"SAR-Lupe" is a fully diploid SAR satellite reconnaissance system consisting of 5 satellites with the highest spatial
resolution in the world today, as far as known to us. The system was handed over to the end-user in November 2008 and
is successfully working 24 hours per day, 12 months per year, 10 years long.
This paper will present some more details on the SAR-Lupe system, how it came to life, and how it probably will be
continued in Germany.
Since 1974 X-ray optics and optical ground support equipment for various national and international X-ray and EUV- missions have been designed, manufactured, tested and delivered by Carl Zeiss/Oberkochen. The range of X-ray optics includes mirror systems for ASTRO 8, ROSAT and ABRIXAS, as well as mandrels for SAX, JET-X, WFXT, XMM, Constellation-X and XEUS. An example for high quality EUV- systems is the Wolter II mirror system for SOHO-CDS. We will give a retrospect to previous programs, report about recently performed and finished X-ray optics, as well as we will give an outlook for future contributions.
The image quality degradation due to atmospheric turbulence is one of the main limitations for imaging, laser propagation, and communication through the atmosphere. Adaptive optics is a technology to overcome these problems by real-time phase compensation. The main components for such systems, like wavefront correctors, wavefront sensors, and dedicated computers, are existing, and complete systems have been successfully tested. This article describes the principles of adaptive optics and concentrates on its applications to astronomical imaging, including some first observing results. The performance in image quality which can be expected from adaptive optics and the requirements for its application are discussed.
The image quality degradation due to atmospheric turbulence is one of the main limitations for imaging, laser
propagation, and communication through the atmosphere. Adaptive optics is a technology to overcome these problems by
real-time phase compensation. The main components for such systems, like wavefront correctors, wavefront sensors, and
dedicated computers are existing and complete systems have been successfully tested. This article describes the principles of
adaptive optics and concentrates on its applications to astronomical imaging, including some first observing results. The
performance in image quality which can be expected from adaptive optics and the requirements for its application are
discussed.
The image quality degradation due to atmospheric turbulence is one of the main limitations for imaging, laser propagation, communication, and metrology in the atmosphere. Adaptive optics is a technology to overcome these problems by real-time phase compensation. the main components exist for systems such as wavefront correctors, wavefront sensors, and dedicated computers, and have been successfully tested. This article describes the principles of adaptive optics and demonstrates the potential of adaptive optics for applications in astronomical imaging, including some first results. The image quality that can be expected from adaptive optics and requirements for its application are discussed.
An investigation is underway regarding the usefulness of altazimuth-mounting telescopes' incorporation of laser gyros for pointing and fiber gyros with extremely small random-walk coefficient for telescope inertial stabilization during tracking. A star tracker is expected to help stabilize long-term gyro bias. Gyro and telescope specifications have been derived by means of computer simulations and systems analyses.
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.
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 latest developments of active optics of the ESO NTT include the reduction of friction in the lateral supports of
the primary mirror and in the positioning system of the secondary mirror. The most important remaining problem
is the local air condition. The implications for the ESO VLT and the latest developments in the design of its active
optics are discussed.
Adaptive optics is one of the main features of the Very Large Telescope (VLT) of the European Southern Observatory (ESO) - an array of four 8 meter telescopes. These telescopes can be operated individually, in an incoherent and in a coherent interferometric beam combination mode. Each telescope will be equipped with adaptive optics systems for real-time correction of atmospheric turbulence effects. First results with a prototype system developed for the VLT demonstrated the feasibility and the significant gain of this technology for astronomical imaging. This paper describes the VLT adaptive optics system and its implementation program.
For the first time in ground-based astronomy, diffraction-limited imaging through atmospheric
turbulence has been achieved in real time by adaptive optics in the infrared wavelengths range.
This paper presents the first results and a short analysis, which demonstrate the considerable gain
in resolution and sensitivity by the application of this technique. Single stars, close binary stars,
and a satellite have been resolved. In one cases an other star several arcseconds apart has been
used as reference for the wavefront sensing.
Pros and cons of Michelson and Fizeau type interferometer configurations are compared for systems in space having baselines in the 5 to 100 meter range, when a large field of view is requested for off-axis tracking. The size of the coherent field-of-view is larger in a Fizeau type interferometer but the tolerances required by wide field operation are easier to achieve in the Michelson type. Furthermore, aberration compensation, which calls for more than three optical elements per beam to assure that the beams overlap in the Fizeau field of view, makes it necessary to split the on and off-axis fields before the f/250 final combination plane in both cases. Two categories of configurations are defined: for baselines B less than 10 meters, a Fizeau type is preferable; conversely a Michelson type should be adopted when B is greater than 10 meters. After summarizing the difficulties to overcome in each type, a solution for each type in space environment is proposed.
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).
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 Very Large Telescope (VLT) presently being developed at ESO is described in terms of technological advances which make its use both technically effective and feasible. The VLT capitalizes on advances in materials, polishing techniques, and mirror support systems. The VLT consists of four 8-m alt-az telescopes and a 2-m auxiliary telescope in a single-dish configuration with Zerodur meniscus mirrors passively supported on a lateral system. A discussion of the tradeoffs between glass and metal mirrors is presented, and computerized polishing is described in relation to optical specifications. The mirror is supported with 150 axial and 60 lateral supports with electromechanical actuators to modulate applied force. The active optics concept is employed via the flexibility of the primary mirror, which generates elastomechanical deformations and the position and orientation of the secondary mirror.
Observational results obtained at a 1.52-m telescope in the near-infrared wavelength range of 1.6-5 micron with the use of an adaptive-optics prototype system are reviewed. The purpose of the experiment is to evaluate the correction performance of adaptive optics under actual turbulence conditions at an astronomical site. The observations demonstrate that the full gain in resolution can be obtained. A significant gain in sensitivity is observed, and it is shown that a considerable improvement in signal-to-noise ratio can be achieved due to the bright maximum of sharpened images in all cases where the signal-to-noise ratio is set by background or detector noise.
The Very Large Telescope Interferometer (VLTI) is one of the operating modes of the VLT. In addition to consisting of the four stationary 8-meter-diameter telescopes, it includes a number of movable Auxiliary Telescopes which both complement the (u,v) plane coverage of the large telescopes and provide a powerful interferometric facility by itself (available 100 percent of the time). The current plans for the implementation of the VLTI are described. These plans will be finalized after the choice of the VLT site in 1990.
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.
Up to now telescope optics were usually specified in terms of geometrical errors which cannot be linked to the actual performance under atmospheric turbulence limitation. A more realistic approach is proposed which takes into account atmospheric seeing and diffraction. The main advantage of the method is that at the same time it describes the final performance of the telescope, and gives to the optical manufacturer the maximum freedom to define and possibly modify its own manufacturing error budget.
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