1. MIDI design, performance, operations, and science Markus Schöller (INS)

2. Why do we use interferometers? Objects Single Telescope Interferometric Fringes Angular Resolution: ~ /D ~ /B Small star Big star

3. MIDI in the VLTI lab IRIS FINITO

4. MIDI in the VLTI lab

5. The MIDI cold optics

8. Coaxial beam combination

9. MIDI lab fringes

10. The VLTI Telescopes

11. VLTI Optical Layout

12. Configurations

13. The uv-plane Where do we sample the spatial frequencies?

14. If you have never tried to FFT -1 … Phase is essential for interferometric imaging

15. Coming next: MATISSE MATISSE will provide: Four telescope beam combination (six baselines, four closure phases) L/M/N band Roughly identical sensitivity R~30-1000 (L/M), R~30-200 (N)

16. MIDI design, performance, operations, and science Christian Hummel (USD)

17. MIDI Publications Nature: –Jaffe et al. 2004 The central dusty torus in the active nucleus of NGC 1068 –Van Boekel et al. 2004 The building blocks of planets within the terrestrial region of proto-planetary disks A&A (72), MNRAS (2), ApJ (9), Icarus (2) Source: ESO Telescope Bibliography at http://telbib.eso.org

18. VLTI publications From: Basic ESO Publication Statistics, 2012, prep. by Grothkopf & Meakins OLBIN

19. Science with MIDI Jaffe et al. van Boekel et al. Zhao-Geisler

20. Science Operations VLTI UT scheduled in blocks Night astronomer selects telescopes from quadruplets OBs selected from MIDI and AMBER queues LST intervals allow user to achieve specific projected Science targets interleaved with interferometric calibrators

21. Operational efficiency MIDI XSHOOTER SQL/IDL code courtesy of Vincenzo Mainieri

22. Acquisition with Coudé guide stars

23. Instrument modes HIGH_SENS: no photometric channels, separate observation for photometry –GRISM: R=320 –PRISM: R=30 SCI_PHOT: simultaneous photometry, chopping –PRISM GRISM

24. Spectrum extraction and sky windows

25. Dispersed interference fringes λ OPD Courtesy: Th. Ratzka 0

26. Fringe scanning

27. SCI_PHOT mode (simultaneous chopping)

28. Visibility amplitude calibration Calibrator: HD 50778 D = 3.8 mas

29. Calibrator selection

30. Jean-Marie Mariotti Center (JMMC) tools

31. Visibility amplitudes of a binary source

32. Observing with MIDI OK with seeing up to 1.5” (limited by MACAO/STRAP) SCI-CAL or CAL-SCI-CAL sequences in concatenations (p2pp3) 25 minutes execution time per OB independent of target Simple model fitting only, spatial resolution 15 – 130 mas Resources –http://www.eso.org/sci/facilities/paranal/instruments/midi/ (MIDI page)http://www.eso.org/sci/facilities/paranal/instruments/midi/ –http://www.eso.org/~chummel/midi/midi.html (data reduction)http://www.eso.org/~chummel/midi/midi.html –http://home.strw.leidenuniv.nl/~nevec/MIDI/index.html (software)http://home.strw.leidenuniv.nl/~nevec/MIDI/index.html –http://olbin.jpl.nasa.gov/news/index.html (Long Baseline Interferometry)http://olbin.jpl.nasa.gov/news/index.html