After a brief introduction of the SDSS-V optical instrumentation installed at the Apache Point 2.5m telescope, the presentation will be mainly focused onto the optical production and testing of the 3 large lenses (diameter 700-800mm) constituting the wide field optical corrector (WFC). Special emphasis will be made onto the measurement issues and solutions of the deep aspherical surfaces as well as the review of the specific anti-reflection (AR) coating with development of a dual band anti-reflective coating, carried out by Thales SESO-France. Before concluding, a dedicated paragraph will address on-sky imaging performances results with this new WFC. The presentation will conclude by a brief overview of the corresponding existing “state of the art” at Thales SESO for future manufacturing of similar or large optics for next generation of very wide field corrector.
For Space Activities, more and more Corner Cubes, used as solution for retro reflection of light (telemetry and positioning), are emerging worldwide in different projects. Depending on the application, they can be massive or hollow Corner Cubes. For corners as well as for any kind of space optics, it usual that use of light/lightened components is always a baseline for purpose of mass reduction payloads. But other parameters, such as the system stability under severe environment, are also major issues, especially for the corner cube systems which require generally very tight angular accuracies.
For the particular case of the hollow corner cube, an alternative solution to the usual cementing of the 3 reflective surfaces, has been developed with success in collaboration with CNES to guarantee a better stability and fulfill the weight requirements.. Another important parameter is the dihedral angles that have a great influence on the wavefront error. Two technologies can be considered, either a Corner Cubes array assembled in a very stable housing, or the irreversible adherence technology used for assembling the three parts of a cube. This latter technology enables in particular not having to use cement. The poster will point out the conceptual design, the manufacturing and control key-aspects of such corner cube assemblies as well as the technologies used for their assembling.
For space born Astronomy as well as Earth Observation from space, more and more focal plane instruments are operating in the near or mid infrared and require therefore optics operating at cryogenic temperature (down to liquid nitrogen temperature or less).
Through several examples of typical past or on-going realizations for different projects requiring such cryogenics optics (e.g. MTG=Meteosat Third Generation program for ESA), the presentation will point out the main technical issues and corresponding solutions for design, manufacturing and testing of necessary lens assemblies, mirrors and relevant optical coatings.
A brief review of the corresponding existing “state of the art” for these technologies in Thales Seso will conclude the presentation.
The Meteosat Third Generation (MTG) Programme is being realised through the well established and successful Cooperation between EUMETSAT and ESA. It will ensure the future continuity of MSG with the capabilities to enhance nowcasting, global and regional numerical weather prediction, climate and atmospheric chemistry monitoring data from Geostationary Orbit.
Many high power laser facilities are in operation all around the world and include various tight optical components such as large focussing lenses. Such lenses exhibit generally long focal lengths which induces some issues for their optical testing during manufacturing and inspection. Indeed, their transmitted wave fronts need to be very accurate and interferometric testing is the baseline to achieve that. But, it is always a problem to manage simultaneously long testing distances and fine accuracies in such interferometry testing. Taking example of the large focusing lenses produced for the Orion experimentation at AWE (UK), the presentation will describe which kind of testing method has been developed to demonstrate simultaneously good performances with sufficiently good repeatability and absolute accuracy. Special emphasis will be made onto the optical manufacturing issues and interferometric testing solutions. Some ZEMAX results presenting the test set-up and the calibration method will be presented as well. The presentation will conclude with a brief overview of the existing “state of the art” at Thales SESO for these technologies.
After two years of research and development under ESO support, LAM and Thales SESO present the results of their experiment for the fast and accurate polishing under stress of ELT 1.5 meter segments as well as the industrialization approach for mass production. Based on stress polishing, this manufacturing method requires the conception of a warping harness able to generate extremely accurate bending of the optical surface of the segments during the polishing. The conception of the warping harness is based on finite element analysis and allowed a fine tuning of each geometrical parameter of the system in order to fit an error budget of 25nm RMS over 300μm of bending peak to valley. The optimisation approach uses the simulated influence functions to extract the system eigenmodes and characterise the performance. The same approach is used for the full characterisation of the system itself. The warping harness has been manufactured, integrated and assembled with the Zerodur 1.5 meter segment on the LAM 2.5meter POLARIS polishing facility. The experiment consists in a cross check of optical and mechanical measurements of the mirrors bending in order to develop a blind process, ie to bypass the optical measurement during the final industrial process. This article describes the optical and mechanical measurements, the influence functions and eigenmodes of the system and the full performance characterisation of the warping harness.
After a brief introduction of what is the Dark Energy Survey (DES) project and which optical instrumentation will be
used, the presentation will be mainly focused onto the optical production of the large lenses (up to 1m diameter)
constituting the DES Camera (DECAM) located at the focal plane of the main observing telescope. Special emphasis
will be made onto the optical manufacturing issues and interferometric testing solutions, including compensation of
index inhomogeneities, which have been carried out by THALES SESO especially for the biggest entrance lens (very
challenging CV/CX meniscus named C1). Through several examples of typical past realizations or future possible
ones for different astronomical projects requiring 1m-class optics, the presentation will conclude by a brief over
review of the corresponding existing "state of the art" at THALES SESO for these technologies.
After a brief introduction of what is the Dark Energy Survey (DES) project and which optical instrumentation will be
used, the presentation will be mainly focused onto the optical production of the large lenses (up to 1m diameter)
constituting the DES Camera (DECAM) located at the focal plane of the main observing telescope. Special emphasis
will be made onto the optical manufacturing issues and interferometric testing solutions, including compensation of
index inhomogeneities, which have been carried out by SESO especially for the biggest entrance lens (very challenging
CV/CX meniscus named C1). Through several examples of typical past realizations or future possible ones for different
astronomical projects requiring 1m-class optics, the presentation will conclude by a brief over review of the
corresponding existing "state of the art" at SESO for these technologies.
For ground-based astronomy, more and more large telescopes are emerging all around the world. Similarly to space
borne telescopes, for which the use of lightened optics has always been a baseline for purpose of mass reduction of
payloads, same kinds of lightened/light mirrors are then now more and more intensively used also for ground-based
instrumentation for astronomy, requiring larger and larger components. Through several examples of typical past
realizations (class 0.5m-1m) for different astronomical projects requiring light or lightened mirrors for different reasons
(optimisation of mass and stiffness, reduction of thermal inertia, increasing of dynamic performance for fast scanning
purpose,....), the presentation will point out issues for lightening design, manufacturing and control of such parts, as well
as brief overview of the corresponding existing "state of the art" for these technologies in SESO.
KEYWORDS: Mirrors, Space telescopes, Telescopes, Off axis mirrors, Manufacturing, Space mirrors, Polishing, Control systems, Interferometry, Satellites
Pleiades is the last generation of French satellite for earth observation. For this space program, SESO has been awarded the
contract (fully completed end 2006), for the manufacturing of the whole set of telescope mirrors (EM, QM and FM, primary
mirror with 700mm CA). These works did also include the mechanical design, manufacturing and mounting of the
attachment flexures (MFDs) between the mirrors and the telescope main structure. This presentation will be focused on the
different steps of manufacturing and control of these mirrors, as well as a presentation of the existing SESO facilities and
capabilities to produce such kind of aspherical components/sub-assemblies.
Large adaptive secondary mirrors are a promising solution for the next generation of high order adaptive optics systems and are under development in all major observatories. One of the key points of these systems is the manufacturing of the large glass thin shell, often convex aspheric, used as the 'mirror surface' and attached to the actuators. Due to the very tight surface quality specifications for high order or extreme adaptive optics systems (XAO), one of the major challenges is to avoid all high spatial frequencies errors during the manufacturing of these extremely thin convex hyperbolic shells. In order to achieve the required surface quality, we present an active optics technique based on elasticity theory and mirror polishing under constraints, allowing to easily generate highly aspheric optics, using only full size tools (spherical or flat), and avoiding such high spatial frequencies defects. The proposed original process for thinning, smoothing and polishing a large (1.1m) thin (2mm) shell has been modelled using finite elements method. The feasibility of this process is demonstrated. Results in terms of load optimization, evolution of stresses and constraints within the shell and expected surface optical quality are presented.
More and more complex telescopes and astronomical instruments require: (1) Mechanics with low diffusion/reflection properties in order to decrease the level of scattered light, especially for use in infrared. (2) Mirrors with high reflectivities, in order to improve the level of useful light and/or extend the useful spectrum, especially to the near UV(320 nm - 400 nm), SESO will present simultaneously here some results of its current developments concerning: (1) Solutions to increase the signal/noise ratio for systems operating in the infrared and needing a cryogenic cryostat assembly for the detection system, (2) A high efficiency reflective UV-coating.
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