Space Science and Exploration Activities

of ISAS/JAXASaku Tsuneta

Institute of Space and Astronautical ScienceJapan Aerospace Exploration Agency

The UK-Japan 150 year anniversaryScience, Technology and Innovation Symposium - Astronomy & Space Science

The Embassy of Japan in the UK 6 December 2013

Hinode

X-ray sun in 2007

X-ray sun in 2012

What is ISAS? • As a national center of space science & engineering

research, ISAS carries out development (including vehicle development), launch and in-orbit operation of space science missions (scientific satellites, probes, sounding rockets, balloons and instruments on ISS)

• As an inter-university research institute, these activities are intimately carried out with both domestic and international partners. ISAS always seeks international collaborations

• Bottom-up process for mission selection: Space science missions proposed by researchers are reviewed by the steering committees for space science and space engineering

• ISAS is in a process of transition of heroic successes in the past 30 years into a future of sustainable excellence as a part of new JAXA.

Genealogy of Space Science missions

【Astrophysics 】

【Solar Science, Exploration,Space Engineering】

Geo-MagnetosphereObservation

X-ray Astronomy

Solar Physics

EngineeringSatellites

PlanetaryScience

Asteroid Exploration

Lunar Exploration

Infrared red Astronomy

Space VLBIAstronomy

First JapaneseSatellite ’70

ISAS strategic line

ISAS strategic line

ISAS strategic line

HINOTORI▼’81

HAKUCHO▼’79

KYOKKO・JIKIKEN▼’78 OHZORA

▼’84AKEBONO

▼’89GEOTAIL

▼’92

TENMA▼’83

GINGA▼’87

ASCA▼’93

SUZAKU▼’05

HALCA‘97 ▼

SFU/IRTS’95 ▼

HINODE▼’06

YOHKOH▼’91

NOZOMI▼’98

AKATSUKI▼’10

HAYABUSA▼’03

KAGUYA▼’07

SAKIGAKE・SUISEI▼’85

HITEN▼’92

MS-T1,T2,T3,T4▼’71-80

ASTRO-I(SPICA)▽’24

ASTRO-H‘15 ▽

ERG▽’15

BepiColombo▽’16

HAYABUSA２▽’14

SELENE-2▽’TBD

2013▼

MS-F2,REXS,SRATS▼’71-75

AKARI▼’06Basic experiment using

baloons

Technical accumulationby ground VLBI observation

OHSUMI

Hisaki▼’13

ISA

S s

trate

gic

line

ISS missions

FundamentalPhysics missions

HAYABUSA(MUSES-C)2003-2010Asteroid Explorer (JSPEC)

AKARI(ASTRO-F)2006-2011Infrared Astronomy

KAGUYA（SELENE)2007-2009Lunar Exploration (JSPEC)

SUZAKU(ASTRO-E2)2005-X-Ray Astronomy

M-V Rocket

AKATSUKI(PLANET-C)2010-Venus Meteorogy

Hisaki (SPRINT-A) -2013-Planetary atmosphere

HINODE(SOLAR-B)2006-Solar Observation

REIMEI(INDEX)2005-Innovative Technology Demonstration Experiment

IKAROS 2010-photon propulsion thin-film solarpowergeneration(JSPEC)

ISAS recent missions

M-V Rocket

AKATSUKI(PLANET-C) – 2010-Venus Meteorogy

Hisaki (SPRINT-A) -2013-Planetary atmosphere

IKAROS 2010-photon propulsion thin-film solarpowergeneration

HAYABUSA2 2014-Asteroid Explorer (JSPEC)

ERG 2015-

Van Allen belt

ISAS missions under development

ASTRO-H 2015-X-Ray Astronomy ESA Bepi-Colombo 2016

SOLAR-C

HINODE(SOLAR-B) 2006-Solar Observation

ESA JUICE 2024-Jupiter Icy moons

SPICA(ASTRO-I)2024-Infrared Astronomy

M-V Rocket

AKATSUKI(PLANET-C) – 2010-Venus Meteorogy

Hisaki (SPRINT-A) -2013-Planetary atmosphere

HAYABUSA2 2014Asteroid Explorer

ERG 2015-

Van Allen belt

SPICA(ASTRO-I) 2024-Infrared Astronomy

ASTRO-H 2015-X-Ray Astronomy Bepi-Colombo – 2016

SOLAR-CSOLAR-C

ESA JUICE 2024Jupiter Icy moons

ISAS missions being considered

ISAS Small satellitesHigh cadence-low cost

focused missions2017, 2020….

ESA Bepi-Colombo 2016

ESA JUICE 2024-Jupiter Icy moons

SELENE2(JSPEC)Lunar landing

ERG 2015-

Van Allen belt SOLAR-C

LiteBird

WISH

Hinode

Technology drivenLeading and creating space

science programs

Science drivenCreate, stimulate and encourage

new technology research

ISAS: a unique combination of space science and space technology

Space Science DivisionsSpace Astronomy Astrophysics

Solar System ScienceInterdisciplinary Space Science

Space Technology DivisionsSpace Flight Systems

Spacecraft Engineering

Recent accomplishments HAYABUSA & IKAROS

Led by JAXA Lunar & Planetary Exploration Program Group

[Tech. Demo. #1] Solar sail deployment

[Tech. Demo. #3]Photon propulsion

[Tech. Demo. #4]Solar sail guidance, navigation and control

Launch(21/May/2010)

Venus Flyby(8/Dec/2010)

[Tech. Demo. #2]Power generation by sail-mounted thin film solar cells

Extended operation phase(Jan/2010 - now)

～9/June/2010

～10/June/2010

IKAROS Technology Demonstration of Interplanetary Solar Power Sail

Thin film solar cell

Solar sail Diagonal20m

Led by JAXA Lunar & Planetary Exploration Program Group

Itokawa falcon

hayabusa

Led by JAXA Lunar & Planetary Exploration Program Group

Hayabusa sample analysis

LL chondrite

Parent body (>20 km)formation

Thermal metamorphism4.562 Gyr ago

Catastrophic destruction (Large-

scale collision)

Reaccumulation

Formation of ItokawaRubble-pile

Micro meteorite

Solar wind Cosmic ray

Space weathering

Resurfacing(～10’s cm/My)

regolith gardening (150 y -3 My)

Astonishing pieces of information Derived from 30-micron sample!

falcon

hayabusa

Planetesimal

Origin and evolution of the solar system Search for organic matter&H2O

4.6 billion years ago...

1999 JU3

Itokawa

In addition to the science of Itokawa...

Organic matter, H2O

Molecular cloud

Solar system

Proto solar system disk

HAYABUSA

Earth

The science of Itokawa

Mineralogy, Topography, Structure,

Regolith, Meteoroid

Space weathering, Impact, Cosmic ray,Solar wind

Boulder

S-type

C-type

falcon

hayabusa

Led by JAXA Lunar & Planetary Exploration Program Group

Hayabusa 2 mission

1/5

falcon

hayabusa

Led by JAXA Lunar & Planetary Exploration Program Group

Hayabusa 2 mission

1/5

falcon

hayabusa

HAYABUSA2 mission• Launch: 2014, arrival:2018, departure: 2019, return: 2020• Target: 1999 JU3, Only known C-type near-earth asteroid

Less exposed to heating events and retain more information of the era when the solar system was formed.Contain much more volatiles, such as organic matter and water.

• Key experiments: close-up observations, sample analyses, impact experiment in space

• Science goalsUnderstand how materials evolve in the early phase of the solar system and are altered at later times on the asteroid.Understand dynamical evolution and resultant structure of the asteroid, as a possible analogue for formatio of planetesimals.

Led by JAXA Lunar & Planetary Exploration Program Group

EpsilonH-II BH-II A• First Flight in 2001• 21 successful launches.• GTO 4-6 ton class

capability

• First Flight in 2009, • 4 successful flights of

16.5 ton HTV to ISS• GTO 8 ton class

capability

• First Launch (2013, Sep. 14)

• 3 stages Solid Rocket• LEO 1.2 ton

SSO 0.45 ton

Launch Vehicles

New Small Satellite Program

• Epsilon Launch Vehicle is a solid propellant rocket capable of launching a satellite weighing 1.2 tonnes into LEO.

• The launch capability will be enhanced per plan.

• With standardized s/c bus, ISAS intend to implement low-cost, high-cadence focused missions.

Unexpected huge public attention

Hisaki Successfully launched on 14 Sep. 2013 by the Epsilon launch vehicleEUV spectrograph for dedicated planetary observations(Venus, Mars, Jupiter, Mercury, Saturn) S/C weight：340kg

S/C power：900WS/C size: 7m x 4m x 1mOrbit：950～1150kmλ：50-150nm (EUV)

Hisaki Successfully launched on 14 Sep. 2013 by the Epsilon launch vehicleEUV spectrograph for dedicated planetary observations(Venus, Mars, Jupiter, Mercury, Saturn) S/C weight：340kg

S/C power：900WS/C size: 7m x 4m x 1mOrbit：950～1150kmλ：50-150nm (EUV)

Erosion?

Habitable Mars Non-habitableMars

Dynamic interaction between solar wind and Martian upper atmosphere (Oxygen ion) (STEL, Nagoya U.)

credit: NASA/Nagoya Univ.

HISAKI First Light! (19 Nov. 2013)

Geocorona

Body Aurora

Body

Jupiter1:51 UT

(High W/L resolution)

(Exposure time of 8 min.)

Venus7:29 UT

Io torus

Wavelength

Space

(Planetary obs. mode)

(Exposure time of 5 min.)

150nm Wavelength 50nm

Raw data

Raw data

ISAS – Lancaster Univ.• Hisaki – ISAS’s most new mission

(Launch 2013 Sep) to observe the Jovian magnetosphere.

• Joint obs. campaign by Hubble Space Telescope in Jan 2014: PI Sarah Badman (Lancaster U).

• Spotty but yet high-resolution obsof aurora by HST combined with the continuous obs. by Hisaki to reveal the fundamental behavior of the Jovian magnetosphere.

ISAS – Imperial CollegeUK-Japan Collaboration in Space Plasma Physics

• Adam Masters leading the Cassini data analysis effort at ISAS discovered an relativistic electron acceleration event at a very high-Mach number shock situated in front of Saturn.

• A discovery that has close relevance to electron acceleration at SNR shocks.

• Coauthors at Imperial College played key roles in the work that has an insightful conclusion with respect to the origin of Cosmic Ray.

Geospace Exploration Project ERG (Exploration of energization and Radiation in Geospace)

ERG is a project to elucidate acceleration and loss mechanisms of relativistic electrons around Earth during space storms. MeV electrons sometimes cause satellite anomaly, so that understanding of the Van Allen radiation belt dynamics is one of the key issues for space weather.

• Comprehensive observations for plasma/particles and field/waves.

• Newly developed wave-particle interaction analyzer

NASA Van Allen Probes (Launch: 2012)

JAXA ERG (Launch: 2015)

Collaboration with UKis essential for comprehensive understanding of the Geospace with ERG• SuperDARN World Wide Radar Network

(British Antarctic Survey, Leicester U., Lancaster U.) Council Chair: Prof. Lester of Leicester U.

• Magnetometer, Optical Imager and other observations at Antarctica by British Antarctic Survey

* Headed by the Prime Minister

Japan Aerospace Exploration AgencyJapan Aerospace Exploration Agency

Council for S&T Policy (CSTP)Council for S&T Policy (CSTP)Space PanelSpace Panel

Ministry of Education, Culture, Sports, Science and Technology (MEXT)Ministry of Education, Culture, Sports, Science and Technology (MEXT)

CabinetCabinet

Ministry of Internal Affairs & CommunicationsMinistry of Internal Affairs & Communications

Basic Space Law(Enacted, May 2008)

Cabinet SecretariatCabinet Secretariat

Strategic Headquarter for Space Policy*Strategic Headquarter for Space Policy*

Basic Plan for Space Policy

(Issued, June 2009)(Issued, January2013)

JAXA Mid-term Plan(5 years)

Other Ministries Other Ministries

Japan’s Space Related Organizations

Annual budget <2B$

Space Policy CommissionSpace Policy CommissionSpace Science and Exploration PannelSpace Science and Exploration Pannel

Space Strategy OfficeSpace Strategy Office

Ministry of Economy, Trade and IndustryMinistry of Economy, Trade and Industry

Cabinet OfficeCabinet Office

Council for Science and Technology (Committee on Space Development & Utilization /Aeronautical Technologies)

Council for Science and Technology (Committee on Space Development & Utilization /Aeronautical Technologies)

Space Transportation

Mission Directorate

Aerospace Research and Development Directorate

General Auditor Office

Institute of Aeronautical Technology

R&D on Aeronautical Science Technologies

Lunar and Planetary Explorations

Aero Technology Programs

Satellite Applications Mission

Directorate II

Satellite Applications

Mission Directorate I

Spectrum M

anagement O

ffice

Consolidated Space Tracking and Data Acquisition Departm

ent

Environmental Test Technology Center

Mamoru ENDOExecutive Director

Shizuo YAMAMOTOExecutive Director

Yoshiyuki HASEGAWAExecutive Director

Safety and Mission

Assurance Department

Dr. Naoki OKUMURAPresident

Kiyoshi HIGUCHIVice President

Tsukuba Space Center Adm

inistration Departm

ent

Security Administration

Office

General Affairs Departm

ent

Human Resources

Department

Contract Department

Ground Facilities Departm

ent

Space Education Center

Public AffairsDepartm

ent

Evaluation andAudit O

ffice

Finance Department

Yoshikazu KATOExecutive Director

International Relationsand

Research Department

Chief Engineer O

ffice

JAXA’s Engineering Digital Innovation Center

Industrial Collaboration and Coordination Center

Information System

s Departm

ent

Strategic Planning and M

anagement

Department

Institute of Spaceand Astronautical Science (ISAS)

Space Science Research and postgraduate

education

Space Science Programs

Technology Development

support for Projects

Promotion O

ffice for Collaboration with

Universities and Research Institutes

General Auditor

As of April 1, 2013

Yuichi YAMAURAExecutive Director

New

Business Prom

otion Office

JAXA Organization

Development of Space

Transportation Systems

Earth Observation

Programs

Disaster Monitoring

and Communications

Programs

Satellite Positioning Programs

Human Spaceflight Mission Directorate

Operations/Utilizationsof ISS and KIBO JEM,

R&D on Human Space Technologies

Lunar and Planetary Exploration

Program Group

Kazuhiro NAKAHASHIExecutive Director

Technical Development Support for Projects Maintenance of base technologies for space utilization / R&D on advanced technologies

Saku TSUNETAExecutive Director

1,000

1,200

1,400

1,600

1,800

2,000

2,200

180.0

（参考）ＪＡＸＡ予算の推移

27

［unit: Billion Yen］

192.5

185.1 186.6 183.4

（22.9)

172.6

172.0

Incl. accelerating the implementation of the supplementary budget

211.2

former 3 agencies

ＪＡＸＡ

• FY2013 Government Budget: 185.4 Billion Yen（Principal Budget:162.5 billion yen, FY2012 Supplementary Budget: 22.9 billion yen）

• Compared to the previous fiscal year: +1.0%（Incl. accelerating the implementation of the supplementary budget ）

185.4

162.5

Transition of JAXA BudgetTransition of JAXA Budget

FY2000 FY2001 FY2002 FY2003 FY2004 FY2005 FY2006 FY 2007 FY2008 FY2009 FY2010 FY2011 FY2012 FY2013

220

200

180

160

140

120

100

FY2013 : 162.5 Bil. YenFY2012: 172.0 Bil. YenFY2011: 172.6 Bil. Yen

FY2013 Annual Budget

International Space Station Program

Others

As of April, 2013

Reliability Improvement

Space TransportationSpace Applications

Space Science &Exploration

Space Technology & Aeronautics

31.319.3％

6.43.9％ 14.0

8.6％

25.015.4％

22.914.1％

24.815.3％

38.023.4％

The Number of Referred PapersSatellite Objective Start of

OperationEnd of

OperationCounting

PeriodNumber

AKATSUKI Venus Atmospheric Obs. 2010 operating 2011-2012 8

KAGUYA Lunar Exploration 2007 2009 2008-2012 190

HINODE Solar Obs. 2006 operating 2007-2012 844

AKARI Infrared Astronomical Obs. 2006 2011 2007-2012 222

SUZAKU X-ray Astronomical Obs. 2005 operating 2006-2012 681

HAYABUSA Asteroid Sample Return 2003 2010 2004-2012 129

NOZOMI Mars Scientific Obs. 1998 2003 1999-2012 26

HALCA Space VLBI 1997 2005 1998-2012 44

ASCA X-ray Astronomical Obs. 1993 2002 1994-2012 2287

GEOTAIL Geo-Magnetospheric Obs. 1992 operating 1993-2012 1236

YOHKOH Solar Obs. 1991 2000 1992-2012 1089

＜reference＞

Subaru Telescope

The Ground based optical&infrared Observatory

1999 operating 2000-2012 1031

0 50 100 150 200 250

Japan

USA

UK

Norway

Spain

France

Italy

Belgium

Germany

Ireland

Czech

China

India

Korea

Russia

Austria

Australia

Netherlands

Greece

Slovakia

Brazil

Switzland

Sweeden

23

20

5

2

3

1

1

0

0

0

0

3

1

4

0

0

0

0

0

0

0

0

0

23

35

15

1

3

0

1

1

10

1

1

4

3

2

0

0

0

0

0

0

0

0

0

13

35

14

2

6

3

3

0

6

1

0

14

8

2

2

1

1

1

1

0

0

0

0

18

43

7

0

6

5

1

1

10

1

2

6

8

4

0

2

0

1

1

1

1

1

0

13

37

18

2

4

1

2

3

8

0

2

12

6

0

0

2

1

1

1

1

0

0

1

17

33

13

2

2

5

2

0

8

2

0

9

8

3

0

0

0

1

5

0

0

1

0

7

18

3

0

2

6

3

1

6

1

0

5

1

1

1

0

0

0

0

1

0

0

0

2007

2008

2009

2010

2011

2012

2013

Hinode refereed papers: 844 papers for 7 yearsImmediate release of just-taken data

with analysis software & latest calibration info.

23 countresApprox. 120 papers per yearNo signature for declineActive Asian countries: China, Korea, InidaSame contribution from Asia, Europe, US

Curator: Dr. Shimojo (NAOJ)

Whole Asia

Whole Europe

FiscalYear 2008 2009 2010 2011 2012 2013 2014 2015 2016 2017 2018 2019 2020 2021 2022

Operating / Concluded

Under Developm

ent Sounding

Rocket

ASTRO-EII（SUZAKU）’05

GEOTAIL’92

SOLAR-B（HINODE）’06

MUSES-C（HAYABUSA）’03

ASTRO-H ’15

ASTRO-H

HAYABUSA SUZAKU

HINODE

Daytime Dynamo ’11,’13▼▼

CLASP ’15 ▼

MMS ’14 ▼

Space Science Cooperation with NASA and ESA

ASTRO-F（AKARI）’05

PLANET-C（AKATSUKI） ’10

BepiColombo ’16

SPICA ’24

JUICE ’22

▼

SPICA

Bepi Colombo

cooperation with NASA cooperation with ESA

HAYABUSA2 ’14 ▼

▼

▼

▼

▼

ERG

ASTRO-H

ISAS/JAXA mission categories

Strategic Large Missions (300M$ class) for JAXA-led flagship science missionwith HIIA vehicle(3 in ten years)

Space Policy Commission under cabinet office intends to guarantee predetermined steady annual budget for space

science and exploration for ISAS/JAXA to maintain its excellent scientific activities

Competitively-chosen medium-sized focused missions (<150M$ class) with Epsilon rocket(every 2 year)

Missions of opportunity (10M$ per year) for foreign agency-led mission, sounding rocket, ISS

SPICA

JUICE

Call for Missionssoon

2010 2020 2030

Strategic(3/10yrs)HIIA

M-class(1/2yrs)Epsilon

S-class

Hayabusa2

Hisaki

SPICA

CLASP(NAOJ-NASA-CNES) ATHENA(ESA)

Three lines for ISAS science missions

BepiColombo

Mission for AO#3Mission for AO#4

New AO

ERG

Astro-H

JUICE(ESA) WFIRST(NASA)

New space science project approved by ISAS

Space Science Communities Space Engineering Communities

Scheme for Project Creation/Selection

Steering Committee ofSpace Science

Mission proposals in response to AO

Working Groups for Project PreparationIncubation, technical & funding supports by ISAS

Steering Committee ofSpace Engineering

Active Working Groups

- International X-ray Observatory (ATHENA) WG- Wide-field Imaging Surveyor for High-redshift(WISH) WG- General Anti-Particle Spectrometer （GAPS) WG- Japanese Terrestrial Planet Finder(JTPF)WG-JUpiter ICy moon explorer ( JUICE) WG- Luna-GLOB Penetrator WG - Solar Observatory Satellite（Solar-C) WG- Mars Atmospheric Escape Study WG- Mars Exploration with a Lander and OrbiterS (MELOS)WG-JEM-EUSO WG

(Small Scientific Satellite)- High-z Gamma-ray bursts for Unraveling the Dark Ages

Mission(Hiz-GUNDUM) WG- Formation Flight All Sky Telescope（FFSAT) WG- Precise Positioning Mission with a micro-Satellite （PPM-sat) WG - Compton telescope for Astro and Solar Terrestrial (CAST) WG - Gravitational DECIGO Pathfinder (DPF) WG- Diffuse Intergalactic Oxygen Surveyor （DIOS) WG- Polarimetry Satellite （POLARIS) WG- Japan Astrometry Satellite Mission for INfrared Exploration(JASMINE) WG

- Lite (light) satellite for the studies of B-mode polarization and Inflation from cosmic background Radiatio Detection(LiteBIRD) WG

- Solar Sail WG- Studies on the Technology for Exploration of

Planetary Surface(STEPS) WG- Hybrid rocket WG

- Spaceplane Engineering Demonstrator (SEED) WG- Formation flying technology WG

- Advanced Solid Rocket R&D WG- next generation small standard bus technology WG- Mars Airplane Exploration (MELOS)WG

(Small Scientific Satellite)- Solar Power Plant Technology Demonstration WG- Smart Lander for Investigating Moon WG- Magnet plasma Sail WG- Demonstration and Experiment of Space Technology for INterplanetary voYage (DESTINY) WG

Steering Committee for Space Science Steering Committee for Space Engineering

Exceptional success UK-Japan Collaboration in Solar Physics

Hinotori, SMM1980-1982195 kg, 2tSOX, XRP

Yohkoh1991-2001390 kgBCS

Hinode2006 -900 kgEIS

Magnetic reconnection as the origin of solar magnetic activity

Solar magnetic fields, dynamics of solar plasmas

SpacecraftOperation PeriodWeightInstrument

Solar-C2020 -4tSUVIT/EUVST

Initiation of high-energysolar physics

3D structure of magnetic field

Fundamentalphysical

Chromosphericcoronal heatingSolar activity

prediction.

1980 1990 2000 2010

SMM

NASA-UK X-ray polychrometer

NAOJ SOX

Yohkoh

Bragg Crystal Spectrometer

Hinotori

EUV Imaging Spectrometer

HinodeSolar-C

Development in spectroscopy through UK-Japan Collaboration(MSSL/UCL and RAL)

80’ High spectral resolution

90’ High sensitivityHigh cadence

20’ High-speed imaging spectroscopy, IFU,Spectro-polarimetry

06’ Imaging-spectroscopy EUV line-profiles

ISAS-UK X-ray satellite Ginga (1987-1991) was only international X-ray

observatory due to the loss of a space shuttle Challenger, and played a vital

role to continue the X-ray astrophysics. Ginga carried the

Leicester U. Large Area Proportional Counter developed

under UK-Japan collaboration.

GINGA was the first Large-scale Japan-UK Collaboration in SpaceFriendship relation between Prof. Pounds and Prof. Oda helped

Key discoveries X-rays from supernova

SN1987A appeared immediately after launch.

Galactic black-holes: from candidates to reality

Iron-line astrophysics: stellar coronae, supernova remnants, Galactic plane, and clusters of galaxies.

Frequent exchange of personnels Sharing the scientific outcome together

400Kg

1980 1990 2000 2010(Year)

Rapid and continued development in X-ray Astronomy —From UK-Japan Ginga to international ASTRO-H —

Rapid and continued development in X-ray Astronomy —From UK-Japan Ginga to international ASTRO-H —

EXOSAT XMM-Newton

ROSAT

ChandraEinstein

Beppo-SAX

RXTE SwiftNuSTAR

Granat

2020

GingaASCA

Suzaku

ASTRO-H

HakuchoTenma

X-ray Astronomy Missions for 4 decades

JapanASTRO-H

Weight: 2.7tLaunch (planned):2015

UK SWG MembersProf. Andy FabianProf. Chris Done

UK SWG MembersProf. Andy FabianProf. Chris Done

Most recent mission • High-resolution

spectroscopy • Wide band from 0.3

to 600 keV

Most recent mission • High-resolution

spectroscopy • Wide band from 0.3

to 600 keV

Infrared Space Astronomy in Japanleading to JAXA-ESA SPICA mission

Balloon1970’s-80’s

SFU/IRTS1995

AKARI(ASTRO-F)2006-2011

SPICA2024

▲▲ ▲ ▲

Collaboration with UK AKARI to SPICAThe AKARI European consortium (Imperial College London, U.kent, U. Sussex etc) actively involved in the AKARI project. The original SPICA consortium had been led by RAL, and the SPICA proposal to the ESA Cosmic Vision program was submitted by the consortium with RAL as a PI institute in 2007. UK is a key player , and is in charge of the development of key components, e.g. far-infrared detectors (Cambridge U. with Netherlands) and far-infrared filters (Cardiff U.).

SPICA Key Specifications• Telescope: 3.2m cooled to 6K• Wavelength: 20-430 microns• Instrument: SAFARI, MCS, (BLISS)• Orbit: Sun-Earth L2 Halo

Cosmic history from big bang to life• Birth and Evolution of galaxies• Formation processes of stellar

planetary systems• Life cycle of complex material in our

universe

SPICA (2024)JWST (2018)

TMT 30m (2021)E-ELT 39m(2020’s) ALMA

Golden age in astrophysics with SPICA2020’s and beyond

SPICA (2024)JWST (2018)

TMT 30m (2021)E-ELT 39m(2020’s) ALMA

Golden age in astrophysics with SPICA2020’s and beyond

Japan (NAOJ) – UK (SERC/PPARC/STFC) Collaborationin Radio and Optical/Infrared Astronomy

1980s – 2000Nobeyama Radio Observatory – UKIRT/JCMT collaboration

Molecular lines studies using the same high angular resolutions

Discovery of fluorescent H2 emission, etc.SCUBA-POL (JCMT) collaboration

Adding polarimetric capability to JCMT SCUBA

2000-Subaru Telescope – UKIRT/JCMT collaboration

Ultra Deep Survey at the Subaru/XMM Deep FieldFirst detection of a primordial galaxy seen during itsformation, etc.

Joint development of FMOS (Fiber Multi-Object Spectrograph)

☝︎ A giant Lyman alpha emiter (primordial galaxy) located at redshift=6.6 discovered in the

Subaru/XMM Deep field (Ouchi et al. 2009)

Initial science results with the First Sound Project to make a 3D galaxy map at 10 billion light years away using FMOS ☞

Dark matterGravitational wave

ISAS scope

Fundamental physics(KEK, ICRR, IPMU)

Kagura, kamiokande, KEK-B, CERN-ATLAS,

ILC

Dark energy, Dark matter2nd Earth

Search for bio-maker & lifeAstronomy from

ground (NAOJ)TMT-ALMA-Subaru

Non-thermal universe2nd Earth

Search for bio-maker&life

Astronomyfrom space

(ISAS)

Space science in Japan: Big picture

space engineering (ISAS)

Planetary science (ISAS)Remote sensing obs.In-site obs&analysis

Sample-return

Potential candidates for future collaboration

• SPICA: Revealing the origin and evolution of galaxies and birth of planetary systems via high-sensitivity far-infrared observations

• Solar-C: Unveiling the elementary magnetic structures that govern the dynamics solar atmosphere via high spatial resolution/cadence spectroscopic and polarimetric observations.

• Asteroid/Planetary exploration• LiteBIRD: Testing cosmic inflation and quantum gravity

theories via full-sky Cosmic Microwave Background polarization survey

• WISH: Exploring the first generation galaxies and the re-ionization of the universe via deep- and wide-field near-infrared survey

Summary• International collaboration allows us to realize

most advanced missions otherwise difficult to implement by bringing together technologies, competent people and money as our history shows.

• UK and Japan have been having intimate and mutually-fruitful collaborations in space science, especially in the area of solar physics and X-ray astronomy as well as in ground-based astronomy in the past 20 years.

• These existing lines of collaborations with immense heritage should be enhanced in the coming era, while collaborations in new research areas should be developed. We have solid ground to do this.

Thank you

Addendum

Hayabusa2 : Nominal Payloads for SciencePayloads Specifications Comments

Multiband Imager (ONC-T)

Wavelength: 0.4 – 1.0 μm, FOV: 5.7 deg x 5.7 deg, Pixel Number: 1024 x 1024 pxfilter (ul, b, v, w, x, p, Wide)

Heritage of Hayabusa(modified)

Near IR Spectrometer(NIRS3)

Wavelength: 1.8 – 3.2 μm, FOV: 0.1 deg x 0.1 deg

Heritage of Hayabusa, but but 3mm range is new

Thermal IR Imager (TIR)

Wavelength: 8 – 12 μm, FOV: 12 deg x 16 deg, Pixel Number: 320 x 240 px

Heritage of Akatsuki

Laser Altimeter (LIDAR) Measurement Range: 50 m – 50 km Heritage of Hayabusa(modified)

Sampler Minor modifications from Hayabusa-1 Heritage of Hayabusa(modified)

Small Carry-on Impactor (SCI)

Small system released form the spacecraft to form an artificial crater on the surface

New

Separation Camera (DCAM)

Small, detached camera to watch operation of Small Carry-on Impactor

Heritage of Ikaros(modified)

Small Rover (MINERVA II-1, II-2)

Similar to MINERVA of Hayabusa-1(possible payload: Cameras, thermometers)

Heritage of Hayabusa(largely modified)

Small Rover (MASCOT)

Supplied from DLR & CNESMicrOmega, MAG, CAM, MARA

New

49

Solar-C

Spacecraft JAXALaunch vehicle JAXASUVIT Large-aperture telescope JAXA (with feed optics to focal plane)

Primary/secondary mirror ESA (with test flat)Focal plane instrumentFiltergraph NASASpectro-polarimeter JAXA-led international consortium

EUVST ESA/NASAXIT Normal incidence NASA

Grazing incidence (optional) TBD

NASA contribution: It is a high priority of the SHP Panel that NASA and its partners form a Science and Technology Definition Team for Solar-C as soon as possible. The panel expects that NASA contributions would involve the most technically challenging elements, such as the focal-plane packages (cameras, detectors, and so on), which would afford the U.S. science community an opportunity to make critical advances in remote-sensing capabilities.

The total cost to NASA through Phase E should be capped at $250 million. Solar-C presents a unique opportunity for solar and space physics to make flagship-level science advances for the cost of an

FY2014: Pre-project (phase-A)FY2015-16: Basic design

(phase-B), PDRFY2016-17: Detailed design

(phase-C), CDRFY2018-20: Fabrication,

testing (phase-D),

PQR/PSRFY2020 - : Launch,

Understand solar and heliospheric magnetic activityDevelop an understanding of the magnetic coupling of convection zone – photosphere – chromosphere –transition region and corona

Develop and observationally test algorithms for solaractivity prediction

JAXA-based working group with more than 70 members & contributors from JAXA, NAOJ, Kyoto U., Nagoya U., Riken, NIST, LMSAL/US, HAO/US, HSAC/US, MPS/DE, IAC/ES, and MSSL/UK [Working group PI: Tetsuya Watanabe (NAOJ)]

Selected as one of eight most important future projects by astronomy/astrophysics division of Science Council of Japan

Recognized as one of key future JAXA missions in solar and heliospheric physics

Expected to include substantial contributions from the UnitedStates and Europe

3D magnetic structure in the solar atmosphere Solar flare prediction – contribution to SW and SSA Chromospheric and coronal heating - Origin of solar wind Fundamental plasma processes - Magnetic

reconnection

a fundamentally new way of viewing the entire solar atmosphere, essentially with the same high spatial and temporal resolution, in addition to performing simultaneous high resolution spectropolarimetric measurements for the first time.

a very challenging mission to design, develop, scientifically and technically, and to deliver an order-of-magnitude improvement over present measurement capabilities.

SUVIT: UV Optical IR TelescopeAperture: 1.5 m diameterFocal Instruments:wide & narrow band imagerspectropolarimeter (2D)

XIT: X-ray Imaging TelescopeNormal incidence EUV imagerangular res.: 0.2" arcsec

(optional) Grazing incidence soft X-ray imagerCMOS-based Ph-counting with 1" ang. res.

EUVST: (UV/)EUV Imaging Spectrometer/LEMURAngular resolution: 0.3 arcsecWavelength: 17-130 nmTemperature coverage: 0.01 - 20 MK

Mission Goals

Project Status/Plan

Distinct Features

Expected Achievements

US-Japan Collaboration

International Task Shares

Schedules(Earliest Possible)

Model Payloads

Fundamental research for space weather

LiteBIRD Lite (Light) Satellite for the Studies of B-mode Polarization and Inflation from Cosmic Background Radiation Detection

100mK focal plane w/multi-chroicsuperconductingdetector array

System overviewScientific objectives

Tests of cosmic inflation and quantum gravity theories with unprecedented precision

Search for primordial gravitational waves to the lower bound of well-motivated inflationary models

-Full success: dr < 0.001 (dr is the total uncertainties on tensor-to-scalar ratio, which is a fundamental cosmology parameter related to the power of primordial gravitational waves)

Expected achievements

Cosmology and Particle Physics-Discovery of primordial gravitational waves-Narrowing down cosmic inflation models-Narrowing down quantum gravity theories-Shed light on fundamental laws of physics

Astronomy-Cosmic reionization-Galactic haze emission-Galactic magnetic fields-Polarized dust emission

Observations Full-sky CMB polarization

survey at a degree scale(30arcmin @ 150 GHz)

6 bands b/w 50 and 320 GHz

Strategy Part of technology verification

from ground-based projects Synergy with ground-based

large telescopes Synergy w/ X-ray mission R&D

Project status/plan International collaboration JAXA-based working group w/ more than 60 members from JAXA,

Kavli IPMU, KEK, NAOJ, UC Berkeley/LBNL, McGill, Riken, MPA and Japanese universities (Working group PI: Masashi Hazumi (KEK))

Selected as one of eight most important future projects by astronomy/astrophysics division of Science Council of Japan

Recognized as one of key future JAXA missions in fundamental physics

To be ready for Mission Definition Review by March 2014 Target launch year ~2020

LiteBIRD working group is already international-US PI of LiteBIRD: Adrian T. Lee (UC Berkeley/LBNL)

Strong collaboration among some of LiteBIRD members also exists for ground-based projects

-POLARBEAR, POLARBEAR-2, Simons Array US contributions in various components are possible

-Superconducting detector array-Cryogenics-Optics

Continuously-rotating HWP w/ 30 cm diameter

60 cm primary mirror w/ Cross-Dragone configuration (4K)

JT/ST + ADR w/heritages ofX-ray missions

Major specifications Orbit: L2 (Twilight LEO ~600km as an option) Weight: ~1300kg Power: ~2000W Observing time: > 2 years Spin rate: ~0.1rpm

WISH█ Explore the universe beyond Cosmic Reionization :

Studying the earliest galaxy formation at z=8-15 █ Cosmic Expansion History with SNIa (type Ia Supernovae)NIR detection and light curves of SNIa at z=0-2█ Deep and Wide-field NIR Survey at 1-5μmVarious fields in astronomy

██ Dedicated deep and wide-field imaging surveys at 1-5μm█ Survey strategy: 100deg2, 28AB (5σ), 6 broad bands (main survey)

█ 1.5m light-weighted glass primary mirror█ CFRP structure @90-100K█ Diffraction limited image at 1-5μm over the flat focal plane█ H2RG 32x2kx2k 128Mpix█ 0.155”/pixel(18μm-pitch), 850arcmin2/FoV█ Light weight: 1.4t (WET)

█ JAXA/ISAS WISH Working Group since 2008 (pre Phase A)█ JAXA/ISAS R&D budget (~1M$, without including man power cost)█ WISH Mission Proposal Draft distributed (2012, in Japanese)█ Potential international Partners: SAO (USA), LAM (France), Canada█ Proposed Schedule: 2014 Mission Definition Review,2016 System Definition Review, Launch by ~2020 █ Expected Cost (w/o launch, operation, data facility) : 250-300M$

█ Collaboration with France optional narrow-field IFU spectrograph(lead by LAM, MoO proposal submitted to CNES)

■ Collaboration with USA detector testing and procurement(lead by SAO, MoO proposal submitted to NASA)

■ Collaboration with Canada, under discussion

Comparison with Euclid WISH is optimized for very high-redshift galaxies and cosmology (SNe), while Euclid is optimized for cosmology (WL, clustering). Euclid has optical imaging, NIR photometry and NIR wide-field spectroscopy.█ uniqueness of WISH:

- higher-resolution (Euclid IR photometer 0.3”/pix) - imaging at 1-5μm (Euclid IR photometer 0.9-2μm)- different survey strategy [WISH UDS: 28AB, 100deg2 / Euclid 24AB (wide) 26AB (deep)]█ similarity:

- primary mirror size (Euclid1.2m), field of view (Euclid 0.5deg), number of pixels (Euclid 96Mpix)

Comparison with WFIRST (AFTA 2.4m)WISH is optimized for very high-redshift galaxies and cosmology (SNe), while WFIRST is optimized for cosmology (SNe, clustering), exolanets, and IR surveys. WFIRST has NIR imaging and wide-field spectroscopy.█ uniqueness of WISH:

- imaging at 1-5μm (0.9-2μm for WFIRST)- earlier launch schedule (proposed)█ similarity: - AFTA 2.4m option may achieve comparable depth (27AB) over

significantly larger area (2500deg2)Comparison with JWST█ uniqueness of WISH:

- wide-field (JWST NIRCam <20 arcmin2)█ synergy: - WISH provides unique and feasible targets for JWST spectroscopy

Synergy with SPICASPICA studies dust emission / dust-free fine structure lines of galaxies while WISH observes the stellar components of high-z galaxies█ WISH core wavelength: 1-5μm SPICA core wavelength 5-210μmSynergy with Extremely Large Telescopes█ WISH survey depth (<28AB) is well matched with

the AO-assisted NIR spectroscopic capability of ELTs.

Science Goals

Key Features

Base Design Model

Current Status

International Collaboration

Comparison

Wide-field Imaging Surveyor for High-redshift