sungkyunkwan University

24 Universite de Libre de Bruxelles 25 Ulsan National Institute of Science and Technology26 ERI, University of Tokyo 27 Hiroshima City University 28 Advanced Science Institute, RIKEN

29 National Institute of Radiological Science 30 Ehime University

5 countries, 126 researchers

2014/10/13 H. Sagawa@UHECR2014

Telescope Array detector

32km

Utah, USA- lat. 39.30°N, long. 112.91°W

28km

5

Fluorescence Detector (FD)

Elevation angle：3～33°

Surface Detector (SD)3m2 scintillator detector507SDs, 、1.2km spacing~700km2


Hybrid observation since Mar, 2008

Refurbished HiRes

Recent TA results

Anisotropy (hot spot)Mass composition (Xmax)

Energy spectrum

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Anisotropy of arrival directions of highest-energy cosmic rays (hotspot)

• TA SD data 5 years (2008/May ~ 2013/May)

• E > 5.7×1019eV以上, zenith angle < 55°：72 events

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distribution of arrival directions (blue points)

TA FoV(Dec. > -10°)

Equatorial coordinates

GC

HotspotAnisotropy of highest-energy cosmic rays

• Maximum significance• direction：R.A. = 146.7°, Dec. = 43.2°• observed：19 (19/72=26%)• Expected for isotropy：4.5 (4.5/72=6%)• Li-Ma significance: 5.1𝜎𝜎

• Chance probability to obtain maximum significance of 5.1𝜎𝜎：3.7x10-4 (3.4𝜎𝜎)

• MC：15, 20, 25, 30, 35°-radius circles

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oversampling using 20-degree radius circles

Significance map

5-year data

ApJ 790, L21 (2014)

Hotspot +1-year data

• 2008/May ~ 2014/May (6 years)

• E > 5.7x1019eV: 72 events→87 events（+15）• Hotspot ： 19events→23 events（ +4）• Max. Li-Ma significance: 5.1𝜎𝜎 →5.55𝜎𝜎 Chance prob. = 3.4𝜎𝜎 →4.0𝜎𝜎2014/10/13 H. Sagawa@UHECR2014 9

Arrival direction distribution Significance map

blue：5-year datared： recent 1-year data

D.BergmanCOSPAR 2014

(19/72~26%, 4/15~26%)5 yrs +1 yr

(3.1x10-5)

Compatibility with isotropy

• Autocorrelation p ~ 0.001 (δ ~ 20o – 25o)• AGN p ~ 0.007• LSS p ~ 0.001

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Xmax analysis by hybrid events• MD FD: [refurbished HiRes] + SD

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J.N.MatthewsQui Nhon 2014arXiv:1408.1726Submitted to APP

(MD FD + SD)

hybrid

H. Sagawa@UHECR2014consistent with a light, largely protonic composition

Black points：TA dataMC(QGSJET-II-03)

blue：Proton, red：Fe18.2 < log10(E/eV) < 18.4

log10(E/eV) > 19

TA energy spectrum

• SD data：2008/May～2014/May (6 years)

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18.70±0.02

19.74±0.04ankleCutoff consistent with GZK cutoff

Ｅ > 1019.8eVExpected (no cutoff) = 85.93observed = 32Cutoff chance prob. = 6.59𝜎𝜎

D.BergmanCOSPAR 2014

Model of extremely-high-energy cosmic rays

2014/10/13 H. Sagawa@UHECR2014 13

Extragalactic proton CR

Distribution cases• isotropic• LSS (2MASS < 250 Mpc) Evolution (1+z)m

Injection spectrum E-P

source

Energy scale Flux normalization factor

4 fit parameters

Propagation code• Kalashev + Kido, arXiv:1406.0735Photon background• CMB• IRBNo GMF and no extra GMF

propagation

z ≲ 0.7○ 5-year TA SD data

If GZK cutoff exists,sources of highest-energy CRs whicharrive at the earth are restricted to nearby objests

Ursa Major cluster(D=20Mpc)

Virgo cluster(D=20Mpc)

2MASS catalog John P. Huchra, et al 2012, ApJ, 199, 26+ TA 5-year significance (color map)

Nearby galaxies(within ~50 Mpc)

14

Distribution of galaxies: anisotropic

Anisotropy of arrival directions ofhighest-energy cosmic rays2014/10/13 H. Sagawa@UHECR2014

• Quadrule TA SD (~3000 km2)• 500 scintillator SDs

2.1 km spacing (Japan)

• 2 FD stations each with 10 refurbished HiRes telescopes (US)

• Apply grants this fall (Japan, US)+ from Korea, Russia

• 2-year construction• 3-year observation

• TA SD: 21 year data• TA hybrid: 18 year data

TA×4 proposal

152014/10/13 H. Sagawa@UHECR2014

Efficiency for additional TA×4 SD array

162014/10/13 H. Sagawa@UHECR2014

TA SD reconstructionefficiency =100% forE > 1019eV

Differential for energiesTrigger condition. 3 MIPS. 3-fold SDs. < 8x2.08/1.2usec

Reconstruction. NSD≥ 4

57 EeV

Trig+recon

Trig. eff

Prospect of ＴＡ×4

• Arrival direction• Hotspot

• Confirmation at > 5𝜎𝜎 level• Fine structure?• Other excess spots?• Study of galactic MF and extragalactic MF

• Point source search• Correlation with the results by other experiments

• TA/Auger whole sky analysis• Search for correlation with gamma-ray sources• Search for correlation with IceCube neutrinos

• Measurement of spectrum and Xmax of cosmic rays around cutoff with high statistics

• Search for UHE gamma rays and neutrinos

172014/10/13 H. Sagawa@UHECR2014

Arrival directions of TA 6-year data

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192014/10/13 H. Sagawa@UHECR2014

Ursa Major Cluster(D=20Mpc)

Virgo Cluster(D=20Mpc)

2MASS catalog velocity 0 – 3000 km/sJohn P. Huchra, et al 2012, ApJ, 199, 26+ 5-year TA data (Color contour)

Nearby Galaxy Clusters and hotspotPerseus-Pisces

Supercluster(D=70Mpc)

Heliocentric velocity (Rough Distance)Red: 0-1000km/s (D = 0-15Mpc)Blue: 1000-2000km/s (D = 15-30Mpc) Green: 2000-3000km/s (D = 30-45Mpc)

20









212014/10/13 H. Sagawa@UHECR2014

Galactic filaments?

Ursa Major Cluster(D=20Mpc)

Virgo Cluster(D=20Mpc)

2MASS catalog velocity 0 – 3000 km/sJohn P. Huchra, et al 2012, ApJ, 199, 26+ 5-year TA data (Color contour)

Nearby Galaxy Clusters and hotspotPerseus-Pisces

Supercluster(D=70Mpc)

Heliocentric velocity (Rough Distance)Red: 0-1000km/s (D = 0-15Mpc)Blue: 1000-2000km/s (D = 15-30Mpc) Green: 2000-3000km/s (D = 30-45Mpc)

22






• TA/Auger whole sky analysis• Search for correlation with gamma-ray sources • Search for correlation with IceCube neutrinos



232014/10/13 H. Sagawa@UHECR2014

Search for clusters of highest energy cosmic rays

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TA: 2008/May – 2013/May (5 yrs) 72 events [ApJ 790 (2014) L21]Auger: 2004/Jan – 2009/Dec (5.5yrs) 62 events [APP 34 (2010) 314]

Hint of a point source?

Auger 123 EeV

TA 136 EeV

TA 101 EeV

Ｅ > 5.7x1019eV

doublet

new event








252014/10/13 H. Sagawa@UHECR2014

26

TA Hotspot5.1σ

Auger ∼3σ around Cen A

TA and Auger pretrial significance summed over with 20o-radius Circle

Adopted same analysis as the TA









272014/10/13 H. Sagawa@UHECR2014

Prospect in the summer of 2020

If we start TAx4 project in 2015,2015-2016 construction of new detectors

2017-2019 operation of full TAx4

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Arrival directions of TA 6-year data

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1 cluster in the hotspotin the summer of 2020

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2 clusters in the hotspot in the summer of 2020

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2 clusters in the hotspot+Perseus cluster in the summer of 2020

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332014/10/13 H. Sagawa@UHECR2014

TA and Auger energy spectrum

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Spectrum by TA SD for 6 years (this conf.)

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Spectrum by TA SD for 7 years in the summer of 2015

Spectrum only by TA SD for 12 years in the summer of 2020

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Spectrum by (TA SD for 9 years and TAx4 for 3 years) in the summer of 2020

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Spectrum by (TA SD for 9 years and TAx4 for 3 years)together with other cases

in the summer of 2020

2014/10/13 H. Sagawa@UHECR2014 39








402014/10/13 H. Sagawa@UHECR2014

Xmax for TA hybrid events for 9 years and TAx4hybrid events for 3 years

(assuming proton QGSJET II-03 model)

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TA hybrid events for corresponding to 18-year TA hybrid events





• TA/Auger whole sky analysis• Search for correlation with gamma-ray sources by MAGIC etc.• Search for correlation with IceCube neutrinos

• Measurement of spectrum and Xmax of cosmic rays above cutoff with high statistics


422014/10/13 H. Sagawa@UHECR2014

Summary

2014/10/13 H. Sagawa@UHECR2014 43

TA

Hotspot: anisotropy ofcosmic rays with E >

5.7×1019eV (post-trial 4σ)

consistent with a light, largely protonic composition

(E > 1018.2eV)

Spectrum breaks consistent with

GZK cutoff (6.6σ)e+e- production dip

TA×4Quadruple TA SD

2 more FDs

Nearby extragalactic universe exploring by highest-energy

cosmic rays5- or 6-year data

END

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TALE+TA spectrum (E > 1015.9 eV)

2014/10/13 45

Energy region over > 4 decades

TALE Ckov: Cherenkov component is major

（FD) (SD)

Breaks at around 1016.2eV and 1017.3eV

H. Sagawa@UHECR2014

TA: 6 year SD dataTALEObservation time:144 hours（2013/Sep/6 ~ 2013/Dec/6)

Statistical test for compatibility with LSS and isotropy

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Correlation with AGN from VCV catalog

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6-year TA SD datazenith angles < 45°

Galactic coordinates● : AGN: ●: TA events correlating within 3.1°○: non-correlating events

Ntot = 53, Ncor = 21, (40%)Nbg = 12.5 (24%)p-value = 0.007 (2.7𝜎𝜎)

Correlation with AGN from VCV catalog

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ta 4 - telescope array projectuhecr14.telescopearray.org/sagawa/20141015-tax4-v5.pdf · ta×4 h....

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