1. INS SW Workshop, Garching 8 October, 2008 Andrea Richichi European Southern Observatory

2. The VLTI Today + FINITO, IRIS, Delay Lines, DDL, ARAL/Marcel, vibration correction,...

3. FINITO offFINITO on IRIS AMBER Medium Res 3 ATs

4. The VLTI Tomorrow MATISSEVSIGRAVITY 3-20µm, 4 beams1-2.5µm, 4-6 beams2.2µm, 4x2 beams Phase A studies concluded (Sep’07) for 2 nd Generation Instruments PRIMA Dual-feed facility Start of integration in Paranal in 2008 First scientific use in 2009 TBC PRIMA Dual-feed facility Start of integration in Paranal in 2008 First scientific use in 2009 TBC

5. Science Cases for MATISSE 1.Star and Planet Formation (e.g. Signatures of Planet Formation, Debris Disks, Mineralogy of Protoplanetary Disks, Binaries, Outbursting YSOs, Massive Star Formation) 2.Evolved Stars 3.Solar System Minor Bodies 4.Extrasolar Planets 5.Active Galactic Nuclei 6.Galactic Center Science Cases for MATISSE 1.Star and Planet Formation (e.g. Signatures of Planet Formation, Debris Disks, Mineralogy of Protoplanetary Disks, Binaries, Outbursting YSOs, Massive Star Formation) 2.Evolved Stars 3.Solar System Minor Bodies 4.Extrasolar Planets 5.Active Galactic Nuclei 6.Galactic Center Unique Breakthroughs: Imaging in N band (general use of closure phases) L&M band extension (simultaneous observations in L&M and N band) Unique Breakthroughs: Imaging in N band (general use of closure phases) L&M band extension (simultaneous observations in L&M and N band)MATISSE PI Nice (F,D,NL,others)

6. MATISSE Science left: model right: reconstruction Protoplanerary disk with planet AGN gas+dust torus Model Reconstruction

7. GRAVITY 6 R S Earth Orbit R S ~ 10 µas General relativity dominates observations: Lensing Beaming Dopplershift Gravitational redshift Design driven entirely by science goal: the black hole in the GC Courtesy F. Eisenhauer PI MPE (D,F,P)

8. Working principle illustrated IRS7, K=6.5, 5.57” separation, AO wavefront reference IRS16C, K=9.7, 1.23” separation, fringe tracking phase reference Galactic Center Black Hole, science object IRS16NW, K=10.0, 1.21” separation, guide star (for tip-tilt residual) VLTI 2” FoV 10”

9. VSI (VLTI Spectro Imager) Extension of AMBER: emphasis on snapshot “imaging” (general use of closure phases) combine 4/6(8) telescopes (observations in J,H,K bands) specialized fringe tracker (now separated) Integrated Optics Design Extension of AMBER: emphasis on snapshot “imaging” (general use of closure phases) combine 4/6(8) telescopes (observations in J,H,K bands) specialized fringe tracker (now separated) Integrated Optics Design PI Grenoble (F,D,I,UK, others)

10. left: model right: reconstruction Surfaces of late-type stars Supergiant Giant VSI (VLTI Spectro Imager) AGN gas+dust torus u-v coverageModel left: 130m telescope right: VLTI (4 UT) 5 mas

11. VSI Control System Design G. Zins, VSI Phase A

12. Costs and schedule October 2007 estimates GRAVITY MATISSE VSI Kick-off PDR FDR PAE 200820092010201120122013 2GFT Phase A ? ? ESO provides detector systems as in-kind contribution, and reimburses capital and FTE costs with GTO Preliminary!

13. Control and Data

14. Conclusions A total of 3 instruments + 1 new fringe trackerA total of 3 instruments + 1 new fringe tracker 2 instruments on track; other one and FT ~1 year delay2 instruments on track; other one and FT ~1 year delay More complex than AMBER and MIDI because of more telescopesMore complex than AMBER and MIDI because of more telescopes Similar data flow, perhaps x2 more than AMBER/MIDISimilar data flow, perhaps x2 more than AMBER/MIDI Most HW will be to ESO standardsMost HW will be to ESO standards Include new standards: CAN, NGC, CPL, ReflexInclude new standards: CAN, NGC, CPL, Reflex