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

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Presentation transcript:

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

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

MIDI in the VLTI lab IRIS FINITO

MIDI in the VLTI lab

The MIDI cold optics

Coaxial beam combination

MIDI lab fringes

The VLTI Telescopes

VLTI Optical Layout

Configurations

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

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

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

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

MIDI Publications Nature: –Jaffe et al The central dusty torus in the active nucleus of NGC 1068 –Van Boekel et al 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

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

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

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

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

Acquisition with Coudé guide stars

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

Spectrum extraction and sky windows

Dispersed interference fringes λ OPD Courtesy: Th. Ratzka 0

Fringe scanning

SCI_PHOT mode (simultaneous chopping)

Visibility amplitude calibration Calibrator: HD D = 3.8 mas

Calibrator selection

Jean-Marie Mariotti Center (JMMC) tools

Visibility amplitudes of a binary source

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 – (MIDI page) – (data reduction) – (software) – (Long Baseline Interferometry)