E-ELT Programme; ESO Instrumentation Project Office Ground-based Instrumentation for VLT, VLTI and E-ELT

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1 Ground-based Instrumentation for VLT, VLTI and E-ELT Raffaele Gratton (with strong help by Sandro D Odorico)

2 VLT 2 nd generation instruments Launched in 2001, completed 2012 HAWK-I (2007): wide field (7.5 arcmin square) NIR imager X-Shooter (2008): very wide band ( μm), high throughput single field spectrograph (R<10000) [154] KMOS (2010): multi-ifu s (24) cryogenic NIR spectrograph, R~3000 [250] SPHERE (2011): XAO-based planet finder [260] AOF+MUSE (2012): 1 arcmin 2 Vis IFS [225] Italian participation: ~30% of X-Shooter, ~15-20% SPHERE ~10% of external to ESO Total GTO nights: 889

3 VLTI 2 nd generation instruments Launched in 2005, completed 2012? Gravity: K-band 4-tel astrometry (2012?) Matisse: LMN band 4 tel (2012?) VSI: 4-6 tel. near IR imager/spectrograph (2012?) At present, two instruments (Gravity and Matisse) recommended for phase-b. VSI may proceed more slowly Italian participation: some part in VSI. Not quantified at present, but less than 10% of the total VLTI 2 nd gen instruments program

4 Retirements: FORS1 (2009; polarimetry and blue camera on FORS2) ISAAC (2010), AMBER,MIDI (2011?), NACO (2012) 2008: 2013: 2020: UT1: ISAAC CRIRES FORS1 UT2: UVES FLAMES X-SHOOTER UT3: visitor (MAD) VIMOS VISIR UT4: HAWK-I SINFONI FORS2 UT1: KMOS CRIRES FORS2 UT2: UVES FLAMES X-SHOOTER UT3: SPHERE VIMOS VISIR UT4: HAWK-I MUSE SINFONI? UT1: KMOS UT2: X-SHOOTER UT3: SPHERE UT4: HAWK-I MUSE

5 New plan for VLT instruments (2008?) Workshop "VLT in the ELT Era STC Recommendations (endorsed by Council): A very stable HR-spectrograph (Very high precision RV for search of rocky planets, variation of physical constants, analysis of chemical composition of stars in nearby galaxies) A wide field, very high multiplex spectroscopic facility Upgrades and/or replacements of VLT "work-horse" instruments: a multiplex NIR spectroscopic capability intermediate to high spectral resolution opt.-nir spectroscopy NIR diffraction limited imaging at least one open slot for new concepts The plan should follow procedures similar to those followed for second generation VLT instruments. Such a plan should be open and transparent for the community.

6 S. D Odorico Slide 1 The European ELT : Status Following one year of intensive studies, in December 2006 the ESO Council approved the proposal for a Phase B Study of a 5 mirror adaptive telescope with diameter ~40m. Present budget estimate for a 42m is 800 Ml + instruments. Start of operation 2017 The Study will extend 3 years with a budget of 57 Ml, mostly for industrial contracts. Project group at ESO of ~ 30 Proposal for construction in Spring 2010

7 E-ELT: 42m,5 mirror AO telescope 10 Nasmyth field with DL image quality, 9% vignetting λ(μm) Diffraction limit F/16 s. d odorico- I AU 250 TMT Design

8 Instrumentation Distribution at the Telescope MACAO MODULE COUDE LABS S. D Odorico Slide 8

9 S. D Odorico Slide 9 TELESCOPE- AO INSTRUMENT INTERFACES Multi-instrument virtual configuration at the Nasmyth focii Test Camera Laser Adaptor, Coude/MCAO feeding unit Adaptor-Rotator with laser WS, gravity invariantfeeding mirror XAO Instrument MCAO and GLAO instruments MCAO Instrument Instrument, M2 lifting platform

10 TELESCOPE - AO INSTRUMENT INTERFACES Nasmyth Focii, Gravity Invariant Focus, Coudè Focus Nasmyth A- F/15 Nasmyth B F/16 Coudè Focus environment provides stability to measure Rv to the accuracy needed for Earthlike planets and the expansion of Universe S. D Odorico Slide 10

11 STATUS OF the 8 E-ELT INSTRUMENTS +2 Post Focal AO MODULES STUDIES (1) Time frame: / Budget: 2.7 M +30 ESO FTEs INSTRUMENT STUDY EAGLE CODEX MAIN OBSERVING MODES WF, Multi IFU NIR Spectrograph. +AO High Resolution, High Stability Visual Spectrograph PROCUREMENT MODE, NATIONALITY OF INSTITUTES Contract to Institutes in France + & UK ESO coordination of Institutes from Italy, Spain, Switzerland and UK ESO coordination of Institutes from France, EPICS + AO Planet Imager and Spectrograph Italy, Switzerland, UK Every instrument study to detail the science case, finalize the instrument requirements and Negotiations develop under way an following instrument an Open Call HARC Camera sampling to the DF for fixed cost study (MICADO Consortium: concept including cost and construction Germany, Italy, The schedule Netherlands) SFWBS MACAO Module MIR Instrum. + AO IFU, Wide Spectral Band Spectrograph Provides DL images over a field up to 2 Mid IR camera /spectrograph Negotiations under way following an Open Call for fixed cost study (HARMONI Consortium): UK, France, Spain) Contract to MAORY Consortium ( Italy and France) Open Call for fixed cost study, deadline in March 08 S. D Odorico Slide 11

12 STATUS OF the 8 E-ELT INSTRUMENTS STUDIES STUDIES + 2 Post Focal AO MODULES (2) Yet to come INSTRUMENT STUDY 2 New Ins Concepts Laser Tomography AO Module MAIN OBSERVING MODES PROCUREMENT MODE, NATIONALITY OF INSTITUTES For Proposer to identify Open Call to be launched in Feb 08 with a deadline in May 08 Provides diffraction limit performances over a small field Open Call to be launched in Feb 08 with a deadline in April 08 S. D Odorico Slide 12

13 EPICS EPICS is an instrument project for the direct imaging and characterization of extra-solar planets with the European ELT The extreme Adaptive Optics (XAO) system The Diffraction Suppression System (or coronagraph) The Speckle Suppression System The Scientific Instrument(s) Integral Field Spectroscopy Differential Polarimetry A speckle coherence-based instrument Data processing strategy

14 EPICS Science Objectives Terrestrial Planets in HZ Some chance for the ~70 M dwarfs (-53<Dec<7) closer than 10pc (HZ at 10 pc is at 15mas, probably beyond inner working angle) However, tidal locking, atmosphere evaporation, likely thin (Lissauer) or no (Brain) atmosphere Some chance for rocky planets inwards of HZ (Venus) for the ~100 G, K and M stars within 10pc Improbable to detect even for the handful of closest K-and and G-stars Little hope for spectroscopy at R>20

15 EPICS Science Objectives Giant Planets, unique science Young self-luminous gaseous planets in star forming regions or young associations EPICS can achieve good resolution even for star forming regions at ~100pc, young planets at >3 AU can be detected, very important observation to understand planet formation Mature giant planets at orbital distances between ~5 and 15 AU in the solar neighbourhood ( 20 pc) Not an easy observation Determine frequency and mass distribution of giant planets Warm Jupiters that have been discovered by radial velocity searches Fairly easy, spectral characterization Understand giant planets atmosphere composition and structure

16 EPICS PHASE A Conceptual Design 24 months (Kick Off meeting Oct. 07) Consortium: ESO, LAOG, LESIA, LUAN, LAM, ONERA, Oxford, INAF-Padova, ETH, UvA, ASTRON, UU

17 EPICS PHASE A Work Breakdown Structure Italian involvement: FTE: 1.35 staff FTE project Money: 81 keuro (32 keuro ESO + 49 keuro FP7)