redundant array + corrugated wavefront
DESCRIPTION
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. - PowerPoint PPT PresentationTRANSCRIPT
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