FUTURE DEVELOPMENTS IN IR INSTRUMENTATION AT ESO Mark Casali.

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Presentation transcript:

FUTURE DEVELOPMENTS IN IR INSTRUMENTATION AT ESO Mark Casali

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

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.

VISTA 16 2kx2k VIRGO 16 2kx2k VIRGO 0.34” pixels 0.34” pixels diameter diameter ZYJHKs + nb ZYJHKs + nb UKATC/RAL

VISTA 16 2kx2k VIRGO 16 2kx2k VIRGO 0.34” pixels 0.34” pixels diameter diameter ZYJHKs + nb ZYJHKs + nb

VISTA 16 2kx2k VIRGO 16 2kx2k VIRGO 0.34” pixels 0.34” pixels diameter diameter ZYJHKs + nb ZYJHKs + nb

HAWK-I 7.5’ x 7.5’ 7.5’ x 7.5’ 0.1” pixels 0.1” pixels Y,J,H,Ks + nb Y,J,H,Ks + nb 90% optics 90% opticsthroughput Nasmyth UT4 Nasmyth UT4 AIT at ESO AIT at ESO Q Q deep imaging of VISTA targets deep imaging of VISTA targets ESO IR dept

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

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

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

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

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

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

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

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

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)

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

CRIRES 4 hybridized Aladdin IIIResolution~100k AO front end5 m/s with gas cells

S pectro- P olarimetric H igh-contrast E xoplanet RE search NIR tigertype IFS – Spectral characterisation of self-luminous planets NIR dual imager – Detection of self- luminous planets, secondary science Visible polarimeter – gas and debris disks, nearby planets in reflection LAOG/LAM/LESIA/ONERA/O.Geneve/MPIA/O.Padova/ETH/O.Ams…..2010

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

VLTI 2 nd Generation Instruments proposals for Phase A studies MATISSEVSIGRAVITY 3-20µm, 4 beams OCA/GEMINI Nice µm, 4-6 beams LAOG Grenoble…. 2.2µm, 4x2 beams MPE….

A European effort MPE, GarchingUSM, MunichETH, Zurich ATC, EdinburghMPIA, HeidelbergU of Durham U of OxfordLAOG, GrenobleLAM LESIAEPF, Lausanne ONERA Obs de GeneveLUANPadova Obs. U of AmsterdamRAL, DidcotObs. Leiden IMT, NeuchatelASTRONObs. Heidelberg

More second generation.. ESO funding for further second-generation instruments from 2010 ESO funding for further second-generation instruments from 2010 currently discussing the process ( call for proposals etc.) currently discussing the process ( call for proposals etc.)