LBT An Adaptive Telescope

To show an application of adaptive optics to an 8 m class telescope, we will briefly describe the AO system of the Large Binocular Telescope (LBT). The LBT with AO can be used in single dish or interferometric mode. The LBT is a binocular telescope made up of two 8.4 m primary mirrors. The mirrors are placed on the same mount and can work as two separate units or as an interferometer (the center to center distance of the two primary mirrors is 14 m). A drawing of the telescope is presented in Fig. 14. It is also interesting to

Lucifer Telescope
Fig. 14. The Large Binocular Telescope mechanical drawing, showing the two primary mirrors supported by a single mount. Cylinders between the two primary mirrors represents the adaptive intruments of the LBT. From bottom to top they are LUCIFER, LBTI, and NIRVANA

note that LBT is possibly the first 8 m telescope to have an adaptive secondary mirror [24]. In other words, both the secondary mirrors of the LBT will have 672 actuators and can provide adaptive correction for all the telescope focii. We will considered in the following all the instruments that are located at the Bent Gregorian focal stations. Those stations and instruments are represented by the cylinders in Fig. 14.

7.1 LUCIFER: The Single Dish Imager and Spectrograph

We begin our AO system description with LUCIFER6 [21], the NIR im-ager and spectrograph placed at the front Bent Gregorian focal station of LBT. This instrument can work in seeing limited or diffraction-limited conditions with a Field of View of 4 x 4 or 0.5 x 0.5 arcminutes, respectively (some instrument characteristics, particulary for these modes, are reported in Table 1).

6 LBT NIR spectroscopic Utility with Camera and Integral-Field Unit for Extragalactic Research.

Table 1. Some basic characteristics of LUCIFER's imaging and spectroscopic modes

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