E-ELT INSTRUMENTATION
The E-ELT Instrumentation Project Office has been established to work
on the instrument studies and the telescope interface. A plan for
instrument and post-focal adaptive optics studies, to be carried out
in collaboration with institutes in the ESO community, was presented
to the ESO Council in June 2007. The plan identified six instrument
concepts, two post-focal AO modules (MCAO and LTAO) of high priority
and two other instruments to be chosen after an open call to the
community for additional concepts. By September 2008, all ten
instrument consortia have been formed and the studies are under way
(see table below). In two cases the consortia are led by ESO, two have
been set up with a direct negotiation with external institutes and all
the others have been selected after an open call for proposals.
Two to three instruments are expected to be ready for first light. A full suite of instruments covering a wide parameter space will be built up over the first decade of E-ELT operations, in a similar way to the VLT.
E-ELT Phase A Instrumentation Studies
| Name | Instrument Type | Principal Investigator Institutes | Wavelength Range Spectral Resolution Field-Of-View |
More Information |
| CODEX | High Resolution, High Stability Visual Spectrograph | Luca Pasquini, ESO Instituto Nazionale di Astrofisica (INAF), Osservatori Trieste and Brera; Instituto de Astrofisica de Canarias (IAC); Institute of Astronomy, University of Cambridge; Observatoire Astronomique de l'Universite de Geneve; |
0.37-0.72μm R = 115300 0.82'' |
|
| EAGLE | Wide Field, Multi IFU NIR Spectrograph with MOAO | Jean-Gabriel Cuby, Laboratoire d'Astrophysique de Marseille (LAM) Observatoire Paris-Meudon (OPM), Laboratoire d'Etudes des Galaxies, Etoiles, Physique et Instrumentation (GEPI) and Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA); Ofice National d'Etudes et Recherches Aérospatiale (ONERA); United Kingdom Astronomy Technology Centre (UK ATC); Durham University, Centre for Advanced Instrumentation |
0.8-2.45μm R = 4000 (HighR ~ 10 000) 1.65'' (Patrol FoV 7.3' ) |
|
| EPICS | Planet Imager and Spectrograph with Extreme Adaptive Optics | Markus Kasper, ESO Laboratoire d'Astrophysique de l'Observatoire de Grenoble (LAOG); LESIA; Universite de Nice; LAM; ONERA; University of Oxford; INAF, Osservatorio Padova; ETH Zurich; NOVA, Universities of Amsterdam and Utrecht |
0.6-1.8μm R = 125, 1500 and 21000 imager: 3'' |
|
| HARMONI | Single Field, Wide Band Spectrograph | Niranjan Thatte, University of Oxford Centre de Recherche Astrophysique, Lyon; Departamento de Astrofisica Molecular e Infraroja, Consejo Superior de Investigaciones Cientificas, Madrid; IAC; UK ATC |
0.8-2.4μm R = 4000, 10 000 and 20 000 0.51'' x 1.02'' |
|
| METIS | Mid-infrared Imager and Spectrograph with AO | Bernhard Brandl, NOVA, University of Leiden MPIA; Commissariat a l'Energie Atomique (CEA) Saclay, Direction des Sciences de la Matiere (DSM)/Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU)/Service d'Astro- physique (SAp); Katholieke Universiteit Leuven; UK ATC |
2.9-13.8μm R = 10 - 100000 imager: 18'' |
|
| MICADO | Diffraction-limited NIR Camera | Reinhard Genzel, Max-Planck Institute for Extraterrestrial Physics (MPE) Max-Planck Institute for Astronomy (MPIA); Universitaets-Sternwarte Munich (USM); INAF, Osservatorio Padova; Nederlandse Onderzoekschool Voor Astronomie (NOVA), Universities of Leiden and Groningen |
0.8-2.4μm R = 3000 and 5000 up to 53'' |
|
| OPTIMOS | Wide Field Visual MOS | tbd Negotiations under way with a Consortium of Science and Technology Facilities Council, Rutherford Appleton Laboratory; University of Oxford; LAM; INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Milan; GEPI; NOVA, University of Amsterdam; INAF, Osservatori Trieste and Brera; Niels Bohr Institute, University of Copenhagen |
0.37-1.7μm MOS: 5000 (for > 300 objects), 20000 (for > 80 objects), 40000 (for 25 objects) MOS: 7' |
|
| SIMPLE | High Spectral Resolution NIR Spectrograph | Livia Origlia, INAF, Osservatorio Bologna INAF, Osservatorio Arcetri; INAF, Osservatorio Roma; Uppsala Astronomical Observatory; Thuringer Landessternwarte; Pontificia Universidad Catolica de Chile |
0.8-2.5μm R = 100000 - 150000 slit lengths 0.45'', 4'' |
Characteristics of the Instruments
Click on the images to display larger versions.
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Width of the field of view vs. wavelength coverage for the eight E-ELT proposed instruments currently under study. When the expected field of view is not squared, the average value of both dimensions or the diameter is shown. In the case of OPTIMOS and EAGLE (up) the shown value refers to the patrol field. For SIMPLE, the plot shows the slit length in single-object and long-slit modes. |
Pixel/spaxel size vs. wavelength coverage for the eight E-ELT proposed instruments currently under study. The diagonal black line shows the diffraction limit of the telescope as a function of wavelength. The values shown here refer to the sampling size of the instruments in their different observing modes. In the case of OPTIMOS-EVE(MOS), the quoted value corresponds to the fibre aperture. CODEX is only included for illustrative purposes as this instrument will not record any spatial information. |
Spectral resolution vs. wavelength coverage for the eight E-ELT proposed instruments currently under study. High, medium and low resolution channels are included when available. The arrow in SIMPLE indicates the potential upper limit to be reached depending on specific construction details. In the case of OPTIMOS-EVE(MOS) the arrow represents the range of resolution expected to be available. |
Post-focal AO Modules
| Name | Instrument Type | Principal Investigator Institutes | Wavelength Range Field-Of-View |
More Information |
| ATLAS | Laser Tomography AO Module | Thierry Fusco, ONERA GEPI and LESIA |
0.6-13.5μm 60'' |
|
| MAORY | Multi Conjugate AO Module | Emiliano Diolaiti, INAF, Osservatorio Bologna INAF, Osservatorio Arcetri; INAF, Osservatorio Padua; University of Bologna; ONERA |
0.8-2.4μm 2' |
Links
- ESO makes available all contributions of ESO authors that were presented at the SPIE conference in Marseille, June 2008 link. Many of the papers located therein describe the E-ELT and its instrumentation.
- presentation by S. D'Odorico (Science Working Group meeting in October 2008)
- presentation by M. Casali (JENAM 2008)