The E-ELT Instrumentation Roadmap Presentation to the Project Science Team

Transcription

1 The E-ELT Instrumentation Roadmap Presentation to the Project Science Team Suzanne Ramsay Mark Casali, Norbert Hubin, Hans Ulrich Käufl, Jean-Louis Lizon, Josef Strasser, Juan Carlos Gonzalez

2 The instrument studies The goal of the study programme was to carry-out a suitable number of instrument studies to work with the ESO community towards construction to verify that instruments can be built at an affordable cost and that they properly address the highest priority scientific goals, to work with telescope and operation groups to identify and define interfaces with the other subsystems and the observatory infrastructure. 9 instrument and 2 post-focal AO studies carried out by >300 scientists and engineers in 40 institutes throughout the ESO community

3 OVERVIEW OF THE E-ELT INSTRUMENT STUDIES

4 Selection process: criteria ESO/COU 1275, December 2009 Nr. Evaluation Criteria for E-ELT instrument selection 1 Scientific Merit : (a) the instrument addresses science goals identified as of highest priority for the E-ELT (b) the instrument can be conceived as an E-ELT workhorse to be used for a variety of programmes, leading to a broad spectrum of potential discoveries (c) the instrument will benefit and complement observations of other major facilities in astrophysics like ALMA and the JWST, which will be already in operation at the time of first light 2 Proven Technical Feasibility and Simulated Performance: the instrument feasibility and its expected performance have been properly demonstrated in the study 3 Affordability: (a) the instrument cost is well estimated and justified (b) the cost to ESO falls within or close to the preliminary budget envelope. 4 Timely Match to the telescope + PFAO performance: the instrument schedule of implementation is well matched to the path of the telescope +AO to full performance. The instrument includes the possibility to do prime science even during the time when the telescope cannot operate with AO.

5 Selection process: scientific priority Science based prioritisation All instruments candidates for selection at first light with the exception of the planet camera and spectrograph, EPICS (highest scientific priority but long technology development) Science Working Group Criteria for selection of first light instruments Scientific impact, including certainty of scientific return Complementarity with other facilities Scientific Flexibility Coverage of expected observing conditions

6 Selection process: the first light pair First light instruments ELT-CAM: NIR diffraction-limited camera with moderate field size ELT-IFU: NIR IFU spectrograph with optical-ir coverage and seeing limited to diffraction limited capabilities Adaptive optics systems as required to meet the science cases of each instrument

7 Primary Imaging Field 53 across, 3mas pix 4x4 HAWAII 4RG det ~20 filter slots High throughput Auxiliary Arm MICADO: Diffraction-limited NIR Camera Imager: 1.5mas & 4mas pixels Spectrograph: R= HAWAII 4RG detector AO System MCAO/MAORY PI: Reinhard Genzel (Ric Davies) MPE, MPIA, USM, INAF-OAPD, NOVA, LESIA

8 MAORY : Multi-conjugate adaptive optics relay Multi-conjugate AO 6 laser and 3 natural guide stars Deformable mirrors conjugated to atmospheric layers at 4km, 12.7km Very high quality images (S.R. >50% in K) over a wide field - 2, Central 1 clear Two output ports PI: Emiliano Diolaiti INAF (Bologna, Padova, Arcetri, IASF-Bologna), Univ.Bologna, ONERA MICADO mounted under MAOR

9 HARMONI Single field, wide band IFU, NIR spectrometer Wavelength range µm Spectral resolving power R 4000, 10000, spatial scales 4mas, 10mas, 20mas, 40mas 4 fields of view 0.5'' x 1.0'', 1.25'' x 2.5'' 2.5'' x 5', 5'' x 10' LTAO/ATLAS PI: Niranjan Thatte, Oxford, CRAL, CSIC, IAC,UK ATC, ONERA

10 ATLAS: Advanced Tomographic Laser AO Adaptive optics using laser guide stars Uses the telescope adaptive mirrors, simple design No additional mirrors in the instrument optical path Very high quality images (S.R. >50% in K) over ~30 field Fixed asterism of six laser guide stars, 2 NGS Excellent sky coverage PI: Thierry Fusco ONERA,GEPI, LESIA, UK ATC, LAM

11 Selection process: planetary camera/spectrograph First light instruments ELT-CAM: NIR diffraction-limited camera ELT-IFU: NIR IFU spectrograph with optical-ir coverage and seeing limited to diffraction limited capabilities Adaptive optics systems as required to meet the science cases of each instrument A planetary camera/spectrograph with Extreme AO (>90% Strehl) has high scientific priority and must be built once the technology is developed

12 ELT-PCS/EPICS exo-planet imaging camera spectrograph Integral Field Spectrograph μm FOV: 0.8'' x 0.8' /2.33mas 0.8'' x 0.014' long slit R = 125, 1400 and EPOL μm Coronagraphic polarimeter FOV: 2'' x 2' /1.5mas Contrast ratios XAO very high (90%) Strehl PI: Markus Kasper, ESO LAOG,LESIA, Uni. Nice, LAM,ONERA, Uni.Oxford, INAF, ETH Zurich, NOVA 12

13 Selection process: a pool of capabilities First light instruments ELT-CAM: NIR diffraction-limited camera ELT-IFU: NIR IFU spectrograph with optical-ir coverage and seeing limited to diffraction limited capabilities Adaptive optics systems as required to meet the science cases of each instrument A planetary camera/spectrograph with Extreme AO has high scientific priority Instruments thereafter of equal scientific priority A pool of scientific capabilities : MIR imaging and spectroscopy, VIS-NIR multi-object spectroscopy, VIS- NIR high resolving power spectroscopy

14 E-ELT Instrumentation Roadmap ELT-IFU and ELT-CAM for first light (SWG/STC/ESO) ELT-MIR, MOS, HIRES scientifically equivalent priorities (SWG/STC/ESO) Selection by other considerations (project readiness) Practical requirements Staggered project schedule for funding profile Staggered commissioning schedule Start enabling technology development, especially for high-priority instruments e.g. ELT-PCS Begin project when feasibility (TRL) is demonstrated

15 Roadmap Considerations ELT-3 to help cover poor IQ conditions (SWG/STC) MOS/HIRES scientific requirements to be developed to allow selection between options (SWG) Keep flexibility (SWG/STC/ESO) Changing science, new member states, precursor instruments Possibility for submission of new/revised ideas (ESO) Competitive calls for proposals where sensible (STC)

16 Instrument Roadmap 7 instruments currently identified for construction 100M Euros in construction budget Construction proposal covers first four instruments Project Science Team involvement in science requirements definition This plan will evolve! Requirement to maintain an Instrument Plan into the operations phase

17 ELT-1 and ELT-2 First light instruments selected as ELT-CAM and ELT-IFU Unchanged from version 1 of Instrumentation Plan. These instrument projects include AO capabilities Require 1-2 years to define Telescope interfaces, Specifications, Integration of AO Contract details Science requirements to be discussed here Negotiation underway with the Phase A consortia

18 ELT-3 ELT-MIR selected as instrument 3 based on readiness and will be based on the METIS study Specifications are well defined Less dependent on best image quality Technically well developed proposal Minimal technology development Aquarius detector on-sky tests with VISIR Successful outcome required before starting ELT-MIR TRL review 2013

19 ELT-MIR/METIS: MIR ELT Imager and Spectrograph o Diffraction limited imager [18 18 ] o L/M band and N band o Includes coronography o R 5000 long-slit spectrometer o includes polarimetry o High resolution IFU [ ] spectrograph o for L/M o R ~ 100,000 PI: Bernhard Brandl, common fore-optics cold calibration unit LM band IFU spectrograph Nova, MPIA, CEA Saclay, KU Leuven, UKATC AO module Imager (LM and N- band channels)

20 ELT-4 and 5 Selected to be a MOS instrument (ELT-MOS) and a highresolution spectrograph (ELT-HIRES) Science requirements for MOS in 2013 Call for proposals

21 ELT-MOS/OPTIMOS-DIORAMAS a wide field imaging MOS o Wavelength range 0.37 m-1.4(1.6) m o MOS and Imager o 6.8 x6.8 FOV o Standard visible and NIR filters o Multiplex: o 480 slits in the visible; 120 for NIR o Spectral resolution o R~300, 1000, 2500 visible o R~400,800,3000 for NIR PI: Olivier Le Fèvre LAM, IASF-Milano, Obs. Haute Provence, Obs. Genève, IAC

22 ELT-MOS/OPTIMOS-EVE: optical-hband fibre MOS o Wavelength range 0.37 m-1.7 m o Patrol field - ~7 o Multiplex options o 240 fibres /R~5000 o 70 fibres / R~15000 o 40 fibres / R~30000 o 30 IFUs 1.8 x 3 o 1 IFU 7.8 x13.5 o Both IFUs / R~5000 PI: Francois Hammer GEPI,NOVA, INAF, RAL, Nils Bohr I.

23 o Near-infrared: m o Patrol field 38arcmin 2 o 20-IFU fields o 1.65 x1.65 o R~4000,10000 o Multi-Object AO o 6LGS, 6NGS ELT-MOS/EAGLE: a wide-field multi-ifu AO assisted NIR spectrograph o >30%EE in 75mas pixels PI: Jean-Gabriel Cuby, Simon Morris LAM, Uni. Durham, UK ATC, GEPI, ONERA, LESIA

24 39-mTelescope-Instrument Interface Change Removal of the gravity invariant platform Implications for the EAGLE instrument are being studied by the team as delta-phase A study

25 ELT-4 and 5 Selected to be a MOS instrument (ELT-MOS) and a highresolution spectrograph (ELT-HIRES) Science requirements for MOS in 2013 Call for proposals Science requirements for HIRES spec option in 2013 Call for proposals

26 ELT-HIRES/CODEX high stability, high resolution visible spectrograph Wavelength range m R~130,000 Field of view (0.82 ) ~2cms -1 Doppler precision over 30yrs no adaptive optics located in the coudé room PI: Luca Pasquini, ESO Geneve Observatory, IAC, INAF-Trieste and Brera, IoA

27 ELT-HIRES/SIMPLE: High resolution NIR spectrograph Wavelength m Complete spectrum R~130,000 Slit: 27x450mas Adaptive optics SCAO on-board MCAO/MAORY LTAO/ATLAS PI: Livia Origlia INAF,UAO, TLS, PUC

28 ELT-4 and 5 Selected to be a MOS instrument (ELT-MOS) and a highresolution spectrograph (ELT-HIRES) Science requirements for MOS in 2013 Call for proposals Science requirements for HIRES spec option in 2013 Call for proposals Followed by 1-2 years of further Phase-A design/technology development Select in 2015 whether MOS or HIRES to become ELT- 4/5 ELT-4 starts in 2016 ELT-5 starts in 2018

29 ELT-6 Unspecified instrument A new call for Phase A studies will be issued in 2015 For rework of existing unselected Phase A studies For new ideas Successful proposals will be funded for Phase A or - Phase A studies (2 years) Competitive Phase A studies Technical and scientific reviews of Phase A results Proposal to STC/Council 2019 selection/2020 start

30 ELT-PCS Instrument selected for construction High priority key instrument High technical risk Enabling technology required Strongly affected by ultimate performance of telescope Baseline start as late as Can start earlier if required TRL has been reached.

31 Instrument Roadmap

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