The European Solar Telescope (EST) is a 4-m class-solar telescope that will become part of the next generation of groundbased facilities. Located at the “Observatorio del Roque de los Muchachos” in La Palma (Spain), it will be aimed to study the magnetic connectivity of the solar atmosphere with high spatial and temporal resolution. The EST optical design has been optimized during the preliminary design phase to maximize throughput, balance the instrumental polarization and to reduce the image rotation due to the change in orientation during operation. The optical system consists of a 4.2m active primary mirror located above the elevation axis to ensure natural air flushing and minimize local seeing degradation and a secondary mirror assembled as an Adaptive Secondary Mirror (ASM). Both arranged in an on-axis Gregorian configuration to deliver an aplanatic secondary focal plane. These are followed by four fold mirrors, which will be upgraded to deformable mirrors and are conjugated to different layers of the atmosphere. These, together with the ASM, M7 and two wavefront sensors, will make up the Multi-Conjugate Adaptive Optics system. Finally, a dioptric system, housed in a vacuum vessel, transfers the light to the science focus, which will be delivered to the Scientific Instrumentation by a dedicated distribution system. EST ultimately provides a diffraction-limited telecentric F/50 science focal plane covering a FOV of 90×90 arcsec2 over a wavelength range from 380nm to 2300nm. Along the contribution, details about the preliminary optical design of EST and its subassemblies will be presented. The expected performance is also discussed.
ANDES,the high resolution spectrograph for the ELT, will work both in seeing limited mode and with Adaptive Optics (AO) correction. ANDES-SCAO is a single conjugated AO system working with natural guide stars, feeding the IFU coupled to the YJH spectrograph. The main science goal of the ANDES AO mode is the characterization of the exo-planet atmosphere in reflected light. Hence, the driving technical requirement for the AO system is the PSF contrast. The level of achieved contrast determines the number of exo-planets on which the instrument will be able to detect bio-signatures. The key challenge for the achievement of high contrast is the control of M4 petalling. Here, we present the current status of the ANDES-SCAO design, approaching the ANDES preliminary design review scheduled in fall 2024.
The Adaptive and Lucky Imagine Optics Lightweight Instrument (ALIOLI) is a portable Adaptive Optics (AO) system capable of being installed on different medium-sized telescopes due to a modular approach to its components. The Wavefront Sensor (WFS) module is designed to be used with three different WFSs: Shack-Hartmann (SH), Two Pupil Plane Position (TP3), and Pyramidal unmodulated, allowing a joint configuration for comparative studies of WFS response when different observing situations. In this article we show the assembly of the TP3 module and we summarize the first open-loop measurements on the bench. These results have been compared with those obtained in the simulation phase. Finally, we present the next proposed tests and the steps to follow for possible updates.
Adaptive optics (AO) systems correct atmospheric turbulence in real time and they are normally used in large and medium telescopes but not in modest telescopes due to their size and cost. Here we propose a portable AO instrument capable of being installed in different medium and small-sized telescopes. The novelty of this new instrument is that it is based on the modularization of its components: simulator/calibrator, Wavefront Corrector (WFC) with a deformable mirror (DM) and Wavefront sensor (WFS) modules. This modular concept allows great flexibility in the design, being possible to easily adapt the instrument to the working telescope or instrument by adjusting each module independently. This concept also makes possible the comparison between different types of WFS such as Shack-Hartmann (S-H), Two Pupil Plane Position (TP3) or Pyramidal. Here we present the optical design and expected performance of the three WFS for 1.52m, Carlos Sanchez Telescope (TCS), and the preliminary results of the S-H sensor in laboratory and the first on-sky test.
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