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E-ELT INSTRUMENTATION. Outline of the talk (adapted from Sandro d’Odorico’presentation) Instruments- 42m Adaptive Optics Telescope Interfaces based on work by F.Zerbi, J.Pirard, B. Delabre, E.Brunetto + many others in INS and TEL Project Offices

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E elt instrumentation
E-ELT INSTRUMENTATION

Outline of the talk

(adapted from Sandro d’Odorico’presentation)

  • Instruments- 42m Adaptive Optics Telescope Interfaces based on work by F.Zerbi, J.Pirard, B. Delabre, E.Brunetto + many others in INS and TEL Project Offices

  • Roadmap to the E-ELT Instrumentation Plan


E-ELT WG

Reports 2006

“Prominent Science Cases” from the ELT Science WG Report (4.2006) drive requirements for telescope and instrumentation

(Including Galactic Centre science)

(To the distance of Virgo and beyond)


E-ELT Top Level Requirements from ESE

  • E-ELT should be a general-use, multi-purpose facility. Instrument friendly

    • multiple foci incl. gravity invariant & coudé-like

    • fast instrument switching & easy maintenance

    • with large back focal distance, weight & volume

    • ADC & pupil position/field curvature “kindness

    • Synergy with ALMA/VLT/JMST strong drivers

    • Located at an optimal site (global science output versus cost)

  • Aiming at improved seeing  DL Image Quality

    • Image Quality within 0.1 “ over most of a 10’ field, DL in ~1’ field

    • GLAO, MCAO, MOAO, LTAO or XAO required for most science cases (LGS & NGS friendly design)

    • Prime wavelength domain 0.45(0.4) μm to 20 μm (max. efficiency incl. reasonably low emissivity)

    • Sub-mm imaging highly valuable but not a driver


OBSERVATORY – INSTRUMENT INTERFACES (6)

Nasmyth Focii, Gravity Invariant Focus, Coudè Focus

Nasmyth B – F/16

Nasmyth A- F/15

Coudè Focus


OBSERVATORY – INSTRUMENT INTERFACES (1)

Multi-instrument test configuration at the Nasmyth focii

Test Camera

Adaptor-Rotator with laser WS, gravity invariant-feeding mirror

Laser Adaptor, Coude/MCAO feeding unit

XAO Instrument

MCAO/MOAO and GLAO instruments

MCAO Instrument

Instrument, M2 lifting platform


EAGLE

OWL Instrument Studies 2004-5

B-Vis

NIR

MIR

Submm


Nir imagery with mcao from m casali
NIR Imagery with MCAO(from M. Casali)


14:17:29

Dichroic

M7 adaptive

conjugated

at 12 km

M10 adaptive

conjugated

at 5 km

M8

M9

window

Folding mirror

M6

F/15 MCAO

focus

125.00 CM

MULTI CONJUGATES

ADAPTIVE OPTICS

Wavefront sensors


1st results from mad at vlt march 07 marchetti hubin
1st results from MAD at VLT (March 07)(Marchetti, Hubin)

Sub-field: 14 x14 arcsec2 of a 1.5 armin fov2, NIR

No correction Single star AO MCAO

FWHM: 0.6 arcsec 0.1 arcsec

=> ELT could be competitive with JWST…


Elt europe instrumentation

EAGLE

ELT - Europe : Instrumentation


Elt eagle science

M32

OA 8m JWST OA 30m

ELT – EAGLE: Science

  • First objects: << 1 Gyr du BB

    ==> re-ionisation epoch (z=7-12)

  • Galaxy assembling (z=1-7)

    … to the Hubble sequence, today


Eagle science from matt lehnert project scientist
EAGLE Science (from Matt Lehnert, Project Scientist)

  • S5: Young star clusters

  • S7: The origin of massive stars

  • G4: Spectroscopy of resolved stellar populations in galaxies

  • G6: Young massive star clusters

  • G9: AGN demographics

  • C4: First light – The Highest Redshift Galaxies (z>10)

  • C5: Galaxies and AGN at the end of reionization

  • C8: Topology of the IGM as a function of redshift

  • C9: Galaxy formation and evolution

  • C10: The physics of high redshift galaxies

  • Could address half of the prominent Science Cases defined by the ELT Science Working Group


  • Why 3d spectroscopy

    Why 3D spectroscopy ?

    • GOAL: mapping physics V, sigma, extinction, O/H, ne

    • ==> at very high z

    GIRAFFE data on z=0.6 galaxies

    Puech et al 2006

    HST velocity field sigma map electronic density


    Spatial resolution

    ESO contract: fwhm= 0.1-0.15 arcsec; best effort 0.05 arcsec

    Spatial resolution

    More constraints at highest redshift

    rhalf at z=7: < 1 kpc or 0.1 arcsec

    0.1 arcsec for targets over a large FoV (> 5x5 arcmin2)

    GLAO not competitive (cf Neichel & Fusco simulations)

    MCAO: too small FoV

    ==> Multiple Object AO (e.g. Falcon)


    Elt eagle concept
    ELT – EAGLE: concept

    • Contrat ESO, Phase A:

    • 20 IFUs (spectro)

    • Fwhm=0.1 arcsec (MOAO)

    • FoV 5’x5’ goal 10’x10’

    • R>5000

    • 1 à 2.2m (spectro refroidi)

    Concept simplifié (sans AO) pour un instrument sur le ciel en 1ère lumière, avec MOAO < 2ans après


    OBSERVATORY – INSTRUMENT INTERFACES (4)

    GRAVITY INVARIANT FOCUS

    Scale at Nasmyth 1”=3.25mm

    45 o Mirror covers the 10’ field

    Dedicated adaptor

    Instrument room


    Elt eagle planning

    • Contrat ESO: 24 mois

    • Juillet 07 - Janvier 08: concept trade-off (spectro, IFU, TAS)

    • Janvier 08 - Juillet 09: design

    • + mise en place d’un démonstrateur de la MOAO sur le WHT (PDR 2009)

    ELT – EAGLE: planning

    F. Hammer ELTs - Conseil Scientifique - Observatoire de Paris 10-05-2007


    Elt eagle consortium
    ELT – EAGLE: consortium

    (PI: J.G. Cuby)

    50-50 FR-UK



    OBSERVATORY – INSTRUMENT INTERFACES (7)

    COUDE LABORATORIES

    For high resolution spectrographs requiring large volume and uniquely high stability (planet searches, QSO absorption lines).


    Codex
    Codex

    • Proposal distributed to community in 1989

    • 1st instrument operating in 1998

    • 10 instruments in operation in 2006 , over 50% in service mode, with very low downtime.


    Conclusion
    Conclusion

    • ELT : high priority in Europe & US (schedule ?), as was the VLT in the end of 80s

    • Most of the present french involvement is in EAGLE

    • Need for a large scientific involvement, including to define other possible scientific objectives


    DRAFT

    Fishing Pond :instruments concepts still to be investigated for the 42m, or not yet firmly associated to prominent science cases

    * : Polarimetry can be included as an observing mode in other instruments, if required by their respective science cases


    The vlt experience 2
    The VLT Experience (2)

    • An Instrumentation Plan defined with the community at the early stage of the program; adjusted on the way taking into account scientific and technical evolution

    • 3 built by ESO, 7 larger fraction by external consortia ( FTEGTO paradigm), with significant ESO project support and control. World-wide competitive , with many excellence peaks. 

      HAWK-I (ESO, 1.5 Gen) to be installed in 2007. Four 2nd Generation Instruments under way (2008-2012). Most work by external consortia with significant ESO contributions ( detectors systems in X-shooter,K-MOS , Sphere & MUSE, system engineering in X-shooter, AO in MUSE)

    • Very few casualties on the way: one instrument contract substantially modified, one instrument requiring substantial refurbishment and one cancelled 


    Roadmap to the e elt instrumentation plan
    ROADMAP TO THE E-ELT INSTRUMENTATION PLAN

    The Instrumentation Plan will include :

    • Policy of ELT instrument procurement

      • Largely following the VLT instrumentation model, ESO contributing to most of the hardware costs, FTEs in external institutes for GTO

      • Most of the instruments built by the community, with ESO contributing on critical subsystems as detectors, common software

      • ESO coordinating the overall effort and controlling advancement of projects according to TS and SoW

    • Selection Procedure for the Study Phase and the Project Contracts

      • No commitment to a single procurement scheme

      • Competing proposals and parallel feasibility studies for a specific instrument possible

      • For complex instruments, ESO in consultation with STC might coordinate the formation of a Consortium to avoid putting unacceptable strain on the community resources.

        ROADMAP TO THE E-ELT INSTRUMENTATION PLAN (11.2006-5.2007)ROADMAP TO THE E-ELT INSTRUMENTATION PLAN (5.200712.2009)


    DRAFT

    High Priority Instrument Batch : candidates for 1st generation

    * Minimum Strehl or EE to be specified ; +: from Science WG Report http://www.eso.org/projects/e-elt/publications.html


    10.87 CM

    NEAR INFRARED IMAGER (1.0-2.5μm)

    1.7 x 1.7 arc min field of view - F/ 0.83

    1024 x1024 detector (18μm)

    Dichroic

    16 cm

    Laser focus

    at 90 km

    Telescope

    Focal plane

    Laser focus

    at 160 km

    Cold stop


    300 mm

    Concept of MCAO IR camera design

    (see talk by M. Casali on Friday)

    Field Stop (1.4 arcmin square)

    M1

    M2

    Pupil Stop

    Entrance

    Window

    M4

    Folding

    Mirror

    M3

    M1 spherical concave R=3050 mm

    M2 spherical convex R=-1590 mm

    M3 spherical concave R=3290 mm

    M4 flat

    Filters

    NIR detector


    Tmt instrument studies
    TMT INSTRUMENT STUDIES

    STATUS: Feasibility Studies (in some cases quite comprehensive) completed and reviewed in 1Q 2006. Currently the all project is being “rebaselined”. Likely 1st generation are underlined in the table.

    For the GMT, very thin instrument concepts with the telescope proposal presented in Feb.2006. Feasibility studies now under way.


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