PatMaj

1st light dates between ( )

AO-based instruments in red

15 May ‘02

DevelopmentDevelopment

ConceptConceptSTC

VLT Instruments Status

StudyStudyPlan

OperationOperation

FORS1 (3Q ’98)ISAAC (4Q ’98)UVES (3Q ’99)FORS2-R (4Q ’99)

PAE

CommissioningCommissioning

PAC

NAOS-CONICA

VIMOSOz-Poz/UVESOz-Poz/Giraffe

AIT

VISIR (4Q ’02)

MACAO (4Q ’02)

Fabrication

SINFONI (1Q ’04)CRIRES (3Q ’04) MAD (3Q ‘03)

FDR

DesignDesign

Final Design

NIRMOS (?)

Prelim. Design

1st Generation Upgrades2nd Generation Projects

2nd Generation Instruments

Paranal Observatory

VLT(I) Instrumentation

An extensive An extensive - - Coverage Coverage

1 10 (µm)

VLTI

VLT Instrumentation

An extensive An extensive - - / / Coverage Coverage

VLT Instrumentation

An extensive set of modesAn extensive set of modesVLT MULTI-OBJECT SPECTROGRAPHY

Operational Status

All four telescopes simultaneously executing scientific programs since 12 August ‘01

Low technical downtime (<2hr/week)P67: 2.5% (UT1) 2.1% (UT2) 0.8% (UT3) 2.1% (UT4)

High shutter open efficiency

P67: 73% (FORS1) 67% (ISAAC) 74% (FORS2) 85% (UVES)

UT1 - ISAAC UT2 - UVES UT3 - FORS1 UT4 - FORS2

FORS-1 & FORS-2FORS-1 & FORS-2

FORS Image Quality & Stability

Image Quality Telescope drivenBest image obtained (HR mode)

• 0.18” (integration time: a few seconds)

• 0.25” (integration time: several minutes)

VLT + FORS-1VLT + FORS-1Seeing ~ 0.6”

Keck + LRISKeck + LRISSeeing ~ 0.55”

Image Stability exceptional

Ellipticity distributionEllipticity distribution

Red: uncorrectedBlue: corrected

young brown dwarfI band - TW5 system

FORS2-R Upgrade

Better sensitivity

Very little fringing

Good astrometry

ISAACISAAC

ISAAC Image Quality

Jupiter AuroraeJupiter Aurorae

Io, deconvolved 0.4” imageIo, deconvolved 0.4” image

NB 4.07 µm

ISAAC Spectroscopic Sensitivity

z =3.2 galaxy “rotation” (V ~ 700 km/s)

OIII lines; 6 hr exposure; 0”.4 seeing

UVES @ UT2 Nasmyth

X-dispersed echelle spectrum

UVES: highly sensitive R~105 Spectrometer

Towards Beryllium primordial abundance

1st optical detection of a stellar coronal line1st Uranium detection outside Solar System

Two optimized channels high efficiency from 0.30 to 0.98 µm

UVES: high precision radial velocities

UVES + iodine cellUVES + iodine cellCommissioning dataDec 1999-Jan 2000(Martin Kürster)

Preliminary conclusion: long-term achievable precision better than 2 m/s

Known to be constant at 4 m/s level

Moderately active star (higher RV scatter)

NAOS-CONICA at Nasmyth UT4

VLT AdapterNAOS

CONICA

Cable Twist

Built by ONERA,, OP & LAOG (F), MPIA & MPE (D) and ESO

NAOS-CONICA Nov. ‘01

ISAAC

• Ks Image; t = 2400 s.

•350 mas fwhm

HST/WFPC2

• 814 nm Image; t = 400 s

• 85 mas fwhm; > 97% Strehl

NAOS-CONICA

• K Image; t =150 s.

• 68 mas fwhm; 56% Strehl

NGC 3603

27”

Built by LAM, OHP & OMP (F), IRA,, IFCTR & OAC (I) and ESO

Visible Imaging Multi-Object Spectrograph (VIMOS)

1st light on 26 February ‘02(2 over 4 channels only due to overweight)

Antennae NebulaVRI - 0.6 arcsec. fwhm

VIMOS IFU mode: first galaxy spectra, 3 March 2002

3120 spectra ; 2 x 27” x 27” field (zoomed); Antennae Nebula

First VIMOS Light

FLAMES Facility

FLAMES

25’ field CorrectorOz-Poz & Giraffe

First FLAMES Light

Oz-Poz + UVES31 March ‘02

• Oz-Poz to UVES (8 fibers)• ~ 47,000 spectral resolution

7 stars in Cen

H

VISIR

Built by CEA-Saclay (F) and Astron (NL)

Small Field Intermediate Field Large Field

VISIR 1st light in the Lab (imager mode)

CEA-SACLAY, 19 December 2001

Images of the distortion grid

First VISIR spectra, 24 April 2002Low resolution N-band (R 400), central 9 µm

Mylar absorber

Calibration etalon

Atmospheric line

SINFONI

VLT UT4 (YEPUN)First Light Jan ‘04

SPIFFI3D spectrometer (0.95-2.5µm) FOV = 0”.8 to 8”, ~ 4000(32 x 32) pixels, 1024 channels

MPE

AO Module

60 elements curvatureNatural & Laser Guide Star

ESO internal development

AO-corrected 3D IR spectro-imager any small structured target

SPIFFI 1st light in the Lab

MPE-Garching, 4 June 2002

Image Slicer output (neon source)

unbaffled direct image

MPE-Garching, 5 June 2002

1st Spectrum (neon source)

• 1-5 m range

• ~ 105

• single order (echelle + pre-disperser)

• visible range; ~ 105 echelle

• fibre-coupled to Cassegrain Adapter• 100 n./yr. x 5 yrs @ La Silla 3.6m• ± 1m/s rms long-term accuracy• 1st light 4Q ‘02

High-Accuracy Radial velocity Planetary Searcher (HARPS)

Built by Geneva Observ. & Bern Univ. (CH), OHP & Service d’Aéronomie (F), ESO La Silla & Garching

March ‘02

The VLT as a Science Machine

Solar System Stellar NurseriesNearby Galaxies

Distant galaxiesQuasarsLSS

Large Scale Structure Competition

IMACS/Magellan I [03?] - FMOS/Subaru [?]

VIMOS/ESO [‘02]

NIRMOS/ESO?

DEIMOS/Keck [‘02]

ISAAC/ESO - NIRSPEC/Keck

IRCS/Subaru - GNIRS/Gemini-N

Giraffe/ESO - MODS2/LBT - LHRS/HET

GMOS/Gemini-N - OSIRIS**/GTC

FOCAS/Subaru - FORS2-R/ESOEMIR/GTC - IRMOS/Gemini?

0.3 0.85 2.4 µm

2

32

512

2048

8

128

ESI/Keck - GMOS/Gemini-S

FORS1/ESO - MODS1/LBT

Giraffe*/ESO - GMOS*/Gemini-N

Nobj

LHRS-J/HET

LUCIFER/LBT - MOIRS/Subaru?

*: mini-IFUs

** : Tunable Filter

Stellar Populations Competition

UVES-B/ESO UVES-R/ESO

HROS/Gemini-S - HIRES/Keck

HDS/Subaru

GNIRS/Gemini-N [IFU]

HRS/HET

PHOENIX/Gemini-S

CRIRES/ESO

IRHS/Subaru

0.3 1.2 5 µm

2 x 104

8 x 104

NIRSPEC/Keck - IRCS/Subaru

MRS/HET [10 objects]

Giraffe/ESO [120 objects]

4 x 104 UVES-R/ESO [8 objects]]

HDS+

/Subaru

R

MRS-J/HET

ISAAC/ESO

Cool Universe Competition

VISIR/ESO [‘02]

8 12

102

104

103

18

24

RMax

VISIR/ESO [‘02]

COMICS/Subaru COMICS/Subaru

LWS LWIRC/Keck - CANARI-CAM/GTC LWS LWIRC/Keck [‘01 ?]

T-ReCS/Gemini-S [‘01] T-ReCS/Gemini-S [‘01]

CANARI-CAM/GTC [‘03]

Michelle/Gemini-N [‘02]

OSCIR/Gemini-N OSCIR/Gemini-N

µm

Year0099 0706050401 02 03

NACO NACO / SINFONI MCAO? SINFONI

VLTI 1-2 AO/VLTI 1 - 4

ESO

S

GEMINI

N

GEMINI

KECK

SUBARU

HOKUPA’A+ / GSAO

ALTAIRHOKUPA’A

MCAO

AOF/KCAMNIRC-NIRSPEC

AO INTERFEROMETRY (1-2)

AO (36 act.)/IRCS (90 act.?) /CIAO

?

?

Adaptive Optics Competition

ALTAIR

MACAO-VLTI

200m

4 Telescopes with coudé trains

4 delay lines

combination ~100m from AO

beams combined in ~1m3

open loop NGS tracking

no AO residual piston

=> major challenges

MCAO: a vast challenge ahead

0

Str

ehl

Classical AOClassical AO MCAOMCAO

0

11

But a promising avenue

Multi-Conjugate Adaptive Optics Demonstrator (MAD) 11:25:09

Scale: 0.14 12-Jan-01

178.57 MM

Derotator2-3 Deformable mirrors

2Kx2K IR cameraFOV: 90”

Multi WFS

Nasmyth focus system

FORS2-J ?

• collimator kept; camera with same front clearance• 150 mm shorter; larger back clearance (cryogenic filters)

• 0.8-1.4 µm; same image quality; same field (6’.8 x 6’.8)

• ~ 65 % total transmission

VLT_FOCALREDUCER Scale: 0.45 eso 11-Mar-02

55.56 MM

2k x 2k Array

18 µm px

Filter Wheel

F/2.25 J-camera

2nd Generation Instruments Status

KMOS- Analysis of the need for wide-field Imaging (fall ‘02)

- Prototyping of multi-IFUs concepts with MPE & Milano

Wide-Field Surveyor- MUSE R/D (image slicers & low-cost multi-spectrometers)

- Analysis of Tunable Filter concept as FORS upgrade

Fast Shooter- Assembling a Consortium for a fast decision (fall ‘02)

Planet Finder- Two concepts: reflected light versus intrinsic emission

choice in fall ‘02

2nd Generation Instruments: I- KMOS

IASFC-Milano (D. Maccagni, PI)

Durham, OMP, LAM, IRA, ESO

Cost ~ 7.5 M€ ?

Fully Cryogenic incl. Mask X-change

8’ x 8’ Imaging & Multi-slit field

24 addressable IFUs in 2’ x 8’ field

~ 4,000 (“)4kx4k Array

Nasmyth focus

grating or mirror

F/3 camera

Pupil relay

Filter wheel Collimator

lens

Significant R&D (masks, IFU)

Bad pupil Image quality

(too) large ESO role

““Super-Super-ISAAC”ISAAC”

Fully Cryogenic multi-IFUs

7’.2 dia. Field; 20 to 40 IFUs

2 (2k x 2k) to 8 (2kx2k)

~ 4,000 (“)

2nd Generation Instruments: I- KMOS

MPE/USM (R. Bender, PI)

Durham, ATC, Oxford, Bristol

Cost 5-12 M€; up to 5 M€ contribution

Choice of opto-mechanical system

Cryogenic motions prototyping

Significant ESO role

““Super-Super-SINFONI”SINFONI”

Fully Cryogenic incl. Mask cryostat

6’ dia. Imaging; 2’ x 6’ Multi-slit

1 (2k x 2k) Array

~ 1,000 (“) with Grisms

2nd Generation Instruments: I- KMOS

University of Florida (R. Elston, PI)

Full Cost 5.5 M€

“modest” System; 2007 delivery

Operational overheads t.b.e.

Major “VLT standard” issue

““Super-SOFSuper-SOF I”I”

2nd Generation Instruments: I- KMOS

The Multi-slit Challenge:The Multi-slit Challenge:

Sensitive enough to use the multiplex Sensitive enough to use the multiplex advantageadvantage

The Multi-IFU Challenge:The Multi-IFU Challenge:

Efficient enough to keep single IFU Efficient enough to keep single IFU detectivitydetectivity

2nd Generation Instruments: II- High-z Surveyor

MUSEMUSE

1’ x 1’ field IFU; 0.48-0.95 µm

24 Spectrometers (4k x 2k)

No moving part, Nasmyth (fixed)

~ 2,000

CRAL-Lyon (R. Bacon, PI)

Durham, OP, Leiden, Cambridge

IAP, LAM, ETH, AIP-Postdam

Cost < 9 M€ ?

Advanced Image Slicers R&D

Low-cost identical systems

High efficiency required

MCAOfocal plane

Enlarger/Anamorphoser Field-splitter

Split focal plane

Image slicer

Spectrometerpseudo-

entrance slit

CollimatorCamera

CCDplane

Dispersing element

Spectrometer

Sub-FoV

2nd Generation Instruments: II- High-z Surveyor

MUSE - low cost spectrometerMUSE - low cost spectrometer

• 0.48-0.95 µm; tilted focal plane

• cryostat head cooling plant

• no motorized part; ~ 2,000 • possible ~ 6,000 [0.48-0.55 µm] (VPHG grism + zero power group)

• opto-mechanics Cost < 1 M€ (24 units)

11:23:27

Scale:0.23Position: 1

ESO 11-Mar-02

108.70 MM

slit

collimator

camera

grism

detector

100 mm pupil

2nd Generation Instruments: II- High-z Surveyor

FASTFAST

Tunable Filter (Fabry-Perot)

Plus high-order scanning FP

370-860 nm

Extensive data reduction SW

LAM-Marseille (M. Marcelin, PI)

Bochum, Byurakian, ESO, OP, Keele, LAE-Montreal, MPIA-Heidelberg, Brera, Oulu, Ahmedabad, Montreal

Cost 0.84 M€

LLL-CCD evaluation

FORS upgrade ?

2nd Generation Instruments: III- Fast Shooter

Triple arm Cassegrain spectrograph

Single slit; 320 to 2400 nm

~ 5,000 (“)

NBI-Copenhagen (P. Rasmussen, PI)

Amsterdam, Tuorla, Sheffield, Southampton, Dwingeloo, ESO

Cost ~ 3 M€ ?

Dicroic or predisperser ?

LLL-CCD evaluation

HEIDIHEIDI

SN 1987A

~ 105 - U to z

2nd Generation Instruments: III- Fast Shooter

Triple arm Spectrograph

Single slit; 320 to 2400 nm

~ 5,000 (“)

OAR-Roma (D. Lorenzetti, PI)

Bologna, Brera, Catania, Padova, Palermo, Trieste

Cost ~ 3 M€ ?

Image slicer ?

Nasmyth (fixed) or Cassegrain

May merge with HEIDI

FIESTAFIESTA

SN 1987A

~ 105 - U to z

2nd Generation Instruments: III- Fast Shooter

Triple arm Spectrograph

Integral field; 320 to 2400 nm

~ 5,000 (“)

OP-Paris (F. Hammer, PI)

Paris-7, IAP

Cost ?

Fast tip/tilt + focus option

Merge with HEIDI & FIESTA ?

IFASTIFAST

2nd Generation Instruments: III- Fast Shooter

5,000 px STJ + Echelle Spectrograph

320 to 2400 nm; ~ 10,000

No spatial information (upgrade?)

UCL-London(M. Cropper, PI)

ESTEC, Cambridge, St Andrews, Southampton

Cost 5.6 M€

Huge ESTEC development needed

SESSES

GRB 990511

SCAM-WHT

2nd Generation Instruments: IV- Planet Imager

Nasmyth (fixed)

H+J integral field; I polarimetric imaging

2 conjugate high-order AO mirrors

MPIA-Heidelberg (M. Feldt, PI)

Padova, Lisboa, Amsterdam, MPE, Tautenburg, ETH, Postdam, OAC, Leiden, Jena, Arcetri, Brera

Cost 4.1 M€

LLL-CCD at 400 MHz (?)

1600 actuators development (Xinetics?)

2nd Generation Instruments: IV- Planet Imager

Advanced coronography

differential multi- & polarimetric imaging

High-order AO mirror

LAOG-Grenoble (A.M. Lagrange, PI)

LAM, ONERA, OP, Nice, OCA, Montreal, Durham, UCL, ATC, Geneve

Cost ?

Detector (?)

High order AO development (Cilas?)

Phase Stop

(10’)2 deployable IFUs(seeing-limited, up to K)

(1’)2 Single IFU(w./w.o. AO)

2nd Generation: Towards High-z Mass Assembly

(7’)2 Imaging-multi-slit(seeing-limited, up to K)

(2’)2 Imaging-multi-slit(MCAO-assisted, up to K)

What flavors?

OSIRIS/GTCLUCIFER/LBT

CROMOS/MPE

MCAO/GEMINIMUSE (AO)/CRAL

IRMOS/LAM-ESO

MEIFU (no AO)/Durham

MOS/ATC-Durham

ISAAC 6 hr exposurez ~3.2 - 0”.4 seeing

(25’)2 deployable IFUs(MCAO-assisted)

FALCON/OP

- X-dispersed echelle a la UVES (or FTS ?)

- Small integral field probe ?

- Multiple arms a la UVES (“x-shooter”)

SN 1987A

~ 105 - U to z

2nd Generation: the fast shooter

~ 104 , Wide-Band (0.35-2.4 m) spectroscopy

Z~ 2.2 Quasar

GRB 990511

Stringent specifications

System aspect essentialSystem aspect essential

Phase Stop

Nuller

“Planet Imager”

2nd Generation: peering around nearby stars

- high contrast Adaptive Optics (new techniques &components)

- advanced coronography