the e-elt instrumentation roadmap - ipagipag.obs.ujf-grenoble.fr/~chauving/eelt_ins_roadmap.pdf ·...

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

E-ELT Instrumentation Roadmap | PST 11.07.2012

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

OVERVIEW OF THE E-ELT INSTRUMENT

STUDIES

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.

ESO/COU 1275, December 2009

Selection process:

criteria


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

Selection process:

scientific priority


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

Selection process:

the first light pair


MICADO: Diffraction-limited NIR Camera

Primary Imaging Field

53” across, 3mas pix

4x4 HAWAII 4RG det

~20 filter slots

High throughput

Auxiliary Arm

Imager: 1.5mas & 4mas pixels

Spectrograph: R=3000

1 HAWAII 4RG detector

AO System – MCAO/MAORY

PI: Reinhard Genzel (Ric Davies)

MPE, MPIA, USM, INAF-OAPD,

NOVA , LESIA


MAORY : Multi-conjugate adaptive optics relay

MICADO mounted under MAORY

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


HARMONI Single field, wide band IFU, NIR spectrometer

Wavelength range 0.47-2.45µm

Spectral resolving power R ≈ 4000, 10000, 20000

4 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


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



ELT-CAM: NIR diffraction-limited camera





A planetary camera/spectrograph with Extreme AO

(>90% Strehl) has high scientific priority and must

be built once the technology is developed

Selection process:

planetary camera/spectrograph


ELT-PCS/EPICS

exo-planet imaging camera spectrograph

Integral Field Spectrograph 0.95-1.65μm

FOV: 0.8'' x 0.8'„/2.33mas

0.8'' x 0.014'„ long slit

R = 125, 1400 and 20000

EPOL 0.6-0.9μm

Coronagraphic polarimeter

FOV: 2'' x 2'‘/1.5mas

Contrast ratios – 10-8 – 10-9

XAO – very high (90%) Strehl

12

PI: Markus Kasper, ESO

LAOG,LESIA, Uni. Nice,

LAM,ONERA, Uni.Oxford, INAF,

ETH Zurich, NOVA



ELT-CAM: NIR diffraction-limited camera





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

Selection process:

a pool of capabilities


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


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)


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


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


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


ELT-MIR/METIS: MIR ELT Imager and Spectrograph

Imager (LM and N-

band channels)

LM band IFU

spectrograph

AO module

cold

calibration unit

common

fore-optics 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 [

0.4˝ 1.5˝] spectrograph

o for L/M

o R ~ 100,000

PI: Bernhard Brandl,

Nova, MPIA, CEA Saclay, KU Leuven, UKATC


ELT-4 and 5

Selected to be a MOS instrument (ELT-MOS) and a high-

resolution spectrograph (ELT-HIRES)

Science requirements for MOS in 2013

Call for proposals


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


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.


ELT-MOS/EAGLE: a wide-field

multi-IFU AO assisted NIR spectrograph

o Near-infrared: 0.8-2.45 m

o Patrol field 38arcmin2

o 20-IFU fields

o 1.65”x1.65”

o R~4000,10000

o Multi-Object AO

o 6LGS, 6NGS

o >30%EE in 75mas pixels

PI: Jean-Gabriel Cuby, Simon Morris

LAM, Uni. Durham, UK ATC, GEPI,

ONERA, LESIA


Removal of the gravity invariant platform

Implications for the EAGLE instrument are being studied

by the team as “delta-Phase A” study

39-mTelescope-Instrument

Interface Change


ELT-4 and 5




Call for proposals

Science requirements for HIRES spec option in 2013

Call for proposals


ELT-HIRES/CODEX high stability, high resolution visible spectrograph

Wavelength range 0.37-0.71 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


ELT-HIRES/SIMPLE:

High resolution NIR spectrograph

Wavelength 0.84-2.5 m

Complete spectrum

R~130,000

Slit: 27x450mas

Adaptive optics

SCAO on-board

MCAO/MAORY

LTAO/ATLAS

PI: Livia Origlia

INAF,UAO, TLS, PUC


ELT-4 and 5




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


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


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 2022. Can start earlier if

required TRL has been reached.


Instrument Roadmap

E-ELT Instrumentation Roadmap | PST 11.07.2012 32

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