Since many years CILAS developed active mirrors for synchrotron radiation beamlines. The paper presents the recent developments of bimorph structures usable for x ray mirrors, monochromator crystals, and gratings. The adaptation of the structure to the 3 applications above mentioned is done by choosing the upperplate material and surface coating. The bimorph structure is designed to produce a simple spherical bending of the active plate, or more sophisticated shapes as ellipsoids or parabola. The bimorph structure can be delivered in a mechanical housing able to properly support it. High voltage amplifiers with digital input fitted to control the shape as well as a curvature measurements system may be delivered providing the possibility of closed loop operation. Standard versions of bimorph mirrors and gratings are available. Most of the development works was done under ESRF support.
The COME-ON+ adaptive optics system was set up on the ESO 3.6-meter telescope for two technical runs (in December 1992 and April 1993) and is now routinely used for astronomical observations. This system is an upgrade of the COME-ON adaptive optics prototype system. During the technical runs, images were recorded in the V, I, J, K and L' spectral bands. Currently, the best resolution obtained is 0.1' in H (1.65 micrometers ) under bad seeing conditions (seeing > 1' and averaged wind speed > 10 m/s) and reference star magnitudes of 6 to 8. The corresponding Strehl ratio is 35%. 70% Strehl ratio was obtained at 2.2 micrometers (K band). At 0.9 micrometers (I band), in the partial correction regime, the resolution is of the order of 0.2' for 0.8' seeing and 10 m/s averaged wind speed. The optimized modal control has been used on faint reference stars. The limiting magnitude (in V band) for wavefront sensing has been measured to 14 and 15 depending on the spectral type of the reference star and the seeing conditions for a low frequency tip-tilt correction.
LASERDOT has acquired a wide experience in Adaptive Optics Systems: components and hardware manufacturing, dedicated software, system integration and maintenance. Associated with several research organizations, it has taken advantage of having installed the first AO systems routinely used by astronomers. This paper presents deformable mirrors as well as tip- tilt mirror designed and achieved at Laserdot jointly with Observatoire de Paris-Meudon. Some comparisons between the different types of deformable mirrors are done.
The problem to be solved is to maintain the best efficiency of an Adaptive Optics System (AOS) during an observing run, versus different seeing conditions and star magnitudes. The paper uses the modal control and partial correction concepts as defined in previous works. It has been demonstrated in these works that the Strehl ratio of images corrected by an AOS can be evaluated by a simple criteria. Such a criteria uses only the temporal covariance of the controls applied to the AO mirror. Using these different results a method to optimize the loop gains is suggested. This method can be applied during real time run of the AOS. It uses the only knowledge of the modal control values applied to the AO mirror and the knowledge of the residual wavefront errors as measured by the wavefront sensor.
Since approximately 5 years, several experimental Adaptive Optics Systems have been tested on different astronomical sites. This paper describes a general purpose AOS designed for new or existing telescopes for diameters ranging from 2 to 4 meters. Investigations on actually available Adaptive Mirrors and Wavefront sensors are made. The use of a bimorph mirror and simplified Shack Hartmann is proposed. Results of simulation to evaluate the Strehl ratios for different wavelengths are given versus seeing conditions and star magnitudes. This leads to the conclusion that low cost, turn key AOS are a new attractive possibility for Astronomy.
Adaptive optics systems have proved their efficiency to obtain high resolution images in he field of large astronomical telescopes. The same technics can be applied to correct X-ray mirror shapes. The paper describes the principle of an adaptive X-ray mirror system (mirror architecture, measurement subassembly, control unit). In a second part, first results obtained during the design study of the ESRF adaptive X-ray mirror are given. The possibility to achieve cylindrical or elliptical mirror surfaces using adaptive optics technics are suggested.
The design of an Adaptive Optics System must take into account at least the following main criterias. First, correction efficiencies versus the atmospherical turbulences, i.e., the Fried diameter and the turbulence power spectrum. Second, sky coverage versus star magnitudes and star classes. To answer these criteria an optimization method is defined. It uses as main parameter the residual mean phase errors of the corrected wavefronts. It is demonstrated that this parameter able us to optimize the System performances: number of modes to be controlled, sampling rates of phase measurements, and noise minimization. Finally an application is done for a 3.6 m class telescope and 2 different adaptive mirror types.
Recent advances in adaptive optics control techniques have demonstrated the interest of modal control in astronomical applications in comparison with a nodal control. This paper describes the advantages to use such a control for the Come-On-Plus project. The different steps of nodal and modal control algorithms used for this experiment are given.
Adaptive optics systems have proven their efficiency for obtaining high resolution images in the field of large astronomical telescopes. The same techniques can be applied to correct x-ray mirror shapes. The paper describes the principle of an adaptive x-ray mirror system (mirror architecture, measurement subassembly, control unit). In the second part, first results obtained during the design study of the ESRF adaptive x-ray mirror are given. The possibility of achieving cylindrical or elliptical mirror surfaces using adaptive optics techniques are suggested.
Over the past two years, laserdot has developed a new machine vision system for obstacle detection by mobile robots. A pulsed laser illuminates the road in a zone from 100 to 150 meters in front of the vehicle and the backscatter is analyzed by a linear array of photodetectors connected to a computer. Each obstacle is detected and its position is determined. The distance is calculated by measuring the pulse time-of-flight, producing a complete three-dimensional image without scanning. The system was jeep-mounted for testing in a military environment at the Angers Technical Center (ETAS) in France. This article describes the laserdot vision system and its design features, as well as the test results from ETAS. The system is capable of providing information on the shape of the road in front of the vehicle, including slope and banking measurements. Lastly, the future integration of the detector in a mobile robot is detailed. These works have been supported by Direction des Recherches, Etudes et Techniques (DRET).
Laserdot has been working on adaptive optics systems for over 15 years. The first applications were about laser beam control. This has led to the first kind of deformable mirrors we use for the correction and dithering of the wavefront. These mirrors may be cooled depending on the laser beam power. Lately, with the participation of different European institutions, this knowledge has been applied to astronomical imaging. The `Come On' project showed how interesting such a technique is. `Come On Plus,' the project to be carried out, will certainly improve these first results. At the same time, jointly with Francois Roddier and for astronomical purposes too, Laserdot has achieved some bimorph mirrors which are to be used with a curvature sensor. This paper aims to oversee the mechanical components which have been designed for these different studies.
This paper is a presentation of the Come-On-Plus adaptive optics system, based on the Come-On
prototype. Come-On-PIus will be set up in 1992 on the ESO 3.6 m telescope in La Silla (Chile). It is an
upgrade of the Come-On instrument, with a 52 actuator deformable mirror, and 30 Hz correction
bandwidth. But the main improvement concerns the wavefront sensing, designed in this instrument for
astronomical applications, with a high detectivity wavefront sensor and a specific mirror control
algorithm. This system is planned for routine astronomical observing as well as providing design
parameters for the adaptive optics system of the ESO Very Large Telescope (VLT).
The optical transfer function (OTF) is examined for an optical instrument corrected by an adaptive optics systems. A model introducing the application of modal control to the OTF and accounting for the effects of time lags and angular depointings is presented. The model allows the estimation of OTF decay in respect to the Fried diameter and for different time lags in an adaptive mirror. Modal control is described and delays in the controls of the adaptive mirror system are discussed.
This paper reports the results of the observations made with the VLT Adaptive Optics Prototype System 'COME-ON' at the ESO 3.6 meter telescope. The analysis of uncorrected and corrected images in the near-IR wavelength range (below 5 microns) leads to a detailed assessment of the system performance in terms of improvement of angular resolution that nearly achieves the ideal diffraction profiles down to 1.7 micron wavelength, as well as a Strehl ratio approaching 0.6-0.8 at 3.8 microns. A resolution of 0.12 arcsec has been obtained with this system at 1.7 microns which is wavelength-dependent on the temporal parameters of the observation. The current limiting magnitude for the reference source is m sub R = 11.5 when applying the full correction capabilities of the system, and m sub R = 13 if only the wavefront tilt is corrected.
An adaptive optical system dedicated to high resolution imaging can be modelized in terms of transfer loops. This model permits one to estimate the response of such a system to time-varying wavefront perturbation. A block diagram describing the closed loop of the adaptive optics of the Come-On project is given and a theoretical expression expressed in terms of the Z transform is found for the case of a nodal approach. In a second step, identification methods are used to determine the best parameter values of these nodal models. Finally, the responses of these models to known perturbations are compared with the experimental data recorded during the Come-On experiments. The same analyses are conducted for modal models. In these two cases, the results are found to be in good agreement.
KEYWORDS: Optical transfer functions, Control systems, Mirrors, Actuators, Signal processing, Performance modeling, Systems modeling, Device simulation, Image processing, Phase measurement
In a preceding paper the authors calculated the mean value of the Optical Transfer Function (OTF) for a high-resolution imaging instrument corrected by adaptive optics. The Come_On experiments carried out during 1990 show good correlation with the mathematical model. In the present paper the model described in the 1987 paper is revised to introduce modal control and take into account the effects of time lags and/or angular depointings on the corrected OTF. These lags represent the time needed to perform the computations between phase measurements and corrections, and the angular depointings define the angular field where the corrections are valuable. The model permits an evaluation of the OTF decay in respect to the Fried diameter. Numerical results are given using the modified model with the Come_On project specifications. These works have been sponsored by the French Defense Ministry through the Direction des Recherches, Etudes et Techniques (DRET).
An adaptive optical system dedicated to high resolution imaging can be modeled in terms of transfer loops. This model permits estimation of the response of such a system to time-varying wavefront perturbation. A block diagram describing an adaptive optic as a closed loop system is given and an analytical expression expressed in Z transform is found. In a second step, identification methods are used; the best estimates for the parameter values of the model are found using as an example the Come_On project data. Finally the responses of the model to known perturbations are compared with the experimental data recorded during the experiments of Come_On; the results are found to be in good agreement.
An adaptive optics system is considered as a multi loops servo system.
The main components of the ioops are:
- the wavefront sensor,
- the real time digital processor,
- the adaptive mirror and the high voltage control amplifiers.
These loops are closed via the wavefront itself.
Generally the detector of the wavefront sensor is a CCD camera. At first, images of
the CCD matrix are digitized and the processor computes the local slopes of the
wavefront ; secondly, the processor performs the calculation needed to output the
values of the controls. Finally data are sended to the adaptive mirror through a
digital/analog converter and the power amplifiers.
A scheme of the loops is given where each major constituent is replaced by its
transfer function. The time lags due to the CCD matrix and calculations are expressed.
Using the Nichols criterion which defines the stability of the loops, the effects of the
sampling rate and time lags on gain and bandwidth are studied. The results of a
numerical model are given and comparisons are made with the COME-ON
experiments.
Same paper has been presented during the SPIE's 1990 Symposium on
Astronomical Telescopes and Instrumentation for the 21St Century in February 1990.
This paper is a presentation of the so-called COME-ON adaptive optics prototype system developed jointly by four
European institutions. This system has been tested on the 1.52m telescope of the Observatoire de Haute Provence on
October 12 to 23 and November 13 to 24, 1989. Diffration-limited infrared imaging has been achieved during these first
tests. The adaptive optics system consists of a 19 actuator deformable mirror and a Hartmann-Shack type wavefront
sensor. In this instrument the wavefront sensing is performed at visible wavelengths while the correction is performed for
near infrared imaging (1 .2 to 5 .tm). Specialized computers drive the deformable mirror and a tip-tilt mirror. The
bandwidth of the servo-loop is 9 Hz at 0 dB point in open-loop. The results obtained with this instrument will be very
useful for the design of the future adaptive optics system for the ESO Very Large Telescope (VLT).
The purpose of the study is to establish the time transfer function of an adaptive-system loop with a CCD camera. Each component of the loop is replaced by its transfer function. The time lags due to the CCD matrix and calculations are determined. The effects of the sampling rate and the time lags on gain and bandwidth are studied by using the Nichols criterion defining the loop stability. It is concluded that the input should be phase perturbations expressed on the basis of the actuator correction shapes, while the output should be the voltage applied at the power amplifiers in order to obtain correction strokes.
This paper is a presentation of the so-called COME-ON adaptive optics prototype system developed jointly by four European institutions. This system has been tested on the 1.52m telescope of the Observatoire de Haute Provence on October 12 to 23 and November 13 to 24, 1989. Diffraction-limited infrared imaging has been achieved during these first tests. The adaptive optics system consists of a 19 actuator deformable mirror and a Hartmann-Shack type wavefront sensor. In this instrument the wavefront sensing is performed at visible wavelengths while the correction is performed for near infrared imaging (1.2 to 5 rim). Specialized computers drive the deformable mirror and a tip-tilt mirror. The bandwidth of the servo-loop is 9 Hz at 0 dB point in open-loop. The results obtained with this instrument will be very useful for the design of the future adaptive optics system for the ESO Very Large Telescope (VLT).
An adaptive optics prototype system has been tested at the 1.52 m telescope of the Observatoire de Haute Provence, resulting in diffraction-limited images at near infrared wavelengths (2.2 to 5 microns). This paper presents the first results and a short analysis, which demonstrate the considerable gain in resolution and sensitivity achieved by this technique. Single stars, close binary stars, and a satellite have been resolved. In some cases another star several arcseconds apart has been used as reference for the wavefront sensing.
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