FUTURE DEVELOPMENTS IN IR INSTRUMENTATION AT ESO

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FUTURE DEVELOPMENTS IN IR INSTRUMENTATION AT ESO

• Mark Casali

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

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VISTA
UKATC/RAL

• 16 2kx2k VIRGO
• 0.34 pixels
• 1.70 diameter
• ZYJHKs nb
• 2007

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VISTA

• 16 2kx2k VIRGO
• 0.34 pixels
• 1.70 diameter
• ZYJHKs nb
• 2007

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VISTA

• 16 2kx2k VIRGO
• 0.34 pixels
• 1.70 diameter
• ZYJHKs nb
• 2007

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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

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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
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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
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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

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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
?
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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

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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

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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

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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

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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)

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CRIRES
R 100k Very stable 1-5 microns polarimetry Delive
ry in next few months
ESO IR department/Käufl
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CRIRES
4 hybridized Aladdin III Resolution100k AO front
end 5 m/s with gas cells
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Spectro-Polarimetric High-contrast Exoplanet
REsearch
LAOG/LAM/LESIA/ONERA/O.Geneve/MPIA/O.Padova/ETH/O.
Ams.. 2010
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VLTI - PRIMA - 2008

• ESO/IMT/O.Geneve/O.Leiden/MPIA/O.Heidelberg/EPF/MP
  E/ASTRON
• Dual-feed on 2 UTs/ATs
• gain of 5 to 6 magnitudes
• Phase-Referenced Imaging with AMBER or MIDI
• High accuracy differential astrometry

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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
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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
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More second generation..

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