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A quick review of tesbed imagers

A quick review of tesbed imagers. Laurent Koechlin. Laboratoire d'astrophysique de Toulouse Tarbes, Université de Toulouse CNRS. Research on these testbeds is financed by. Tesbed imagers. 2x2 cm array. I have it here, It's working. live demo For those who Haven't already Seen it….

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A quick review of tesbed imagers

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  1. A quick review of tesbed imagers Laurent Koechlin Laboratoire d'astrophysique de Toulouse Tarbes, Université de Toulouse CNRS

  2. Research on these testbeds is financed by Tesbed imagers

  3. 2x2 cm array I have it here, It's working. live demo For those who Haven't already Seen it…

  4. Testbed Gen I (2005-2009): 8x8 cm array Will be presented by Denis Serre 116 zones, 8 x 8 cm 26680 apertures "orthocircular" design. F= 23 m at = 600 nm Precision: 5m on holes positioning =>/70 on wavefront. Achievements: Diffraction limited Broad band imaging (450-850nm) 10-6dynamic range metal foil 100 m thick Photo T.Raksasataya

  5. Testbed Gen II: 20x20 cm, on sky sources (2009-2011) 0.8" resolution 1000x1000 field λ0 = 800 nm Δλ = 100 nm Implementation of testbed Gen II at Nice observatory will be presented by Jean-Pierre Rivet Photo D.Serre

  6. 20 cm Metal foil 9.7 105 apertures, Slightly apodized, 696 Fresnel zones. Photo P.Deba

  7. Testbed Gen II Results & targets will be presented by Truswin Raksasataya First light on a star done July 17th Not yet the nominal optics

  8. Goals and first results of testbed Gen II Will be presented by Truswin Raksasataya Assess performances on real sky objects: do better than other 20 cm aperture instruments. Targets: Dynamic range on real stars Limiting magnitude

  9. Assessment of a membrane telescopeis currently envisioned by ESA

  10. Space mission proposal We have a concept that opens the way to very large apertures in space. It can be validated on ground based facilities only for small apertures. Large apertures need to be tested in space, but it's hard to get a large mission approved if it's based on a new technology. Science cases? Credibility?

  11. Rationale Meet acceptability threshold for a new technology mission Make it simple, try to keep the cost below 300 M€ Scientific return over cost:must be higher than that ofcompeting concepts λ/50 wavefront, at any λ => High Dynamic range from IR to UV mas angular resolution 1000x1000 resel. fields Spectral resolution Suitable for several astrophysical fields...

  12. The Fresnel Imager Space Mission 3m to 100m diameter, or more. Thin membrane "Primary Array" module: Field optics telescope 1/10th to 1/20th the diameter of Primary Array. Dispersion correction: order -1 diffraction Blazed lens or concave grating, 10 to 30 cm diameter focal Instrumentation: Spectro-imagers

  13. Strategy, sky targets - Start with UV domain? - limited budget => limited aperture, but high resolution - High quality wavefront at any wavelength - angular resolution : 7 mas with a 4m Fresnel array - The UV universe is almost unknown at these resolution and dynamic range

  14. Space Mission: optical scheme Spacecraft 1 Solar Baffle, to protect from sunlight Large "Primary Fresnel Array: Thin foil, 4 to 30 m diameter, or more. Field optics telescope Order zero blocked Focal instrum. Diffraction order 1: focused, but with chromatic aberration. Spacecraft 2 pupil plane Diffraction order 0: unfocussed will be focused by field optics, then blocked. Focal instruments Chromatic correction: Blazed Fresnel grating 5 km (for a 4m aperture) to 100 km (for a 30m aperture) image plane 1dispersed image plane 2 achromatic

  15. Goals and conception of testbed Gen III:UV domain • Before proposing a UV space mission, • we need to validate the technology in the UV. • Build a testbed to validate : - the dynamic range, - wavefront quality, - angular resolution, - spectral bandwidth, - light transmission efficiency. Will be presented by Paul Deba

  16. Testbed Gen III: UV domain Will be presented by Paul Deba R&T financed by CNES & STAE Size : 8 cm, square 240 Fresnel zones (110 000 apertures) metal sheet 100 m thick, laser carved Operates in the UV (250-350 nm) Focal length: 26.6 m for = 250 nm Precision on array : 5m i.e./30 on wavefront

  17. Targets: S/N on exoplanets in UV Signal / noise as a function of  uv uv Signal / noise > 30 0.5 Jupiter diameter 1 Jupiter diameter planet Signal / noise > 3 Signal / noise < 3 Signal / noise > 3 Signal / noise < 3 Images & spectra of exoplanets: 1 UA from solar type star, 10Pc away 4m aperture, 10h integration spectral res.  /= 50 dynamic range of raw image: 2 10^-8

  18. Conclusion: Future space mission. Build up a proposal for a 2020 / 2025 launch Science cases: Exoplanets stellar physics compact objects reflection nebulae extragalactic solar system objects observation of the earth

  19. Thank you for your attention!

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