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 ArrayCCD Image

Reconstruction from visibility measurements

1D non-redundant

array

Interferogram

First lab-demonstration of image reconstruction by using a pupil remapping system

T. Kotania,b, S. Lacourb, E. Choqueb, G. Perrinb, P. Fedoub

aISAS/JAXA, bLESIA, Observatoire de Paris, section Meudon, France

Speckle Nulling Demonstration

A Wavefront Correction System for SPICA Coronagraph Instrument

T. Kotani1, K. Enya1, T. Nakagawa1, L. Abe2, T. Miyata3, S. Sako3, T. Nakamura3, K. Haze1,4, S. Higuchi1,3, Y. Tange5

SPICA and Coronagraph Instrument

PSF

- Laboratory testbed (at room temperature) - Contrast of over 106 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

CandidatePupil 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 106 contrast

Wavefront correction system Over 106 contrast

at 3.5 ~10 λ/DAfter Speckle nulling

Before Speckle nulling

over 106 contrast from 3.5 to 10 λ/D

All Sky Transit Observer (ASTrO)

Table 1. Planets In Monte Carlo Simulation For Unconfused Sky*

Single Transit SNR

All Spectral Type Hosts

M Star Hosts

Nominal Sensitivity

Nominal Sensitivity

Gas/Icy Rocky Gas/Icy Rocky Low (3-10) 210 666 129 134 Med (10-50) 828 32 326 14 High (>50) 688 0 216 0 Total 1726 698 671 148 *2×106 stars in unconfused 60% of sky; Final SNR32>7; # Transits/star> 3. Including low galactic latitudes, |gal. lat.|<20o, will add ~ 20% more objects

• Spacecraft with 24 cameras (10 cm) @ L2• Operation at 1.6 mm 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

Dynamical stability in the habitable zones of nearby extrasolar planetary systems

B. Funk1, E. Pilat-Lohinger2, Á. Süli1, R. Schwarz2, S. Eggl2

1: Department of Astronomy - Eötvös Loránd University - Budapest2: 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

Ground-based Transmission Spectrocopy Projectwith 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

Discovery of a Retrograde ExoplanetNarita 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

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. Schwarz1, B. Funk2, E. Pilat Lohinger1

1: Institute for Astronomy – University of Vienna, Austria 2: Department of Astronomy – Eötvös University, Budapest

Poster Nr. 53

National Aeronautics and Space AdministrationJet Propulsion LaboratoryCalifornia Institute of Technology

SIM

Lite

AST

ROM

ETRI

C OBS

ERVA

TORY

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 chopsbetween 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.

9/10/2009 10Renaud Goullioud

Science

Guide 4.2-meter BaselineGuide 1

Guide 2

Science

Bay 1

AstrometricBeam Combiners

Bay 2

Guide 1

Science 6-meter Baseline

T

R1

R2

R3

R4