2. Redundant Array + Corrugated Wavefront Non-Redundant Array + Spatially Filtered Wavefront Single-mode fibers Lenslet array Flat wavefront after calibration A laboratory demonstration of high dynamic range imaging using single- mode fiber pupil remapping system FIRST 2D-Fiber Array CCD Image Reconstruction from visibility measurements 1D non- redundant array Interferogram First lab-demonstration of image reconstruction by using a pupil remapping system T. Kotani a,b, S. Lacour b, E. Choque b, G. Perrin b, P. Fedou b a ISAS/JAXA, b LESIA, Observatoire de Paris, section Meudon, France

3. 10 λ/D Speckle Nulling Demonstration A Wavefront Correction System for SPICA Coronagraph Instrument T. Kotani 1, K. Enya 1, T. Nakagawa 1, L. Abe 2, T. Miyata 3, S. Sako 3, T. Nakamura 3, K. Haze 1,4, S. Higuchi 1,3, Y. Tange 5 SPICA and Coronagraph Instrument PSF - Laboratory testbed (at room temperature) - Contrast of over 10 6 from 3.5 to 10 λ/D region - Cryogenic test-bed is being built at JAXA - MEMS deformable mirror (DM) and a fast tip-tilt correction system - will have a potential of higher contrast than coronagraphs of JWST Candidate Pupil Mask 3D layout of Coronagraph Optics SPICA telescope 1: ISAS/JAXA; 2: Université de Nice-Sophia Antipolis; 3: University of Tokyo; 4: The Graduate University for Advanced Studies; 5: EORC/JAXA - SPICA is the Japanese led, joint JAXA-ESA mission - 3-meter class cryogenic space telescope - Coronagraph Instrument for characterization of Jovian planets from 3.5 to 27 μm - High-contrast imaging and spectroscopy (R=200) up to 10 6 contrast Wavefront correction system Over 10 6 contrast at 3.5 ~10 λ/D After Speckle nulling Before Speckle nulling over 10 6 contrast from 3.5 to 10 λ/D

5. All Sky Transit Observer (ASTrO) Spacecraft with 24 cameras (10 cm) @ L2 Operation at 1.6  m emphasizes M stars Continuously monitor 24% of sky for 60d 2 million stars in unconfused sky (>60%) >2,000 planets overall; >150 rocky planets in/near HZ of nearby M stars Bright targets for spectroscopic follow-up No new technology Probe Class, $500-600M, dep. on launch vehicle

6. Dynamical stability in the habitable zones of nearby extrasolar planetary systems B. Funk 1, E. Pilat-Lohinger 2, Á. Süli 1, R. Schwarz 2, S. Eggl 2 1: Department of Astronomy - Eötvös Loránd University - Budapest 2: Institute for Astronomy - University of Vienna http://www.univie.ac.at/adg/hzcat/ This investigation tackles the dynamical stability of potential additional terrestrial planets in nearby (within 30 pc) extrasolar planetary systems. Poster 54

7. Ground-based Transmission Spectrocopy Project with the Subaru HDS Norio Narita (NAOJ) and the Subaru HDS collaboration Result of HD189733b: 2007 July 12 Other targets and nights: HD189733b: 2 nights (2009) HD149026b: 2 nights (2009) HAT-P-2b: 1 night (2009) HD17156b: 1 night (2009) HD80606b: 1 night (2010) Poster No.81

8. Discovery of a Retrograde Exoplanet Narita N., Sato B., Hirano T., Tamura M. (2009) PASJ Letters, Vol. 61, L35-L40 (arXiv:0908.1673) The Rossiter-McLaughlin Effect of HAT-P-7b Poster No.82

9. The scheme for the three different models: (upper graph) stability for a compact close-in systems with 11planets with a star of 0.3 Msun (middle graph) stability of planets in the HZ for 0.3 Msun and 0.5 Msun (lower graph). Habitable planets in compact close-in planetary systems R. Schwarz 1, B. Funk 2, E. Pilat Lohinger 1 1: Institute for Astronomy – University of Vienna, Austria 2: Department of Astronomy – Eötvös University, Budapest Poster Nr. 53

10. National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology SIM Lite A STROMETRIC O BSERVATORY CALTECH SIM-Lite Instrument Description, Operation and Performance SIM Lite would search about 60-100 nearby Sun-like stars for planets of mass down to one Earth mass, in the Habitable Zone. SIM-Lite will also perform global astrometry on a variety of astrophysics objects, reaching 4 μas absolute position and parallax measurement accuracy on objects brighter than 16th visual magnitude and 10 μas at magnitude 20. The instrument consists of: – A 6m Optical Michelson stellar interferometer – A 4.2m “Guide” Michelson stellar interferometer – A 30cm “Guide” Telescope. The first interferometer chops between the target star and a set of reference stars. The second interferometer monitors the attitude of the instrument in the direction of the target star. The telescope monitors the attitude of the instrument in the other two directions. 9/10/200910Renaud Goullioud Science Guide 4.2-meter Baseline Guide 1 Guide 2 Science Bay 1 Astrometric Beam Combiners Bay 2 Guide 1 Science 6-meter Baseline T R1R1 R2R2 R3R3 R4R4