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FUTURE DEVELOPMENTS IN IR INSTRUMENTATION AT ESO

FUTURE DEVELOPMENTS IN IR INSTRUMENTATION AT ESO. Mark Casali. 1. Photon starved science Detection Basic information. 2. Photon rich science Spatial/astrometric Spectral Polarimetric temporal. 1. Photon starved science. Finding the faintest/most distant objects

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FUTURE DEVELOPMENTS IN IR INSTRUMENTATION AT ESO

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  1. FUTURE DEVELOPMENTS IN IR INSTRUMENTATION AT ESO Mark Casali

  2. 1. Photon starved science Detection Basic information 2. Photon rich science Spatial/astrometric Spectral Polarimetric temporal

  3. 1. Photon starved science • Finding the faintest/most distant objects • The first galaxies. Imaging, spectroscopy • Star formation at high z • High-z clusters • Quasars • T dwarfs and their atmospheres.

  4. VISTA UKATC/RAL • 16 2kx2k VIRGO • 0.34” pixels • 1.70 diameter • ZYJHKs + nb • 2007

  5. VISTA • 16 2kx2k VIRGO • 0.34” pixels • 1.70 diameter • ZYJHKs + nb • 2007

  6. VISTA • 16 2kx2k VIRGO • 0.34” pixels • 1.70 diameter • ZYJHKs + nb • 2007

  7. HAWK-I ESO IR dept • 7.5’ x 7.5’ • 0.1” pixels • Y,J,H,Ks + nb • 90% optics throughput • Nasmyth UT4 • AIT at ESO • Q1 2007 • deep imaging of VISTA targets

  8. HAWK-I • 7.5’ x 7.5’ • 0.1” pixels • Y,J,H,Ks + nb • 90% optics throughput • Nasmyth UT4 • AIT at ESO • Q1 2007 • deep imaging of VISTA targets 10.6’ Maximum Field

  9. Adaptive Optics Facility • Deformable M2 with 1170 voice coils • 1.1m/2mm, 9kg • 2012 • Conjugated to Ground Layer • Seeing improver over wide field • 4 Na Fibre Raman Lasers ESO AO/LGS departments

  10. Adaptive Optics Facility • Deformable M2 with 1170 voice coils • 1.1m/2mm, 9kg • 2012 • Conjugated to Ground Layer • Seeing improver over wide field • 4 Na Fibre Raman Lasers

  11. Adaptive Optics Facility • Deformable M2 with 1170 voice coils • 1.1m/2mm, 9kg • 2012 • Conjugated to Ground Layer • Seeing improver over wide field • 4 Na Fibre Raman Lasers MUSE HAWK-I ?

  12. KMOS UKATC/MPE/USM/U.Durham/U.Oxford • 24 deployable arms/IFUs • 7’ diameter pickoff field • 14x14 spatial elements/IFU • R = 3400-3800 • 3 x 2kx2k H2RG detectors • PDR in May. First light 2010

  13. KMOS UKATC/MPE/USM/U.Durham/U.Oxford • 24 deployable arms/IFUs • 7’ diameter pickoff field • 14x14 spatial elements/IFU • R = 3400-3800 • 3 x 2kx2k H2RG detectors • PDR in May. First light 2010

  14. KMOS UKATC/MPE/USM/U.Durham/U.Oxford • 24 deployable arms/IFUs • 7’ diameter pickoff field • 14x14 spatial elements/IFU • R = 3400-3800 • 3 x 2kx2k H2RG detectors • PDR in May. First light 2010

  15. KMOS UKATC/MPE/USM/U.Durham/U.Oxford • 24 deployable arms/IFUs • 7’ diameter pickoff field • 14x14 spatial elements/IFU • R = 3400-3800 • 3 x 2kx2k H2RG detectors • PDR in May. First light 2010

  16. 2. Photon rich science • young stars – atmospheres and discs • astrometry. Extrasolar planet orbits. Stellar orbits at the galactic centre. • stellar seismology. • nucleosynthesis and chemical evolution • direct detection of photons from extrasolar giant planets • first order characterization exoplanet atmospheres (Clouds, dust content, Methane, water absorption, Effective temperature, radius, dust polarization)

  17. CRIRES R~ 100k Very stable 1-5 microns polarimetry Delivery in next few months ESO IR department/Käufl

  18. CRIRES 4 hybridized Aladdin III Resolution~100k AO front end 5 m/s with gas cells

  19. Visible polarimeter – gas and debris disks, nearby planets in reflection NIR dual imager – Detection of self-luminous planets, secondary science NIR tigertype IFS – Spectral characterisation of self-luminous planets Spectro-Polarimetric High-contrast Exoplanet REsearch LAOG/LAM/LESIA/ONERA/O.Geneve/MPIA/O.Padova/ETH/O.Ams….. 2010

  20. 4x8 milli arcsec K u-v coverage (UT 8 hours d=-15º) Airy disk UT VLTI - PRIMA - 2008 • ESO/IMT/O.Geneve/O.Leiden/MPIA/O.Heidelberg/EPF/MPE/ASTRON • Dual-feed on 2 UTs/ATs • gain of 5 to 6 magnitudes • Phase-Referenced Imaging with AMBER or MIDI • High accuracy differential astrometry

  21. VLTI 2nd Generation Instrumentsproposals for Phase A studies 3-20µm, 4 beams OCA/GEMINI Nice.... 1-2.5µm, 4-6 beams LAOG Grenoble…. 2.2µm, 4x2 beams MPE…. MATISSE VSI GRAVITY

  22. A European effort MPE, Garching USM, Munich ETH, Zurich ATC, Edinburgh MPIA, Heidelberg U of Durham U of Oxford LAOG, Grenoble LAM LESIA EPF, Lausanne ONERA Obs de Geneve LUAN Padova Obs. U of Amsterdam RAL, Didcot Obs. Leiden IMT, Neuchatel ASTRON Obs. Heidelberg

  23. More second generation.. • ESO funding for further second-generation instruments from 2010 • currently discussingthe process ( call for proposals etc.)

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