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A laboratory demonstration of high dynamic range imaging using single-mode fiber pupil remapping system FIRST. 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. Lenslet array. Single-mode fibers.

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slide2

A laboratory demonstration of high dynamic range imaging using single-mode fiber pupil remapping system FIRST

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

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

Lenslet array

Single-mode fibers

Flat wavefront

after calibration

Non-Redundant Array +

Spatially Filtered Wavefront

Redundant Array +

Corrugated Wavefront

1D non-redundant array

Reconstruction

fromvisibility measurements

2D-Fiber Array

Interferogram

CCD Image

First lab-demonstration of image reconstruction

by using a pupil remapping system

slide3

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

1: ISAS/JAXA; 2: Université de Nice-Sophia Antipolis; 3: University of Tokyo; 4: The Graduate University for Advanced Studies; 5: EORC/JAXA

SPICA telescope

Candidate

Pupil Mask

3D layout of Coronagraph Optics

SPICA and Coronagraph Instrument

- 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

PSF

Wavefront correction system

Over 106 contrast

at 3.5 ~10 λ/D

After

Speckle nulling

Before Speckle nulling

  • MEMS deformable mirror (DM) and
  • afast tip-tilt correction system
  • - will have a potential of higher contrast than coronagraphs of JWST

Speckle Nulling Demonstration

- 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

over 106 contrast from 3.5 to 10 λ/D

10 λ/D

all sky transit observer astro
All Sky Transit Observer (ASTrO)
  • 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

Dynamical stability in the habitable zones of nearby extrasolar planetary systems

Poster 54

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

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.

slide7

Ground-based Transmission Spectrocopy Project

with the Subaru HDS

  • Norio Narita (NAOJ) and the Subaru HDS collaboration

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

  • Result of HD189733b: 2007 July 12
discovery of a retrograde exoplanet

Poster No.82

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

slide9

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

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).

sim lite instrument description operation and performance
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.

Science

Guide 1

Guide 2

Guide 4.2-meter Baseline

Guide 1

Science

R2

Bay 1

R1

R3

Science 6-meter Baseline

T

R4

Astrometric

Beam Combiners

Bay 2

Renaud Goullioud