1. Oct.10, 2007EAMA7 Japanese Space Activity on Exoplanets (JAXAs prespective) & Pathways to Habitable Planets September 16, 2009 Takao Nakagawa (ISAS/JAXA)

2. Where are we from ? Are we alone ?

3. 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 gas Diversity and Unified Scheme

4. Synergy Planetary Science In situ measurements Astronomy Remote Sensing Hayabusas view of ItokawaAKARIs view of HIP7978

5. 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

6. Overview of SPICA

7. 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

8. Focal Plane Instruments λ v 2 m20 m200 m 300 (100 km s -1 ) 3000 (100 km s -1 ) 30000 (10 km s -1 ) Herschel JWST WIDE FOV SPICA Unique Capability optimized for mid- and far-infrared Good Sensitivity

9. Huge Gain of Sensitivity ! 2.5 orders SPICA SPICA/ SAFARI 2 orders Herschel PhotometrySpectroscopy

10. SPICA for the study of formation process of planets

13. Disk Meneralogy and Snow Line

14. Characterization of Giant Planets SPICA Coronagraphy High Contrast (10 6-7 ) 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 star Simulated for SPICA coronagraph (Kotani)

15. SPICA as an International Mission

16. 16 International Collaboration Scheme ESA I/F Management SAFARI Consortium System Integration European Teams Japanese Teams FPI : SAFARI ESA Manufacturing test @ 80K JAXA Integration test @<10K Telescope JAXA Subsystem Integrator Japanese Group Korean Team (TBD) NAOJ (TBD) FPI:MIRs SCI JAXA SPICA team: System Integration SPICA Steering Committee FPI:FPC FPI: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 Joint System Engineering Team

17. Schedule APPROVED Project Approval Review CV Down Selection CV Final Selection

18. Japanese Perspective on Pathways to Habitable Planets

19. 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

20. R&D strategy Coronagraph SPICA Enyas talk Posters (Kotani, Haze) Interferometry FITE (Shibais poster) Test Bed Small satellite series E.G. 60cm telescope on ASNARO

21. Space Odyssey in 2018 Where are we from ? Are we alone ?