2. PatMaj

3. 1 st light dates between ( ) AO-based instruments in red 15 May ‘02 Development Concept STC VLT Instruments StatusStudy Plan Operation FORS1 (3Q ’98) ISAAC (4Q ’98) UVES (3Q ’99) FORS2-R (4Q ’99) PAECommissioning PAC NAOS-CONICA VIMOS Oz-Poz/UVES Oz-Poz/Giraffe AIT VISIR (4Q ’02) MACAO (4Q ’02) Fabrication SINFONI (1Q ’04) CRIRES (3Q ’04) MAD (3Q ‘03) FDRDesign Final Design NIRMOS (?) Prelim. Design 1st Generation Upgrades 2nd Generation Projects 2 nd Generation Instruments

4. Paranal Observatory

6. VLT(I) Instrumentation An extensive  -  Coverage 110 (µm) VLTI

7. VLT Instrumentation An extensive - /  Coverage

8. VLT Instrumentation An extensive set of modes VLT MULTI-OBJECT SPECTROGRAPHY

9. 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 - ISAACUT2 - UVES UT3 - FORS1UT4 - FORS2

10. FORS-1 & FORS-2 FORS-1 & FORS-2

11. FORS Image Quality & Stability §Image Quality Telescope driven Best image obtained (HR mode) 0.18” (integration time: a few seconds) 0.25” (integration time: several minutes) VLT + FORS-1 Seeing ~ 0.6” Keck + LRIS Seeing ~ 0.55”  Image Stability exceptional Ellipticity distribution Red: uncorrected Blue: corrected young brown dwarf I band - TW5 system

12. FORS Spectroscopic Sensitivity §4 hour integration (FORS2) §0.5” seeing §excellent defringing l dithering l stability of instrument I=22.9 I=23.7 I=24.4 z = 1.07 z = 1.229 z = 1.036 Rosati 2001

13. FORS2-R Upgrade §Better sensitivity §Very little fringing §Good astrometry

14. ISAAC

15. ISAAC Image Quality Jupiter Aurorae Io, deconvolved 0.4” image NB 4.07 µm

16. ISAAC Spectroscopic Sensitivity z =3.2 galaxy “rotation” (  V ~ 700 km/s) OIII lines; 6 hr exposure; 0”.4 seeing

17. UVES @ UT2 Nasmyth X-dispersed echelle spectrum

18. UVES: highly sensitive R~10 5 Spectrometer Towards Beryllium primordial abundance 1 st optical detection of a stellar coronal line 1 st Uranium detection outside Solar System Two optimized channels  high efficiency from 0.30 to 0.98 µm

19. UVES: high precision radial velocities UVES + iodine cell Commissioning data Dec 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)

20. NAOS-CONICA at Nasmyth UT4 VLT Adapter NAOS CONICA Cable Twist Built by ONERA,, OP & LAOG (F), MPIA & MPE (D) and ESO

21. NAOS-CONICA Nov. ‘01

22. 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”

23. Built by LAM, OHP & OMP (F), IRA,, IFCTR & OAC (I) and ESO Visible Imaging Multi-Object Spectrograph ( VIMOS )

24. 1 st light on 26 February ‘02 (2 over 4 channels only due to overweight) Antennae Nebula VRI - 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

25. FLAMES Facility

26. FLAMES 25’ field Corrector Oz-Poz & Giraffe

27. First FLAMES Light Oz-Poz + UVES 31 March ‘02 Oz-Poz to UVES (8 fibers)  ~ 47,000 spectral resolution 7 stars in  Cen HH

28. VISIR Built by CEA-Saclay (F) and Astron (NL)

29. Small FieldIntermediate FieldLarge Field VISIR 1 st light in the Lab (imager mode) CEA-SACLAY, 19 December 2001 Images of the distortion grid

30. First VISIR spectra, 24 April 2002 Low resolution N-band (R  400), central   9 µm Mylar absorber Calibration etalon Atmospheric line

31. SINFONI VLT UT4 (YEPUN) First Light Jan ‘04 SPIFFI 3D spectrometer (0.95-2.5µm) FOV = 0”.8 to 8”,  ~ 4000 (32 x 32) pixels, 1024 channels MPE AO Module 60 elements curvature Natural & Laser Guide Star ESO internal development AO-corrected 3D IR spectro-imager  any small structured target

32. SPIFFI 1 st light in the Lab MPE-Garching, 4 June 2002 Image Slicer output (neon source) unbaffled direct image  MPE-Garching, 5 June 2002 1 st Spectrum (neon source)

33. 1-5  m range  ~ 10 5 single order (echelle + pre-disperser)

34. visible range;  ~ 10 5 echelle fibre-coupled to Cassegrain Adapter 100 n./yr. x 5 yrs @ La Silla 3.6m ± 1m/s rms long-term accuracy 1 st 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

35. The VLT as a Science Machine Solar SystemStellar Nurseries Nearby Galaxies Distant galaxies Quasars LSS

36. 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/ESO EMIR/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 N obj LHRS-J/HET LUCIFER/LBT - MOIRS/Subaru? *: mini-IFUs ** : Tunable Filter

37. 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 10 4 8 x 10 4 NIRSPEC/Keck - IRCS/Subaru MRS/HET [10 objects] Giraffe/ESO [120 objects] 4 x 10 4 UVES-R/ESO [8 objects]] HDS + /Subaru R MRS-J/HET ISAAC/ESO

38. Cool Universe Competition VISIR/ESO [‘02] 8 12 10 2 10 4 10 3 18 24 R Max VISIR/ESO [‘02] COMICS/Subaru LWS  LWIRC/Keck - CANARI-CAM/GTC LWS  LWIRC/Keck [‘01 ?] T-ReCS/Gemini-S [‘01] CANARI-CAM/GTC [‘03] Michelle/Gemini-N [‘02] OSCIR/Gemini-N µm

39. Year009907060504010203 NACONACO / SINFONIMCAO? SINFONI VLTI 1-2AO/VLTI 1 - 4 ESO S GEMINI N GEMINI KECK SUBARU HOKUPA’A + / GSAO ALTAIRHOKUPA’A MCAO AOF/KCAM  NIRC-NIRSPEC AO INTERFEROMETRY (1-2) AO (36 act.)/IRCS  (90 act.?) /CIAO ? ? Adaptive Optics Competition ALTAIR

40. MACAO-VLTI  200m 4 Telescopes with coudé trains 4 delay lines u combination ~100m from AO  beams combined in ~1  m 3 u open loop NGS tracking u no AO residual piston => major challenges

41. MCAO: a vast challenge ahead

42. 0 Strehl Classical AO MCAO 0 1 1 But a promising avenue

43. Multi-Conjugate Adaptive Optics Demonstrator (MAD) Derotator 2-3 Deformable mirrors 2Kx2K IR camera FOV: 90” Multi WFS Nasmyth focus system

44. 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 2k x 2k Array 18 µm px Filter Wheel F/2.25 J-camera

45. 2 nd 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

46. 2 nd 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 wheelCollimator lens Significant R&D (masks, IFU) Bad pupil Image quality (too) large ESO role “Super-ISAAC”

47. Fully Cryogenic multi-IFUs 7’.2 dia. Field; 20 to 40 IFUs 2 (2k x 2k) to 8 (2kx2k)  ~ 4,000 (“) 2 nd 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- SINFONI”

48. Fully Cryogenic incl. Mask cryostat 6’ dia. Imaging; 2’ x 6’ Multi-slit 1 (2k x 2k) Array  ~ 1,000 (“) with Grisms 2 nd 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-SOF I”

49. 2 nd Generation Instruments: I- KMOS The Multi-slit Challenge: Sensitive enough to use the multiplex advantage The Multi-IFU Challenge: Efficient enough to keep single IFU detectivity

50. 2 nd Generation Instruments: II- High-z Surveyor MUSE 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

51. 2 nd Generation Instruments: II- High-z Surveyor MUSE - 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) 100 mm pupil

52. 2 nd Generation Instruments: II- High-z Surveyor FAST 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 ?

53. 2 nd 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 HEIDI SN 1987A  ~ 10 5 - U to z

54. 2 nd 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 FIESTA SN 1987A  ~ 10 5 - U to z

55. 2 nd 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 ? IFAST

56. 2 nd 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 SES GRB 990511 SCAM-WHT

57. 2 nd 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?)

58. 2 nd 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

59. (10’) 2 deployable IFUs (seeing-limited, up to K) (1’) 2 Single IFU (w./w.o. AO) 2 nd 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/GTC LUCIFER/LBT CROMOS/MPE MCAO/GEMINI MUSE (AO)/CRAL IRMOS/LAM-ESO MEIFU (no AO)/Durham MOS/ATC-Durham ISAAC 6 hr exposure z ~3.2 - 0”.4 seeing (25’) 2 deployable IFUs (MCAO-assisted) FALCON/OP

60. - X-dispersed echelle a la UVES (or FTS ?) - Small integral field probe ? - Multiple arms a la UVES (“x-shooter”) SN 1987A  ~ 10 5 - U to z 2 nd Generation: the fast shooter   ~ 10 4, Wide-Band (0.35-2.4  m) spectroscopy Z~ 2.2 Quasar GRB 990511

61. Stringent specifications  System aspect essential Phase Stop Nuller “Planet Imager” 2 nd Generation: peering around nearby stars - high contrast Adaptive Optics (new techniques &components) - advanced coronography