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The E-ELT

The E-ELT. J.-G. Cuby , LAM. ESO, December 2011 Proposal for a 39-m diameter telescope Cost to completion : 1180 M€ Including 100 M€ for (4) instruments 100 M€ contingency Start of operations Q4 2022

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The E-ELT

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  1. The E-ELT J.-G. Cuby, LAM

  2. ESO, December 2011 • Proposal for a 39-m diameter telescope • Cost to completion : 1180 M€ • Including 100 M€ for (4) instruments • 100 M€ contingency • Start of operations Q4 2022 • Approval: possibly in 2012, contingent on Brazil joining ESO and member states approving their extra contribution to finance the E-ELT • France has ! LIA-Origins Workshop 2012

  3. The European Extremely Large Telescope ESO (14 European member states + Brazil) 5-mirror design, 10 arcmin field of view Adaptive Optics Telescope Deformable mirror Laser Guide Stars (6-8) 39-m segmented M1 (1100 m2), 798 / 931 segments, 1.45 m M2: 4.1-m M3: 3.7-m M4: 2.4-m (adaptive) M5: 2.6-m LIA-Origins Workshop 2012

  4. LIA-Origins Workshop 2012

  5. The Adaptive Optics Zoo Extreme Adaptive Optics SCAO, MCAO, LTAO, GLAO, MOAO, XAO • 2 Families: • High correction over ~1-2' arcmin fov (MCAO), or locally over 5-10' fov (MOAO)‏ • MCAO / MOAO • IQ From 5-10 mas to 100 mas • Low correction over a 5-10' fov • noAO / GLAO • IQ ~ 300-600 mas LIA-Origins Workshop 2012

  6. E-ELT Instrument Suite • Phase A conceptual studies: eight instruments + 2 Adaptive Optics modules • Two first light instruments selected: • Micado. Diff. limited near-IR imager, 1 arcminfov. • Harmoni, multi-mode IFU, 5” x 10” • (this represents ~ 50% of the TMT first light instrument capabilities) • Then (#3) a mid-IR instrument (ELT-MIR) • Then ELT-MOS and ELT-HIRES (#4 and #5, order TBD) • ELT-6 TBD • ELT-PCS (XAO high contrast imager for exoplanets) as technological maturity allows LIA-Origins Workshop 2012

  7. E-ELT MOS • 3 concepts have been studied as part of the ELT instrument phase A studies • EAGLE (IFUs) • OPTIMOS-DIORAMAS (slits) • OPTIMOS-EVE (fibres) LIA-Origins Workshop 2012

  8. E-ELT HIRES • 2 instrument have been studied as part of the ELT instrument phase A studies, one in the optical (with extreme stability – laser comb) and one in the near IR (CODEX and SIMPLE) • E-ELT HIRES will rely on one of these two concepts, or a combination of both LIA-Origins Workshop 2012

  9. Science cases • Similar to all ELT projects • Strong synergies with ALMA, JWST, etc. • Headings of the TMT science cases • The first luminous objects • High-redshiftUniverse • Dissecting galaxies • The physics of galaxy formation and evolution • Stellar Populations in the Local Universe • Black holes and active galactic nuclei • Physics of Star and Planet Formation • Characterizing exoplanets • Spectroscopy of exoplanetatmospheres • Doppler detection of terrestrial planets • Atmospheres of terrestrial planets • Solar system studies • Some projects somewhat specific to the E-ELT: acceleration of the Universe, Galactic Center, etc. LIA-Origins Workshop 2012

  10. ELT parameter space • 10 to 20 arcminfov (max). In practice, 5 to 10 arcmin • Spatial resolution (from a few milli-arcsec to 500 mas) • Mostly Red / Near IR / mid IR • Same paradigm as with HST and current generation of 8-10 m telescopes: Imaging in space (JWST), Spectroscopy from the ground (ELT) LIA-Origins Workshop 2012

  11. Exoplanets • Radial velocity down to 1 cm.s-1 • High contrast imaging (XAO + coronagraph • Near IR high-Res spectroscopy of transiting planets Earth-like planets from RV Simulation of the direct imaging of exoplanets with the E-ELT. Near-infrared spectrum of an Earth-like atmosphere (transit spectroscopy) LIA-Origins Workshop 2012

  12. Stellar-Archaelogy ACS: F814W [~3x3 arcmin] Anonymous galaxy, 2 Mpc ACS image

  13. Stellar-Archaelogy 9 arcsec ACS image ACS image

  14. Stellar-Archaelogy 9 arcsec ACS image Simulated E-ELT 3D-cube plane DRSP: 1000 stars in ~ 25 hrs ACS image

  15. The physics of highredshift galaxies The physics of galaxies at z = 3-6 On-going and future studies with VLT (SINFONI, KMOS,…) • E-ELT Instruments: • Harmoni • EAGLE • Optimos-EVE • Optimos-Dioramas Programme of 100 galaxies at the VLT (SINFONI). z = 1-2 LIA-Origins Workshop 2012

  16. The most distant galaxies The physics of the ‘first light’ galaxies (z > 7). UV continuum spectroscopy. Doing at z ~ 8 what Keck has done at z =3 (LBGs) z = 7-8 galaxies in the HUDF (HST/WFC3) • E-ELT Instruments: • Harmoni • EAGLE • OPTIMOS-Dioramas Shapley et al., 2003 Bouwens et al., 2011, ApJ737

  17. The redshift drift • The estimated amplitude of this redshift drift over a decade is only about 6 cms-1. • Effect detectable with a ultra-high stability and precision spectrograph (a few cm/s) over 10 – 20 yrs: 4000 hours over 20 years willunequivocallyprove the existence of darkenergywithoutassumingflatness, usinganyothercosmologicalconstraints or makinganyotherastrophysicalassumption • Providesindependent confirmation of SNIaresults, using a different method and a complementaryredshiftrange LIA-Origins Workshop 2012

  18. Conclusions • Stay tuned, funding decision hopefully in 2012 • Start of operations 2022 • With two or three instruments • More instruments developed one every ~ 2 yrs LIA-Origins Workshop 2012

  19. ELT projects • TMT • 30m • 20’ fov • First light ~ 2022 • GMT • 21m • 20’ fov • E-ELT • 39m • 10’ fov

  20. Instrumentation 38 Institutes in 10 ESO countries +1 in Chile, >100FTEs ~ 2 M€ (out of 2.8 in Phase B) to external institutes for the studies + 25 ESO FTEs • First two instruments are being chosen to be included in proposal for construction • Pool of 4-5 instruments to be progressively deployed at the telescope • Schedule and process unclear at this point LIA-Origins Workshop 2012

  21. Context • Wide field surveys on 4-m and 8-m telescopes from ground (VLT, VISTA, Big-Boss, PFS, etc.) and from space (Euclid) • Narrow field facilities for deep surveys (VLT, ALMA, JWST, etc.).

  22. SF2A, Marseille 17 May 2012 LIA-Origins Workshop 2012

  23. A dynamical measurement ofthe expansion history of the Universe • 4000 hours over 20 years willunequivocallyprove the existence of darkenergywithoutassumingflatness, usinganyothercosmologicalconstraints or makinganyotherastrophysicalassumptionwhatsoever. • Providesindependent confirmation of SNIaresults, using a different method and a complementaryredshift range. 27 LIA-Origins Workshop 2012

  24. Some numbers • 984 /1148 segments • Industrial challenge for manufacturing • ~ 2 segments to coat per day • 6-m active M2 • 2.5-m Adaptive M4 and Tip-tilt M5 • 4500 tons SF2A, Marseille

  25. TMT

  26. 1.0 m/s HARPS Exoplanets Direct Detection High contrast imaging, extreme Adaptive Optics ESO Design Reference Mission Doppler detection down to ~ 1cm/s SF2A, Marseille

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