One of the most ambitious goals of modern astronomy is to uncover signs of extraterrestrial biological activity, primarily achieved through spectroscopic analysis of light emitted by exoplanets to identify specific atmospheric molecules. Most exoplanets are indirectly identified through techniques like transit or Doppler shift of the host star's flux. Long-term surveys have yielded statistical insights into the occurrence rates of different planet types based on factors such as radius/mass, orbital period, and the spectral type of the host star. Initial estimates of terrestrial planets within the habitable zone have also emerged. However, the difficulty of detecting light from these exoplanets leaves much unknown about their nature, formation, and evolution. As the number of rocky exoplanets around nearby stars rises, questions about their atmospheric composition, evolutionary trajectory, and habitability increase. Direct measurement of an exoplanet's atmospheric composition through its spectral signature in the infrared can provide answers. Measuring the infrared spectrum of these planets poses significant challenges due to the star/planet contrast and very small angular separation from their host stars. Previous research showed that space-based telescopes are mandatory, and unless large primary mirrors (>30m in diameter) can be sent into space, interferometric techniques become essential. Combining light from distant telescopes with interferometric techniques allows access to information at minimal angular separation, operating within the diffraction limit of individual telescopes. Successful demonstrations of on-ground nulling interferometry open a new era for such space-based missions. They are vital to sidestep and tackle these scientific questions. We recently initiated a new study with the European Space Agency to explore the design parameters and the performances related to an interferometric concept based on a single spacecraft and sparse multiple sub-apertures. Launch constraints are linked to the use of an Ariane 6 launch vehicle. Our parametric study covers a range of 1-4m for the diameter of the telescope and a 10-60m baseline. The most promising concept working in the infrared range (3-20μm) will be highlighted. This study is conducted by TUDelft in cooperation with KULeuven, CSL/ULiège, and Amos with the support of the European Space Agency.
KEYWORDS: Equipment, Calibration, Short wave infrared radiation, Design and modelling, Signal to noise ratio, Modulation transfer functions, Thermography, Tunable filters, Optical filters, Telescopes
The Land Surface Temperature Monitoring (LSTM), part of the expansion missions of the Copernicus programme, aims at providing data for land surface temperature and evapotranspiration at unprecedented spatio-temporal resolution, with the main objective of providing valuable data for improved water management at individual European field scale. This paper gives an overview of the instrument main requirements flowing down from the mission objectives, and the instrument design selected to fulfill them. The technical challenges are described as well as the key performances.
KEYWORDS: Equipment, Signal to noise ratio, Calibration, Short wave infrared radiation, Modulation transfer functions, Design and modelling, Astronomical imaging, Thermography, Tunable filters, Telescopes
The Land Surface Temperature Monitoring (LSTM), part of the expansion missions of the Copernicus programme, aims at providing data for land surface temperature and evapotranspiration at unprecedented spatio-temporal resolution, with the main objective of providing valuable data for improved water management at individual European field scale. This paper gives an overview of the instrument main requirements flowing down from the mission objectives, and the instrument design selected to fulfill them. The technical challenges are described as well as the preliminary predicted performances.
Additional presentation content can be accessed on the supplemental content page.
Due to the continuous trend towards higher resolution, future large optical missions for both Astronomy and Earth Observation (telescopes, interferometry,...) are facing new challenges in terms of enabling technologies fighting adverse effects linked to the payload size (manufacturing issues, alignment and integration, in-orbit effects,...). We present here an updated overview of our R&D activities in this field as well as perspectives on the way-forward to technological maturity and implementation within future ESA mission concepts.
We present our latest results on a refined unimorph deformable mirror which was developed in the frame of the ESA GSTP activity ”Enabling Technologies for Piezo-Based Deformable Mirrors in Active Optics Correction Chains”. The identified baseline concept with the soft piezoceramic material PIC151 successfully sustained all vibration requirements (17.8 gRMS random and 20 g sine) and shock testing (300 g SRS). We cover the mirror design development which reduces the stress in the brittle piezo-ceramic by 90% compared to the design from a former GSTP activity. We briefly address the optical characterization of the deformable mirror, namely the achieved Zernike amplitudes as well as the unpowered surface deformation (1.7 μm) and active flattening (12.3 nmRMS). The mirror produces low-order Zernike modes with a stroke of several tens of micrometer over a correction aperture of 50 mm, which makes the mirror a versatile tool for space telescopes.
This paper presents the results of the technology development project “Enabling Technologies for Piezo-Based Deformable Mirrors in Active Optics Correction Chains” conducted by OHB System AG together with its partner Münster University of Applied Sciences (MUAS). The project was funded by ESA within their General Support Technology Programme (GSTP). We address in this paper mainly the definition, flow-down and verification of the requirements for the Deformable Mirror (DM). The requirements were derived from a set of real space mission applications. The deformation of the mirror is performed by piezo-ceramic actuators in an unimorph configuration. The finally developed DM is able produce Zernike modes with a stroke of several tens of μm over a clear optical aperture of 50 mm in diameter. It underwent successfully a full environmental qualification campaign including thermal cycling, shock- and vibration testing, as well as exposure to proton and γ–ray radiation. Thermal and performance tests were performed in the temperature range from 100 K to 300 K. Furthermore, the DM sustained all vibration (random 17.8 g RMS and sinus) and shock (300 g) testing. Thereby all criticalities which were identified a previous study have been overcome successfully. A Technology Readiness Level (TRL) of 5 is reached, as the component has been validated in relevant environment. Based on the high level of maturity, this deformable mirror is now ready for the incorporation in future flight instruments. The achieved TRL of 5 is sufficient for the status of a PDR at payload level and gives thus a very good basis for all kinds of potential B2, C/D payload developments.
S. Fray, J. Hofmann, Alessandro Boni, T. Deuschle, C. Küchel, U. Förster, J. Plumhof, M. Gerstmeier, G. Bambina, G. Petitjean, J. Ouaknine, J. Durand, P. Hallibert
The Flexible Combined Imager (FCI), main instrument of the Meteosat Third Generation Imager (MTG-I) satellite, will image the on-Earth instrument swath with high image quality and highly stable line of sight. It is composed by a Three Mirror Anastigmatic (TMA) telescope assembly, followed by a Spectral Separation and Detection Assembly (SSDA) which has the function to separate the different spectral channels and focus them onto the detector. The Telescope assembly, developed by OHB System AG in Oberpfaffenhofen, will be the subject of this article, presenting first its optical design concept and its main characteristics. Thereafter, the FCI Telescope Assembly (FCI-TA) alignment will be presented, followed by the full test campaign accomplished to characterize the full optical performance of the FCI-TA. The telescope optical design is based on an off-axis field TMA telescope. It is composed by three aspheric off-axis mirrors, having a focal length of 1650 mm, an F/# of 5.5 and an entrance pupil diameter of 302 mm. A fourth, folding, mirror deflects the beam onto the TA focal plane, while in front of the first TMA mirror there is a Scan mirror, in order to let the telescope scan the whole Earth disc. In mid-2019 OHB ended the alignment of this first flight model of FCI-TA. We will show in this article the good results in terms of optical performance obtained from that alignment with a worst WFE of 63 nm and a LOS error of 7.8 arcsec.
The field of earth observation requires increasingly complex optical instruments to meet the final requirements . The anticipation of instrument integration and alignment activities on the subsystem side is essential. Thales SESO manufactures opto-mechanical subsystems assembled in such different space instruments. The evolution of instruments, as TMA type, concerning the reduction of the space allocated requires Thales SESO to offer opto-mechanical components and associated measurements that are increasingly precise and reliable. The challenge here for Thales SESO is to manufacture, integrate and measure off-axis mirrors while ensuring accurate apex positioning. We will share here the results on the instrument of the MTG program for Telescope Optics subsystems of the two instruments FCI and IRS. Through a specific metrology scheme, including accurate scanning of the optical surface Thales SESO delivers to the customer a reliable and accurate location of the optical reference frame of each sub - assembly toward its mechanical reference frame. From these relative location, the customer is able, in its assembly process, to “plug” the sub-assembly directly in its nominal position to start the alignment process with interferometric system. The data transmitted by Thales SESO made it possible to anticipate each adjustment of the optical subsystems and to make a very accurate prediction of the alignment requirement. With the data measures by Thales SESO, our customers realize a very quick final alignment procedure, with minimum displacements, to meet the final goal. In this process, the alignment budget is also minimized, leading to a final WFE largely under the predictions made by the customer before receiving the assemblies.
This paper describes the outcomes of a study funded by the European Space Agency aimed at identifying the technical challenges and trade-offs at the system level, performing preliminary designs of an active correction loop for large deployable telescopes, and defining technological roadmaps for the development of the active correction loop for the selected designs. This study has targeted two very different application cases, one for High Resolution Earth Observation from Geostationary orbit (called GeoHR, with a 4m diameter entrance pupil) and one for Science missions requiring very large telescopes (with a up to 18 m diameter entrance pupil) with high-contrast imaging capabilities for exo-Earth observations and characterization. For both application cases, this paper first summarizes the mission objectives and constraints that have influence on the telescope designs. It then presents the high-level trade-offs that have been led and the optical and mechanical design that have been developed, including the deployable aspects. Finally, the performance assessment is presented, and is the basis for the justification of an active optics correction chain, with a preliminary set of requirements for typical components of the system. The presentation is concluded with proposed technological roadmaps that aim to allow the development of the building blocks on which the next generation instruments will be able to rely on.
This paper presents an overview of an optical instrument for disaster and security monitoring from the geostationary orbit. The described instrument is the payload of the GEOBS (GEOstationary OBServatory) concept, which is the result of an ESA exploratory activity conducted at the ESA-ESTEC Concurrent Design Facility (CDF) in early 2020 in order to assess the technical and programmatic feasibility of optical mission concepts from GEO. Recent improvements in the maturity of critical technologies (e.g. adaptive optics, large CMOS detector arrays, ultra-stable materials,…), together with the development of adequate manufacturing facilities and the required manufacturing techniques in Europe and Japan, have provided the ground for further investigation of the current technical and programmatic feasibility of a geostationary observation system for disaster and security monitoring. The instrument on-board the GEOBS satellite provides medium spatial resolution imagery (10-20 m Ground Sampling Distance at equator) in three visible narrow bands (Red, Green and Blue - RGB), one Panchromatic band and one band in the Near Infrared (NIR). The instrument acquires images using a step-and-stare observation technique, enabling persistent monitoring of selected areas. The instrument is sized to provide a footprint >100 km at Equator and observe the area from 30° to 55° North in Latitude and from 10° West to 36° East in Longitude, with observations possible from 4:00 a.m. to 8 p.m. local solar time. The instrument architecture is based on a Korsch telescope, with an active optics correction loop (wavefront sensor, deformable mirror, 5 degrees-of-freedom mechanism on the secondary mirror), and a focal plane based on multiple CMOS detectors, assembled in either 1D or 2D large arrays to cover the full field of view. The instrument concept also includes ultra-stable structures and light-weight sun-shields to reduce straylight and thermos-elastic effect.
Arnaud Lecuyot, Charlotte Pachot, Pascal Hallibert, H. Oetjen, Francois Laurent, Bruno Napierala, Louis Moreau, Gaetan Perron, M. Lekouara, K. Holmlund
This paper presents the Arctic and Nordic Imager as a concept investigated by the European Space Agency (ESA) and the European Organisation for the Exploitation of Meteorological Satellites (EUMETSAT). The concept addresses a recognized gap in the near-real-time coverage at high latitudes (above 55 degrees) from geostationary satellites, due to viewing geometry over polar areas. The paper recalls the context, summarises the requirements customized for it, describes the main trades, features and sizing parameters of the mission and sensor, and illustrates potential implementations. The requirements are similar to those of geostationary systems. They call for near-real-time multispectral optical observations in the Visible, Near Infrared, Short Wave Infrared, Water Vapour, and Thermal Infrared bands, at moderate spatial resolution. The mission profile proposed uses Highly Elliptical Orbits (HEO). The sensor concept is largely derived from GEO imagers in operation or in development, due to very similar requirements. In the current instrument concepts, the area of interest is covered using a scanning mirror in two directions. A telescope and complementing optics then redirect the optical beam to focal plane assemblies and optical detectors. The instrument also includes calibration subsystems and all necessary equipment i.e. cryocoolers for infrared detectors and electronics for data handling. The major trades are to do with meeting the very demanding optical performance, and to a lesser degree with the radiometric one. These include aperture sizing, definition of scanning law and principle, telescope concept, cryostat design, and image registration. The resulting concepts yield state-of-the-art large space optical instruments.
The current trend for higher resolution and sensitivity for Astronomy and Earth Observation space missions is leading to larger entrance apertures for future optical payloads, often requiring challenging and ultra-stable optical performances driving the instrument design and implementation. The level of complexity for such large systems requires a multidisciplinary approach and technological developments in cross-sectorial areas such as optics, structures, pointing accuracy, control, mechanisms… We present here a range of ESA R&D developments related to future large ultra-stable optical instrument architectures, providing perspectives on the identification of enabling technologies in view of current and future optical missions as well as and a wayforward to maturity for implementation within potential future missions.
The current quest for higher resolution and sensitivity for Astronomy and Earth Observation space missions is leading to larger entrance apertures for future optical payloads, resulting in new technological challenges in terms of optomechanical manufacturing, integration and testing. Ensuring feasibility and minimizing schedule impact of tight manufacturing and integration constraints or mitigating adverse in-orbit effects, Active Optics encompasses a range of enabling technologies for future large optical space instruments.
We present here an updated status overview of our current R and D activities in Active Optics, ranging from deformable space-compatible components to full correction chains. Finally we will share our perspectives on the way-forward to reaching technological maturity and ensuring implementation within future large optical missions.
Meteosat Third Generation is the next ESA Program of Earth Observation dedicated to provide Europe with an operational satellite system able to support accurate prediction of meteorological phenomena until the late 2030s. The satellites will be operating from the Geostationary orbit using a 3 axes stabilized platform. The main instrument is called the Flexible Combined Imager (FCI), currently under development by Thales Alenia Space France. It will continue the successful operation of the Spinning Enhanced Visible and Infrared Imager (SEVIRI) on Meteosat Second Generation (MSG) with improved performance.
This instrument will provide full images of the Earth every 10 minutes in 16 spectral channels between 0.44 and 13.3 μm. The ground resolution is ranging from 0.5 km to 2 km. The FCI is composed of a telescope developed by Kayser-Threde, which includes a Scan mirror for the full Earth coverage, and a calibration mechanism with an embedded black body dedicated to accurate in-flight IR radiometric calibration. The image produced by the telescope is split into several spectral groups by a spectral separation assembly (SSA) thanks to dichroïc beamsplitters. The output beams are collimated to ease the instrument integration before reaching the cryostat. Inside, the cold optics (CO-I) focalize the optical beams onto the IR detectors. The cold optics and IR detectors are accurately positioned inside a common cold plate to improve registration between spectral channels. Spectral filters are integrated on top of the detectors in order to achieve the required spectral selection.
This article describes the FCI optical design and performances. We will focus on the image quality needs, the high line-of-sight stability required, the spectral transmittance performance, and the stray-light rejection. The FCI currently under development will exhibit a significant improvement of performances with respect to MSG.
In recent years, a trend for higher resolution has increased the entrance apertures of future optical payloads for both Astronomy and Earth Observation most demanding applications, resulting in new opto-mechanical challenges for future systems based on either monolithic or segmented large primary mirrors. Whether easing feasibility and schedule impact of tight manufacturing and integration constraints or correcting mission-critical in-orbit and commissioning effects, Active Optics constitutes an enabling technology for future large optical space instruments at ESA and needs to reach the necessary maturity in time for future mission selection and implementation. We present here a complete updated overview of our current R and D activities in this field, ranging from deformable space-compatible components to full correction chains including wavefront sensing as well as control and correction algorithms. We share as well our perspectives on the way-forward to technological maturity and implementation within future missions.
KEYWORDS: Space telescopes, Wavefront sensors, Mirrors, Active optics, Deformable mirrors, Telescopes, Actuators, Wavefronts, James Webb Space Telescope, Infrared telescopes
The next generation of UVOIR space telescopes will be required to provide excellent wavefront control despite
perturbations due to thermal changes, gravity release and vibrations. The STOIC project is a response to an ESA
Invitation to Tender to develop an active optics correction chain for future space telescopes. The baseline space telescope
being considered is a two-mirror, 4m telescope with a monolithic primary mirror – we refer to this concept as Hypatia.
The primary mirror diameter could be extended, but is limited in the near future by launch vehicle dimensions. A
deformable mirror (pupil diameter 110mm) will be an integral part of the telescope design; it is being designed for high
precision and the ability to maintain a stable form over long periods of time. The secondary mirror of the telescope will
be activated to control tip-tilt, defocus and alignment with the primary. Wavefront sensing will be based on phase
diversity and a dedicated Shack-Hartmann wavefront sensor.
The project will develop a laboratory prototype to demonstrate key aspects of the active correction chain. We present the
current state of the preliminary design for both the Hypatia space telescope and the laboratory breadboard.
An increasing need for higher resolution for both Science and Earth Observation applications demands a bigger entrance aperture of future optical payloads, leading to large primary mirrors, either monolithic or deployable. Correcting issues linked to manufacturing, integration, launch and use of large light-weighted optics (and associated structures), Active Optics constitutes an enabling technology for future large space instruments. This paper presents the current status of technological developments at ESA in this very promising field.
The Meteosat Third Generation (MTG) Programme is being realised through the well-established and successful cooperation between EUMETSAT and ESA. It will ensure the continuity with, and enhancement of, operational meteorological and climate data from Geostationary Orbit as currently provided by the Meteosat Second Generation (MSG) system. The industrial Prime Contractor for the Space segment is Thales Alenia Space (France) with a core team consortium including OHB-Bremen (Germany) and OHB-Munich (Germany. This contract includes the provision of six satellites, four Imaging satellites (MTG-I) and two Sounding satellites (MTG-S), which will ensure a total operational life of the MTG system in excess of 20 years. A clear technical baseline has been established for both MTG-I and MTG-S satellites, and confirmed through a rigorous Preliminary Design Review (PDR) process that was formally concluded during 2013. Dedicated reviews have been held for all the main elements including the core instruments (Flexible Combined Imager (FCI) and Infrared Sounder (IRS)), the Platform (which is largely common for the two satellites), the Lightning Imager (LI) and the MTG-I and MTG-S satellites as a whole. The satellites and instruments are at the moment in preparation for the Structural and Thermal Models (STM). The FCI is designed to provide images of the Earth every 10 to 2.5 minutes in 16 spectral channels between 0.44 and 13.3 μm, with a ground resolution ranging from 0.5 km to 2 km. The on-board calibration is based on the use of a Metallic Neutral Density (MND) filter for VIS/NIR channels and a blackbody for the IR channels. This paper introduces the overall FCI design and its calibration concept covering VIS/NIR and IR domains and it describes how the use of the MND makes it possible to accurately correct the medium and long term radiometric drifts of the IR3.8 μm channel.
Active optics for Space is relatively new field that takes advantage of lessons learnt on ground, and together with the
tighter constrains of space environment it allows operation of larger mirrors apertures for space telescopes and better
image quality. Technical developments are crucial to guarantee proper technological readiness for applications on new
missions whose performance can be driven also by these novelties. This paper describes the philosophy pursued at ESA,
providing an overview of the activities run within the Agency, as well as perspectives for new developments. The Optics
Section of the Directorate of Technical and Quality Management of ESA/ESTEC is currently running three projects.
Two examples are here addressed.
KEYWORDS: Mirrors, Telescopes, Space telescopes, Sensors, Sun, Calibration, Near infrared, Signal to noise ratio, Modulation transfer functions, Tolerancing
Meteosat Third Generation is the next ESA Program of Earth Observation dedicated to Nowcasting and very short term Weather Forecasting (NWC), medium/short range Global and Regional Numerical Weather Prediction (NWP), and Climate and Air Composition Monitoring. The satellites will be operating from the Geostationary orbit using a 3 axes stabilized platform. The main instrument is called the Flexible Combined Imager (FCI), currently under development by Thales Alenia Space France (TAS-F). This instrument will provide full images of the Earth every 10 minutes in 16 spectral channels between 0.44 and 13.3 μm, with a ground resolution from 0.5 km to 2 km. The FCI is composed of a TMA telescope developed by Kayser-Threde (KT), which includes a Scan mirror, and a calibration mechanism with an embedded black body dedicated to accurate in-flight IR radiometric calibration and a Metallic Neutral density for dedicated VNIR Sun calibration. The image produced by the telescope is split into several spectral groups by a spectral separation assembly (SSA) with dichroïc beamsplitters. The output beams are collimated to ease the instrument integration, and reach the cold optics (CO-I) which focalize the optical beams onto the detectors. The cold optics and IR detectors are accurately positioned inside a common cryostat to improve registration between spectral channels. Spectral filters are integrated on top of the detectors in order to achieve the required spectral selection. This article will describe the optical design and the main optical performances of the FCI: image quality, very high line-of-sight stability, and an efficient stray-light rejection thanks to the implementation of dedicated baffles and a stringent control of contamination. The FCI currently under development is expected to exhibit a significant improvement of performances with respect to Meteosat Second Generation satellites.
ASSIST: The Adaptive Secondary Setup and Instrument STimulator is the test setup for the verification and calibration
of three elements of the VLT Adaptive Optics Facility.; the Deformable Secondary Mirror (DSM) the AO system for
MUSE and HAWK-I (GALACSI and GRAAL). In the DSM testing mode the DSM will be tested using both
interferometry and fast wave front sensing. In full AO mode, ASSIST will allow testing of the AO systems under
realistic atmospheric conditions and optically equivalent to the conditions on the telescope. ASSIST is nearing its final
design review and in this paper we present the current optical and mechanical design of ASSIST. In this paper we
highlight some of the specific aspects of ASSIST that we are developing for ASSIST.
ASSIST - The Adaptive Secondary Setup and Instrument STimulator is a test setup to verify the operation of three
elements of the VLT Adaptive Optics Facility, namely the Deformable Secondary Mirror (DSM) and the two AO
systems using this DSM, the AO system for the visible light integral field spectrograph MUSE (GALACSI) and the AO
system for the IR wide field imager HAWK-I (GRAAL). To support the testing of these elements, ASSIST will provide
both an interferometry setup for testing the DSM as well as a full atmospheric turbulence simulator and star simulator to
mimic the conditions at the telescope. To test the instruments using the DSM, the output beam is matched the output
beam of the VLT telescope, including the correct exit-pupil and high-quality imaging and a similar hardware interface is
provided. Since one of the modes to be verified is nearly diffraction limited, also the thermal and vibrational stability
are very important, with strong constraints on both the mechanical as well as the optical design.
A comprehensive suite of Adaptive Optics systems and AO-assisted instruments is currently under development for the VLT and will be built around a hyperbolic convex adaptive Deformable Secondary Mirror (DSM). In telescopes with such a secondary mirror, test and calibration of both the DSM and the science instruments using it are notoriously expensive and time-consuming. The Adaptive Secondary Setup and Instrument Stimulator (ASSIST) is being developed to allow test and integration of three key elements of the future VLT Adaptive Telescope Facility: the DSM and 2 instrument-specific adaptive optics systems (GALACSI for MUSE and GRAAL for HAWK-I). The core of ASSIST is a standalone interferometric test setup for the DSM allowing its test at its center of curvature (significantly reducing the size of the classical hyperbole focii test configuration). This setup is completed by a star simulator for both natural and laser guide stars, a turbulence generator (for realistic AO performance measurements), a corrector system generating a VLT-like exit pupil and a Nasmyth rotator simulator interfacing with the two AO systems.
In this paper we present the optical architecture of ASSIST, detailing the current design of the different parts of the system, and discuss its projected performance and compliance with the test and calibration requirements.
The current generation of Adaptive Optics systems has lead to an improvement in resolution and contrast of up to one to two orders of magnitude for 8-10 meter class telescopes. With the upcoming generation of Extremely Large Telescopes, AO has the potential for an even larger gain. But the scaling of the current AO systems to ELTs will not be trivial; both in AO hardware as well as in AO control, techniques need to be developed which can cope with the large number of sub-apertures. The Leiden High Order AO Testbed was developed for the implementation and testing of innovative ELT-compatible AO systems. In the current setup, the system is centered around a Liquid Crystal Spatial Light Modulator, a Shack-Hartmann wavefront sensor and a PC based RTC. Initially, the system will be used to develop and test efficient high-order AO algorithms under laboratory conditions, but is sufficiently flexible to allow for fast replacement of all components for the testing of different hardware components. In this paper we will present the design, building and testing of HORATIO.
In telescopes with a Deformable Secondary Mirror, the testing and calibration of both the DSM itself as well as the instruments using this DSM are expensive and time consuming processes. Especially in telescopes without an intermediate focus before the DSM, a number of calibrations can only be performed on a real star during night time. A full suite of Adaptive Optics systems and AO-assisted instruments is currently under development for the VLT, also know as the VLT Adaptive Telescope. ASSIST was developed to assist in the integration and testing of three elements of the VLT Adaptive Telescope Facility; the DSM; the MUSE AO system 'GALACSI' and the HAWK-I AO system 'GRAAL.' The core of ASSIST is a support infrastructure to integrate the DSM in a compact and stable test setup. A Nasmyth rotator simulator will be provided for attaching the two AO systems, while ASSIST will be fed by a star simulator and turbulence generator for realistic performance measurements of both the DSM as well as the AO system under test. An on-axis high-speed interferometer will be used for additional testing of the functional operation of the DSM. In this paper we present the requirements and design of ASSIST and the projected performance of the test bench for both the testing and calibration of the DSM as well as for the two AO systems under test.
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