2018/12/21 ICRR 1

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CALET collaboration team

1) Aoyama Gakuin University, Japan2) CRESST/NASA/GSFC and Universities Space Research Association, USA3) CRESST/NASA/GSFC and University of Maryland, USA4) Hirosaki University, Japan5) Ibaraki National College of Technology, Japan6) Ibaraki University, Japan7) ICRR, University of Tokyo, Japan8) ISAS/JAXA Japan9) JAXA, Japan10) Kanagawa University, Japan11) Kavli IPMU, University of Tokyo, Japan12) Louisiana State University, USA13) Nagoya University, Japan14) NASA/GSFC, USA15) National Inst. of Radiological Sciences, Japan16) National Institute of Polar Research, Japan17) Nihon University, Japan

18) Osaka City University, Japan19) Ritsumeikan University, Japan20) Saitama University, Japan21) Shibaura Institute of Technology, Japan22) Shinshu University, Japan23) St. Marianna University School of Medicine, Japan24) University of Denver, USA25) University of Florence, IFAC (CNR) and INFN, Italy26) University of Padova and INFN, Italy27) University of Pisa and INFN, Italy28) University of Rome Tor Vergata and INFN, Italy29) University of Siena and INFN, Italy30) University of Tokyo, Japan31) Waseda University, Japan32) Washington University-St. Louis, USA33) Yokohama National University, Japan34) Yukawa Institute for Theoretical Physics, Kyoto University, Japan

O. Adriani25, Y. Akaike2, K. Asano7, Y. Asaoka9,31, M.G. Bagliesi29, G. Bigongiari29, W.R. Binns32, S. Bonechi29, M. Bongi25, P. Brogi29, J.H. Buckley32, N. Cannady12, G. Castellini25, C. Checchia26, M.L. Cherry12,

G. Collazuol26, V. Di Felice28, K. Ebisawa8, H. Fuke8, G.A. de Nalfo 14, T.G. Guzik12, T. Hams3, M. Hareyama23,N. Hasebe31, K. Hibino10, M. Ichimura4, K. Ioka34, W.Ishizaki7, M.H. Israel32, A. Javaid12, K. Kasahara31,

J. Kataoka31, R. Kataoka16, Y. Katayose33, C. Kato22, Y.Kawakubo1, N. Kawanaka30, H. Kitamura15,H.S. Krawczynski32, J.F. Krizmanic2, S. Kuramata4, T. Lomtadze27, P. Maestro29, P.S. Marrocchesi29,

A.M. Messineo27, J.W. Mitchell14, S. Miyake5, K. Mizutani20, A.A. Moiseev3, K. Mori9,31, M. Mori19, N. Mori25, H.M. Motz31, K. Munakata22, H. Murakami31, Y.E. Nakagawa8, S. Nakahira9, J. Nishimura8, S. Okuno10,

J.F. Ormes24, S. Ozawa31, L. Pacini25, F. Palma28, P. Papini25, A.V. Penacchioni29, B.F. Rauch32,S.B. Ricciarini25, K. Sakai3, T. Sakamoto1, M. Sasaki3, Y. Shimizu10, A. Shiomi17, R. Sparvoli28, P. Spillantini25,

F. Stolzi29, I. Takahashi11, M. Takayanagi8, M. Takita7, T. Tamura10, N. Tateyama10, T. Terasawa7,H. Tomida8, S. Torii9,31, Y. Tunesada18, Y. Uchihori15, S. Ueno8, E. Vannuccini25, J.P. Wefel12, K. Yamaoka13,

S. Yanagita6, A. Yoshida1, K. Yoshida21, and T. Yuda7

2018/12/21 ICRR 4

FRGF (Flight Releasable Grapple Fixture)

CGBM (CALET Gamma-ray Burst Monitor)

ASC (Advanced Stellar Compass)

GPSR (GPSReceiver)

MDC (Mission Data Controller)

Calorimeter

� Mass: 612.8 kg� JEM Standard Payload Size:

1850mm(L) × 800mm(W) × 1000mm(H)� Power Consumption: 507 W�max�� Telemetry:

Medium 600 kbps (6.5GB/day) / Low 50 kbps

Launched on Aug. 19th, 2015by the Japanese H2-B rocket

Emplaced on JEM-EF port #9on Aug. 25th, 2015(JEM-EF: Japanese ExperimentModule-Exposed Facility)

Kounotori (HTV) 5

JEM/Port #9

CALET Payload

2018/9/15 4JPS 2018 Autumn - 60 years of PRL -

Observation by High Energy Trigger for 1032 days : Oct.13, 2015 – July 31, 2018p The exposure, SΩT, has reached to ~ 89.6 m2 sr day for electron observations

by continuous and stable operations.p Total number of triggered events is ~ 670 million with a live time fraction

of 84.0 %.

Observation with High Energy Trigger (>10GeV)

Accumulated triggered event numberAccumulated observation time (live, dead)

Live Time Fraction: 84.0%

6.53 x105 events /day (� 7.6 Hz)

Total Number�6.68 x 108 events

Y.Asaoka, S.Ozawa, S.Torii et al. (CALET Collaboration), Astropart. Phys. 100 (2018) 29.

Fe, ΔE=9.3 TeV

Gamma-ray, E=44.3 GeV Electron, E=3.05 TeV

Proton, ΔE=2.89 TeVExamples of Observed Events

Unit in MIP

Event Display: Electron Candidate (>100 GeV)

TASC Energy Deposit Distribution of All Triggered-Eventsby Observations for 1023 days

1 PeV

LE-Triggerregion

HE-Triggerregion

The TASC energy measurements have successfully been carried out in the dynamic range of 1 GeV – 1 PeV.

All Particles

Only statistical errors presented

Distribution of deposit energies (ΔE) in TASC

Performance of electron energy measurement in 1GeV-20TeV

Energy resolution for electrons (TASC+IMC):

< 3% over 10 GeV; <2% over 20GeV

Y.Asaoka, et al. (CALET Collaboration), Astroparticle Physics 91 (2017) 1.

2018/12/21 7ICRR

All-Electron (electron + positron) Analysis

CALET is an instrument optimized for all-electron spectrum measurements.

Þ CALET is best suited for observation of possible fine structures in the all-electron spectrum up to the trans-TeV region.

1. Reliable trackingwell-developed shower core

2. Fine energy resolution full containment of TeV showers

3. High-efficiency electron ID30X0 thickness,closely packed logs

3TeV Electron Candidate

Corresponding Proton Background

(Flight data; detector size in cm)

10X0

17X0

30X0

2018/12/21 8

(A+B+C+D) (A+B+C+D)

Extended Analysis of e/p Separation to Full Acceptance

Analyzed Flight Data:• 780 days (October 13, 2015 to November 30, 2017)• Full CALET acceptance at the high energy region (Acceptance A+B+C+D; 1040cm2sr).

In the low energy region fully contained events are used (A+B; 550cm2sr)

(A+B+C+D)

2018/12/21 9ICRR

Approximately doubled statistics above 500GeV by using full acceptance of CALET

CALET: Phys. Rev. Lett. 120 (2018) 261102 (~ 2 x PRL2017)DAMPE: Nature 552 (2017) 63, 7 December 2017

2018/12/21 10ICRR

All-Electron Spectrum Measuredwith CALET from 11 GeV to 4.8TeV

Spectral breakat 0.9TeV

Blue: DAMPE broken power-law,χ2/NDF = 17/25

Green: exponential cut-off,χ2/NDF = 13/25 (break ~2.3TeV)

Black: single power-law,χ2/NDF = 26.5/26

CALET All-Electron Spectrum in sub-TeV to TeV region

CALET observes flux suppression consistent with DAMPE within errors above 1TeV.

DAMPE: Nature 552 (2017) 63

2018/12/21 ICRR 11

Comparison with DAMPE’s result

We don’t see any peak-like structure at around 1.4TeV even in the shifted energy binning.

What happens if we shifted our energy binning…

ICRR2018/12/21 12

Prospects for CALET All-Electron Spectrum

Extension of energy reach⇒ identification of local

cosmic-ray accelerator

Further precision ⇒ origin of positron excess

pulsar or dark matter

Five years or more observations ⇒ 3 times more statistics, reduction of systematic errors

• The possibility of new discoveries dwells in fine structures of the all-electron spectrum.

• Taking advantage of localness, the TeV all-electron spectrum approaches its origin.

Vela

Contribution from distant SNe

13

Local young SNe

2018/12/21 ICRR

HHe

LiBeB

C

N

O

F

Ne

Na

Mg

Al

KCa

Si

PSCl Ar Ti

Sc V

Fe

Mn

Ni

2018/12/21 14

Charge Identification of Nuclei with CHD

CHD charge resolution(2 layers combined) vs. Z

• ΔZ= 0.1e (p)~ 0.28e (Fe)

• Charge separation in B to C : ~7 σ

Non-linear response

to Z2 is corrected in

CHD using a model.

ICRR

HHe

LiBeB

C

N

O

F

Ne

Na

Mg

Al

KCa

Si

PSCl Ar Ti

Sc V

Fe

Mn

Ni

15

Preliminary Flux of Primary Nuclei Components

Flux measurement: N(E): Events in unfolded energy binSΩ : Geometrical acceptanceT : Live time ε(E) : Efficiency ΔE : Energy bin width

Observation period: 2015.10.13 – 2017.5.31 (962 days)Selected events: ~17 million

2018/12/21 ICRR

Flux validation with bright sources

CALET Gamma-ray Sky (>1GeV)

Geminga:432 Vela:138Crab:150All: 45740(As of 180131)

Crab Geminga Vela

Electromagnetic Emission from Gravitational Wave Events ?

90 % CL Upper Limits for GW Counterpart Search

2018/12/21 ICRR 19

Publication List in FY 2017-2018 �refereed)

1) “Characteristics and Performance of the CALorimetric Electron Telescope (CALET) Calorimeter for Gamma-Ray Observations”, *N.Cannady, *Y.Asaoka, et al. (CALET Collaboration), The Astrophysical Journal Supplement Series 238:5 (16pp), 2018.

2) “Search for GeV Gamma- Ray Counterparts of Gravitational Wave Events by CALET", O.Adriani, *Y.Asaoka, *M.Mori, et al. (CALET Collaboration), The Astrophysical Journal, 863:160 (9pp), 2018.

3) “Extended Measurements of Cosmic-ray Electron and Positron Spectrum from 11 GeV to 4.8 TeV with the Calorimetric Electron Telescope on the International Space Station”, O. Adriani, *Y. Asaoka , *S.Torii, et al. (CALET Collaboration), Phys. Rev. Lett. 120, 261102 (7pp) (2018).

4) “Detection of the thermal component in GRB 160107A”, *Kawakubo Yuta, Sakamoto Takanori, et al. (CALET collaboration), Publication of the Astronomical Society of Japan, 70(1) p.61

5) �Energy Spectrum of Cosmic-Ray Electron and Positron from 10 GeV to 3 TeV Observed with the Calorimetric Electron Telescope on the International Space Station”, O. Adriani, *Y. Asaoka , * S. Torii, et al. (CALET Collaboration), Phys. Rev. Lett. 119, 181101(6pp) (2017).

6) “On-orbit Operations and Offline Data Processing of CALET onboard the ISS”, *Y. Asaoka, S.Ozawa, S. Torii, et al. (CALET Collaboration), Astroparticle Physics, 100 (2018) 29-37

7) “Energy calibration of CALET onboard the International Space Station”,*Y. Asaoka, et al. (CALET Collaboration), Astroparticle Physics, 91 (2017) 1-10.

2018/12/21 ICRR 20

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Summary and Future Prospects

p CALET was successfully launched on Aug. 19, 2015, and the detector is being very stable for observation since Oct. 13, 2015.

p As of July 31, 2018, total observation time is 1032 days with live time fraction to total time close to 84%. Nearly 670 million events are collected with high energy (>10 GeV) trigger.

p Accurate calibrations have been performed with non-‐interacting p & He events + linearity in the energy measurements established up to 106 MIP.

p All electron spectrum has been extended in statistics and in the energy range from 11 GeV to 4.8TeV.

p Preliminary analysis of nuclei and gamma-rays have successfully been carried out and spectra are obtained in the energy range:

• proton: 50 GeV ~ 100 TeV, helium: 10 GeV/n ~ 20 TeV/n, C-Fe: 50 (200) GeV ~ 100 TeV.• B/C ratio: 20 GeV/n ~ 1 TeV/np Preliminary analysis of UH cosmic rays up to Z=40 was achieved.p CALET’s CGBM detected nearly 60 GRBs (~20 % short GRB among them ) per year in the

energy range of 7keV-20 MeV. Follow-up observations of the GW events were carried out .p The so far excellent performance of CALET and the outstanding quality of the data suggest

that a 5-year observation period is likely to provide a wealth of new interesting results.