JEM-EUSO mission and GRIDJEM-EUSO mission and GRIDToshikazu EbisuzakiToshikazu Ebisuzaki

RIKENRIKEN

for the JEM-EUSO Collaborationfor the JEM-EUSO Collaboration

Toshikazu EbisuzakiToshikazu EbisuzakiRIKENRIKEN

for the JEM-EUSO Collaborationfor the JEM-EUSO Collaboration

EExtreme UUniverse SSpace OObservatory

Do-Son ACCGRID School November 16, 2007Do-Son ACCGRID School November 16, 2007

Japan : T. Ebisuzaki, Y. Uehara, H. Ohmori, Y. Kawasaki, M. Sato, Y. Takizawa, K. Katahira, S. Wada, K. Kawai, H. Mase (RIKEN), F. Kajino, M. Sakata, H. Sato, Y. Yamamoto, T. Yamamoto, N. Ebizuka, (Konan Univ.), M. Nagano, Y. Miyazaki (Fukui Inst. Tech.), N. Sakaki, T. Shibata (Aoyama Gakuin Univ.), N. Inoue (Saitama Univ.), Y. Uchihori (NIRS), K. Nomoto (Univ. of Tokyo), Y. Takahashi (Tohoku Univ.), M. Takeda (ICRR, Univ. Tokyo), Y. Arai, Y. Kurihara, H.M. Shimizu, J. Fujimoto (KEK), S. Yoshida, K. Mase (Chiba Univ.), K. Asano, S. Inoue, Y. Mizumoto, J. Watanabe, T. Kajino (NAOJ), H. Ikeda, M. Suzuki, T. Yano (ISAS, JAXA), T.Murakami, D. Yonetoku (Kanazawa Univ.), T. Sugiyama (Nagoya), Y. Ito (STEL, Nagoya Univ.), S. Nagataki (YITP, Kyoto Univ.), A. Saito(Kyoto Univ.), S. Abe, M. Nagata (Kobe Univ.), T. Tajima (KPSI, JAEA) 、 M. Chikawa (Kinki Univ.), and M. Tajima (Hiroshima Univ.)USA : J. H. Adams Jr., S. Mitchell, M.J. Christl, J. Watts Jr., A. English, R. Young (NASA/ MSFC) , Y. Takahashi, D. Gregory, M. Bonamente, P. Readon, V. Connaughton, K. Pitalo, J. Hadaway, J. Geary, R. Lindquist, P. Readon (Univ. Alabama in Huntsville), H. Crawford, C. Pennypacker (LBL, UC Berkeley), K. Arisaka, D. Cline, J. Kolonko, V. Andreev (UCLA), T. Weiler, S. Csorna (Vanderbilt Univ.),France : J-N. Capdevielle, P. Gorodetzky, P. Salin, J. Dolbeau), T. Patzak, F. Vanucci (APC,CNRS ), J. Weisbard (IN2P3)Germany: M. Teshima, T. Schweizer (Max Planck Munich), A. Santangelo, E.Kendziorra, F.Fenu (Univ. Tuebingen), P. Biermann (MPI Bonn), K. Mannheim (Wuerzburg), J. Wilms (Univ. Erlangen)Italy : S. Bottai. P. Spillantini, A. Zuccaro (Firenze), A. Anzalone, O. Catalano, M.C. Maccarone, P. Scarsi, B. Sacco (IAS-PA/INAF), G. D’Ali Saiti (U. Palermo), B. Alpat, R. Battiston, B. Bertutti, E. Fiandrini, P. Zuccon (Perugia), M. Casolino, M.P. De Pascale, A. Morselli, P. Picozza, R. Sparvoli (INFN and Univ. Rome “Tor Vergata”), P. Vallania (INAF-IFSI Torino), P. Galleotti, C. Vigorito, M. Bertaina (Univ. Torino), A. Gregorio (Trieste) Mexico: G. Medina-Tanco, J.C. D’Olivo, J.F.Valdes (Mexico UNAM), H. Salazar, O. Martines (BUAP), L. Villasenor (UMSNH)Republic of Korea : S. Nam, I. H. Park, J. Yang (Ehwa W. Univ.)Russia: Garipov G.K., Khrenov, B.A., Klimov P.A. Panasyuk M.I., Yashin I.V. (SINP MSU), D. Naumov, Tkachev. L (Dubna JINR)Switzerland : A. Maurissen, V. Mitev (Neuchatel, Switzerland) :Spain: D.Rodriguez-Frias, L.Peral, J.Gutierrez, R.Gomez-Herrero (Univ. Alcala)

10 countries, 53 institutions, 139 membersJEM-EUSO Collaboration

JEM-EUSO=Astronomical Earth Observatory

EECR ｓ

X, γ,ν,p, e

UV, X, γ,νp, n, e

EHE Neutrinos

Non-Local EECR

UV

Plasma Discahrge

Dust and Meteors

Night glow

Solar wind

From EUSO to JEM-EUSO EUSO @ ESA selection 2000 -• Europe ： Phase-A Completed

»By July 2004

• Japan ： JAXA and RIKEN funded concept studies 1998-06

• USA ： End-to-End MIDEX $36M

ESA/ESTEC meeting, October 2005,　 Plan changed due to large stopping factors: (i) USA changed the ISS plan and the usage of STS, (ii)Budgetary troubles at D/S of ESA for Columbus EUSOESA D/HME and NASDA worked together to use (JEM EF)

and HTV/H2B for EUSO (Phase-A extension 2004).Japan and USA and a part of Europe made JEM-EUSO

Working Group. It was authorized by JAXA/ISAS; Europe re-organized, and Russia/Korea/Mexico joined.

Collaboration: （ 9 nations ）Italy, France, Switzerland Germany, (Portugal), (Spain)Japan, USA, (Brazil), Russia, Korea, Mexico

Robotic Arm

JEM Exposure Facility

　・ Number of ports: 10

　・ Power ： 120Vdc 、 Max10kW

　・ Communication ： low speed （ MIL-STD-1553B ）　 medium speed （ Ethernet ）、 High speed :FDDI ）

　・ Coolant ： controlled temperature 20±4℃

ELM/ES

　 Recycling of payloadPayload

standard envelope ： 1.85m×1.0m×0.8m

mass ： less than500kg

Pressurized Module

Airlock between Pressurized Module

and Exposure Facility

Outline of JEM Exposure Facility

6

Resources of the 2nd phase JEM utilization by JAXA (under study)

2007H19

2008H20

2009H21

2010H22

2011H23

2012H24

2013H25

2014H26

2015H27

2016H28

△Shuttle Retirement

HTV △TF

△2J/A

2017H29

Verification

1st phase 2nd phase 3rd phase

New Rack

New Rack

1J/A △　　　 1J△

New EF Payload

RYUTAI Rack

MAXI

SMILES

SEDA-AP

New EF Payload

JFY

Verification

SAIBO Rack

KOBIRO Rack

Small Payloads

JEM-PM

JEM-EF

HDTV System

Launch by HTV (Under study)

H-II Transfer Vehicle (HTV)H-II Transfer Vehicle (HTV)H-II Transfer Vehicle (HTV)H-II Transfer Vehicle (HTV)

©JAXA

HTV is 4m across and about 10 m long

Parameters of Mission• Time of launch: year 2013• Operation Period: 3 years (+ 2 years)• Launching Rocket : H2B• Transportation to ISS: non pressurized Carrier of

H2 Transfer Vehicle (HTV)• Site to Attach: Japanese Experiment Module/

Exposure Facility #2• Height of the Orbit: ~430km• Inclination of the Orbit: 51.6°• Mass: 1896 kg• Power: 998 W 　 (operative),

344 W (non-operative)• Data Transfer Rate: 297 kpbs

Important calendar (recent past)• ESA Selection 2000; • NASA selection 2003; Supports by JAXA and RIKEN 1997-2007• Phase-A completion 2004

• June 2006: – JEM-EUSO WG was approved by Space Science committee of ISAS/JAXA

• Aug. 2006: – JEM-EUSO Planning Committee was established by K. Kaya, Director General of

DRI/RIKEN• Nov. 2006:

– AO was released by JAXA• Feb. 2007:

– Proposal was submitted from RIKEN• May 2007:

– The selection of JEM-EUSO was announced by JAXA• June 2007

– Kick-Off Meeting– International Advisory Board Meeting– 2-Yr Contract of Phase-A/B Between JAXA and RIKEN

Important calendar (forthcoming)

• Two-Year-Long Phase-A/B Study– Short report to the selection committee

• Nov. 2007

– Midterm Review• Apr. 2008

– Final Review for later phases• The end of Phase-A/B study

– Production, Assembly & Verification by 2012

• Expected launch by HIIB-HTV in 2013

Principle of EUSO- first remote-sensing from space, opening a new window

for the highest energy regime

From College de France: better data now

TPC-likenaturalchamber

Cf: Ground-based arrays < 0.01 EUSO(1) Scintillator array,(2)Fluorescence telescope array

1020 eV

Airshower observed from JEM-EUSO

• Smaller Mie Scattering– ~20%

• Low Cloud (2~3km) in night– Most of the showers reaches

the maximum above the cloud

• Smaller Absorption (loss)– ~ 0.3, and uncertainty < 0.05– Large absorption/uncertainty

(loss) X 10 ~100 for ground fluorescent observatory

• Well determined Distance to a Shower – Observation altitude : ~400km– Shower altitude : ~10km

Looking Down from Space is much better than Looking up from the Ground

Altitude of the starting point

Tra

nsm

issi

on

Earth Atmosphere as a Detector

EUSO ~ 1000 x AGASA ~ 30 x AugerEUSO (Instantaneous) ~ 5000 x AGASA 　　　　　　　　　　　　　　　　　　　 ~ 150 x Auger

AGASA

JEM-EUSO tilt-mode

JEM-EUSO FoV

Tilt Mode FOV

Tilt Angle [degree]

Are

a of

FO

V [

km

2 ]

Science Objectives

Fundamental Objective:

Extreme energy astronomy by particle channel

Exploratory Objectives• Detection of extreme energy neutrinos to examine extra

dimensions in super-gravity/string theory• Examination of quantum gravity, dark matter and

quantum limit at super-LHC energies to m > 300 TeV/c2

• Global observations of night-glows, plasma discharges and lightings

E>1020 eV particles are not reflected by GMF

Specify origins by the arrival direction:

Particle Astronomy

Arrival Directions （ AGASA ）

1438 deployed 1400 filled 1364 taking data

090707 ~ 85%

All 4 fluorescence buildings complete,each with 6 telescopes

1st 4-fold on 20 May 2007

AIM: 1600 tanks

HYBRID DETECTOR

AugerVIETNAM TEAM OF PROF. DARRIULAT

OF INST

Centaurs A

Centaurs A

• Radio Galaxy– Most luminous in the

sky

• Double Lobe Source• Elliptical galaxy with a

dark lane– Recent accretion

event of gas rich spiral

Optical

Radio X-ray

Clusters of AGASA are in the region diflection angles less than 5 degrees

Auger

• Stronger magnetic field

• Lower energy >6x1019 eV

• Still, Auger sees the correlation with AGNs

JEM-EUSO

• All sky observation

• higher energy>1020eV G. A. Medina Tanco et al. astro-ph/9707041

Auger: Stronger Magnetic FieldSouthern sky is not good for astronomy

UHECR possible LLSA.Olinto et al.

到来方向解析

Particle Astronomy

- 1,000 events : E>7x1019eV- Several dozen clusters are expected- All sky coverage

If we get >1,000 events,

by Boris Khrenov 2006

Progress of EECRs we expect in the near future:

4×105JEM-EUSO(nadir)

JEM-EUSO 　 (tilt)

観測期待事例数 (GZK)

Log(E) Nadir Tilt 30° Tilt 35° Tilt 37°

19.7 1317.3 1394.0 1575.4 1966.0

19.8 570.5 653.7 790.8 916.4

20.0 74.7 86.4 111.7 146.5

20.2 14.1 20.4 24.1 30.0

20.4 5.7 9.9 11.7 13.9

20.6 2.4 4.5 5.4 6.5

20.8 0.9 1.8 2.2 2.7

21.0 0.2 0.4 0.5 0.6

Integral/year

Auger Residual plot

スペクトル解析

GZK 　 complex （ one set ）スペクトル解析

GZK cut-off

GZK recovery

GZK bump

Ankle region

proton

E = 1020 eV

2.7K CMB γ

neutron

π

e

e

protonee

2.725 K

410 photons / cm3 Gamma Beam Energy (GeV)

Cro

ss S

ect

ion

(m

b)0.1

0.01

γ + p→Δ （1232）→ π o p or π + n

Gamma Beam Energy (GeV)

Cro

ss S

ect

ion

(m

b)0.1

0.01

γ + p→Δ （1232）→ π o p or π + n

Gamma Beam Energy (GeV)

Cro

ss S

ect

ion

(m

b)0.1

0.01

γ + p→Δ （1232）→ π o p or π + n

0.6 x 10-27 cm2Cosmic Microwave Background

Exploratory objective 1: GZK process makes neutrinos

ニュートリノ

Sensitivity for neutrino (preliminary; TBC)

Air

earth

*Hundreds of neutrino events

100 times even rate in the case of extra dimension

ニュートリノ

Cross-section will be increased by a factor of 100 in the case of extra-

dimension

Atmospheric Sciences

• Lightning, TLE ｓ– Nadir Observation of Lightning and TLE ｓ– Global Survey of TLE ｓ

• Night Grow, Plasma Bubbles– Global Imaging of O2 　 Hertzburg I night grow– Formation Mechanism of Plasma Bubbles– Energy, Momentum, and Material transfers in upper a

tmosphere• Clouds

– Global survey of cloud top hight• Meteors

大気圏

大気圏

From EUSO to JEM-EUSO

JEM-EUSO is the direct successor of EUSO,Improved performance: by larger capacity of JEM

EUSO Eth = 5×1019eV 　　　　↓JEM-EUSO Lower threshold

• New Material (CYTOP) and Advanced Design

×1.5 reduction in Eth

• Higher QE devices 　 >×1.5

• Advanced Trigger algorithm 　 >×2

• Tilt mode enlarges exposure

×5 exposure at E >1020 eV

CYTOP

PMMA~50% up

Field of View (deg)

En

circ

led

En

erg

y w

ith

in 5

mm

dia

. optics

進歩 1/4

50% increase

detector

Higher sensitivity :x2

Trigger algorithm

The TUS detector will be launched on a new platform separated from the main body of the “Foton” satellite (RosCosmos project,Samara enterprise, launching in 2009-2010). Satellite limits for the scientific instrument are:mass 60 kg, electric power 60 Wt, orientation to nadir ±3o .Preliminary TUS design: 1- in the transportation mode, 2 – in operation.

1 2

Mirror area 1.5 m2 , pixels cover 4000 km2 of the atmosphere (orbit height 400 km).

TUS ： Path finder mission

Summary• EUSO completed Phase-A from 2000 to 2004 in

the ESA program and NASA MIDEX program

• JEM-EUSO has been selected by JAXA as a mission candidate for the second-phase utilization of JEM/EF on ISS for launch in 2013for 5-yrs (or longer) exposure.

• Phase-A/B Study at JAXA began: Two-years-long– Short report: October 2007– Midterm Evaluation ： April 2008

• JEM-EUSO has exposure (with tilt) > 106 km2 sr yr• Data Sharing in Collaboration by GRID enviroment

JEM-EUSO and GRID

• National Research Grid Initiative – Directed by Ken Miura– Development of Middle and application software in GRID

environment– Collaboration with Data Center

• KEK EGEE in GIN (High Energy physics)• National Astronomical Observatory in Virtual Observatory

(Astronomy)• Bioinformatics (RIKEN and others)

• JEM-EUSO is a part of LIA of France-Japan PPL• 10 years operation of Computer Center in INST

– Directed by Dr. Le Van Ngoc– Supported by RIKEN