Oct.10, 2007 EAMA7

Japanese Space Activity on Exoplanets (JAXA’s prespective) &

Pathways to Habitable PlanetsSeptember 16, 2009Takao Nakagawa (ISAS/JAXA)

Where are we from ?

Are we alone ?

Scientific Goals What are the conditions for planetary

formation ? Incl. detection and characterization of habitable

planets. Formation of proto-planetary disk

Condensation of dust Formation and growth of

planetesimals Formation of rocky planets

and planetary cores Formation of giant planets Dissipation of gasDiversity and Unified

Scheme

Synergy

Planetary Science In situ measurements

Astronomy Remote Sensing

Hayabusa’s view of Itokawa AKARI’s view of HIP7978

Strategy to reveal the conditions of Planetary Formations

Protoplanetary disk Line spectroscopy in MIR~FIR (~mm)

IR Obs: Inner disk, complementary to ALMA

Condensation of dust and formation of planetesimals Thermal imaging in MIR and FIR

Formation of Giant Planets Direct detection and spectroscopy : MIR coronagraph Spectroscopy using transits: Stable MIR Spectrometer

Dissipation of Gas Sensitive MIR spectrometer (H2)

Formation of Habitable planets Detection of biomarkers

Overview of SPICA

Sun

L1 L2

L4

L5

Earth

L3

Mission Overview Specifications

Telescope: 3.5m, 5 K Revolving CIB at its energy peak Foramtion of Planetary Systems

Core wavelength: 5-210 μm MIR Instrument

Including Coronagraph & Spectro. Far-Infrared Instrument (SAFARI)

Orbit: Sun-Earth L2 Halo Mission Life

3 years (nominal) 5 years (goal) No expendables

Weight: 3.6 t Launch: 2018

Focal Plane Instruments

λ

v

2 m

20 m

200 m

300(100 km s-1)

3000(100 km s-1)

30000(10 km s-1)

HerschelJWST

WIDE FOV

SPICA

Unique Capability optimized for mid- and far-infrared

Good

Sensitivity

Huge Gain of Sensitivity !

2.5 orders

SPICASPICA/SAFARI

2 orders

Herschel

Photometry Spectroscopy

SPICA for the study of formation process of

planets

Disk Meneralogy and Snow Line

Characterization of Giant Planets

SPICA Coronagraphy High Contrast (106-7) Continuous Spectral Coverage

with R~200 λ ~ 3.5 – 28μm

Moderate IWA (~1”) Transit Spectroscopy

High dynamic range (fast readout)

Pointing Stability FPC-G for stability IFU for good photometric

stability Characterization of IR detectors

Dofocusing Model Atmosphere by Burrows et al. (2003) For 2Mj, 100 Myr planets around G2V starSimulated for SPICA coronagraph (Kotani)

SPICA as an International Mission

16

International Collaboration Scheme

ESAI/F Management

SAFARI Consortium

System Integration

EuropeanTeams

JapaneseTeams

FPI : SAFARI

ESAManufacturing（ test @ 80K ）

JAXAIntegration（ test @<10K ）

Telescope

JAXASubsystemIntegrator

Japanese Group

Korean Team (TBD)

NAOJ (TBD)

FPI:MIRs ＋ SCI

JAXA SPICA team: System Integration

SPICA Steering Committee

FPI:FPCFPI:BLISS

NASA Team

(TBD)

※ FPI : Focal Plane Instrument SAFARI : SPICA Far-Infrared Instrument MIRs : Mid Infrared Insturuments (MIRACLE,MIRMES,MIRHES) BLISS : Background-Limited Infrared-Submikimeter Spectrograph FPC : Focal Plane finding Camera

Science Advisory Committee

Join

t Syst

em

Engin

eeri

ng

Team

Schedule

APPROVED

APPROVED

Project Approval Review

CV Down SelectionCV Final Selection

Japanese Perspectiveon Pathways to Habitable

Planets

Japanese Perspective The enterprise to achieve the ultimate

goal (detection and characterization of habitable planets) should be international JTPF WG activity (M. Tamura’ s talk)

Concrete and coherent strategy with important mile stones. SPICA is a very important mile stone

Scientific achievements Technology development

R&D strategy Coronagraph

SPICA Enya’s talk Posters (Kotani, Haze)

Interferometry FITE (Shibai’s poster)

Test Bed Small satellite series

E.G. 60cm telescope on ASNARO

Space Odyssey in 2018

Where are we from ?

Are we alone ?