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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
slide2
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)

slide3
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
slide4
OBSERVATORY – INSTRUMENT INTERFACES (6)

Nasmyth Focii, Gravity Invariant Focus, Coudè Focus

Nasmyth B – F/16

Nasmyth A- F/15

Coudè Focus

slide5
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

slide6
EAGLE

OWL Instrument Studies 2004-5

B-Vis

NIR

MIR

Submm

slide8
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 eagle science
Stellar populations in nearby galaxies

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

slide17
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

slide22
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
slide25
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)

slide28
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

slide29
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

slide30
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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