The MPIA is leading an international consortium
of institutes in building an instrument initially called LINC,
the LBT INterferometric Camera.
Our collaborators include the Arcetri Astrophysical Observatory (Firenze), the MPI for Radioastronomy (Bonn), and the University of Köln .
LINC will combine the radiation from the two 8.4 m primary mirrors of the LBT in so-called "Fizeau" mode. This configuration preserves phase information, and allows true imagery over a wide field of view. The beam combiner will operate at wavelengths between 0.6 and 2.4 microns, using state-of-the-art detector arrays. When coupled with the advanced adaptive optics system of the LBT, the LINC instrument will deliver the sensitivity of a 12 m telescope and the spatial resolution of a 23 m telescope, over a field approximately 10-20 arcseconds square.
LINC will combine the radiation from the two 8.4 m primary mirrors of the LBT in so-called "Fizeau" mode. This configuration preserves phase information, and allows true imagery over a wide field of view. The beam combiner will operate at wavelengths between 0.6 and 2.4 microns, using state-of-the-art detector arrays. When coupled with the advanced adaptive optics system of the LBT, the LINC instrument will deliver the sensitivity of a 12 m telescope and the spatial resolution of a 23 m telescope, over a field approximately 10-20 arcseconds square.
(Move your mouse over the image to zoom in on LINC / NIRVANA)
( Click on the image to see the full-size version)
The interferometric camera will be developed in two steps, the first (LINC)
incorporating a single, on-axis adaptive optics (AO) system. Ultimately, multi-conjugate
AO will provide diffraction-limited performance over a wider field of view. After
completion of the second phase, the instrument will be known as NIRVANA, the Near-IR
/ Visible Adaptive INterferometer for Astronomy.
The image at the top right shows the LINC/NIRVANA interferometric camera (center part) mounted on the central instrument platform of the LBT. Light from the sky reflects from the two primary mirrors through an intermediate focus then bounces off the adaptive secondary mirrors. Tertiary mirrors directly above the primaries then redirect the radiation into the instrument.