More than 20 years have already passed since the first light of Antu, the Very Large Telescope (VLT) Unit 1 at Paranal Observatory on 25th of May 1998. Encoders are key parts of the control of axes like Altitude, Azimuth, Adapters and Rotators in all the telescopes, where absolute encoders are used to get an accurate measurement of the position, at the level of micrometer. The intention of this document is to summarize and show some problems we had in these years, some modifications and suggestion to improve the design in order to avoid those problems. We also present some new applications of encoders to measure speed instead of position. A typical problem in the Adapters is analyzed, given that the encoder tape is located too close to the bearing it easily gets dirty, forcing our Maintenance Support and Engineering Department (MSE) to dismount the attached instrument and the whole Adapter Rotator getting access to clean its encoder system, with the consequent risk of losing operation time. Same issue is shown in Auxiliary telescopes, GRAAL Co-rotator and the European antenna in ALMA. All the encoder heads in the Adapters and Rotators were modified to avoid damage in the encoder tape, a change of a damaged tape was needed in 2005 and was done for the first time at ESO. A new design of the encoder head support is shown for both Altitude and Azimuth, which provides a fine and accurate way to adjust them. They have been installed in UT4 Azimuth and UT3 Altitude axes. A new design for Azimuth encoder tape is suggested to improve its robustness against variations of height in the hydraulic bearing system. Preventive, Condition-based, Corrective, and “Predictive” Maintenance applied to encoder systems are commented. The Obsolescence is analyzed. And a special case related with Calibration of encoders is also discussed. The integration of encoder signals to the axes plays a pivotal role in the deployment of a cutting-edge control system for the primary axes, Altitude and Azimuth. These encoders not only accurately gauge position but also serve to measure velocity during the encoder initialization phase and provide high-precision commutation information for the power amplifiers. This further enhances precision and efficiency.
The operations at the Paranal Observatory have hit their 25th year milestone for the Unit Telescope 1 that saw first light in 1998. We will review different technical and organizational aspects of the technical operations over the last years. First, we present an update on the reliability and availability of the observatory systems and in particular the scientific instruments over the last decade. Corrective maintenance metrics will be presented to show the trends and compare with previous similar studies. Second, we present a review of our current maintenance processes after an analysis started recently for planning the future integrated operations with the Extremely Large telescope (ELT). The exercise revealed how the resources are used as well as the gaps and potential for improvements, in particular in the context of our methodology of Maintenance in Conditions of Operation (MCO), which we implemented in 2014. Finally, we will give an update on obsolescence management by describing some of the solutions we have implemented, and our strategy and forecast for the future decades given the aging of the Observatory and the need to keep the Very Large Telescope (VLT) competitive in the era of ELT.
The GRAVITY+ project includes the upgrade of the Very Large Telescope Interferometer infrastructure and of the instrument GRAVITY to improve sky coverage, high contrast capabilities, and faint science. The improved sky coverage is obtained via the implementation of one Laser Guide Star (LGS) on each Unit Telescope (UT). This first requires an upgrade of the infrastructure of each of the UTs, which was made over 18 months in 2022 and 2023. The addition of the LGS system requires the implementation of multiple components on several areas of the telescope. These areas include the top ring, the centerpiece, a new platform under the Nasmyth platform, and in the basement. The system includes pointing and aircraft avoidance cameras, the laser projector, laser and electronics cabinets, a heat exchanger, and pumps. As none of the UTs were developed with the infrastructure needed to carry such a system, the same upgrade is made for each of the three UTs. This upgrade consists of a full adaptation of the centerpiece, an upgrade of one of the altitude cable wraps, the installation of a platform under the Nasmyth platform, and the implementation of a cooling circuit running from the basement to the new sub-Nasmyth platform via the azimuth cable wrap. This upgrade requires two missions per telescope, for a total of 30 nights out of operation per telescope. The centerpiece activity also requires the removal of the M1 mirror and cell. The activities were therefore coordinated with the regular recoating of the M1 to minimize the number of nights out of operation. The upgrade required approximately 7.5 staff years of work and 36 missions from Europe to Chile, with around 60 people participating in at least one of the seven missions.
Following the arrival of MATISSE, the second-generation of VLTI instrumentation is now complete and was simultaneously enhanced by a major facility upgrade including the NAOMI Adaptive Optics on the Auxiliary Telescopes. On the Unit Telescopes, significant efforts were also made to improve the injection stability into VLTI instruments. On top of GRAVITY's own evolution, its fringe tracker is now being used to allow coherent integrations on MATISSE (the so-called GRA4MAT project). Meanwhile, operations also evolved to be more flexible and make the most of an extended observing parameter space. In this context, we present an overview of the current VLTI performances. Finally, we will report on on-going improvements such as the extension of the longest baselines.
After 20 years of operations, the Paranal Observatory has accumulated some experience with maintenance of systems, and has lately adopted the methodology called ‘Maintien en Condition Operationnelle’ (MCO). We will describe and review the practical implementation of this strategy, the tools used, the benefits and challenges as well as practical examples and how it is overall managed. The approach is also a benchmarking exercise for operation of the ESO-ELT in the future.
The near-infrared GRAVITY instrument has become a fully operational spectro-imager, while expanding its capability to support astrometry of the key Galactic Centre science. The mid-infrared MATISSE instrument has just arrived on Paranal and is starting its commissioning phase. NAOMI, the new adaptive optics for the Auxiliary Telescopes, is about to leave Europe for an installation in the fall of 2018. Meanwhile, the interferometer infrastructure has continuously improved in performance, in term of transmission and vibrations, when used with both the Unit Telescopes and Auxiliary Telescopes. These are the highlights of the last two years of the VLTI 2nd generation upgrade started in 2015.
ESO is undertaking a large upgrade of the infrastructure on Cerro Paranal in order to integrate the 2nd generation of interferometric instruments Gravity and MATISSE, and increase its performance. This upgrade started mid 2014 with the construction of a service station for the Auxiliary Telescopes and will end with the implementation of the adaptive optics system for the Auxiliary telescope (NAOMI) in 2018. This upgrade has an impact on the infrastructure of the VLTI, as well as its sub-systems and scientific instruments.
More than 10 years have already passed since the first Multiple Application Curvature Adaptive Optics (MACAO) facilities got the first light in UT2 the 18th of April, 2003, in the Very Large Telescope (VLT) at Paranal Observatory.
The achievable image sharpness of a ground-based telescope is normally limited by the effect of atmospheric turbulence. However, with Adaptive Optics (AO) techniques, this major drawback can be overcome so that the telescope produces images that are as sharp as theoretically possible, i.e., as if they were taken from space. [1]
The intention of this document is summarize in few pages some highlights related with the activities needed to keep MACAO units in operation. Some statistics of problems based in Action Remedy tool is included, showing how through these years the number of problems has been reduced, even when there are still some unsolved ones. Some lessons have been learned and there are others one to learn. Corrective and predictive maintenance performed are shown too like the current measurements, transfer functions measurements, thermography pictures, health checks measuring interaction matrix and flat vectors to detect dead APDs or short circuits in the DM, etc. Some forced interventions are included as well like the removal of the cabinets from Coude rooms to avoid that acoustic noise and vibrations perturb the operations, the deformable mirrors reached by cooling leaks and a mirror that got rusty are shown too.
Well knowledge of the system, good interaction between different disciplines groups to perform corrective and preventive maintenance seems to be key aspects of keeping it under control and operative during all these years leading to this good result.
As part of the preparation for the arrival of the MUSE instrument to the VLT, it was required to adapt the hosting
telescope (UT4) guide probe, to increase its back focal length. This is to allow enough space for the later deployment of
the MUSE Adaptive Optics module GALACSI, in-between the telescope adapter rotator and the instrument itself. The
UT guide probe is a critical component for the successful operation of the telescope, so its modification to increase the
telescope’s back focal length, while maintaining full compatibility with the existing operation model and other hardware,
was rather demanding.
The design, manufacture, assembly and test for the new supporting arm in the UT guiding probe is presented. It mixes
the use of novel materials (HB-CESIC® for the mirrors substrates) and state of the art manufacturing techniques (3D
printing mould production and rapid casting for the support structure), which allow producing easily a high performance
subsystem. Characterization of the system prior delivery to the telescope, its integration in the UT and results after
commissioning is presented. Its successful implementation has validated new manufacturing techniques that may prove
very useful for future instruments development.
More than 11 years have passed, since the first of the four Unit Telescopes of the VLT on Cerro Paranal has entered into
operations. To keep four such complex telecopes at a high level of availability with only around 3 percent of technical
down time does not only depend on a good and robust design and manufacturing process, but long term also on a sound
preventive maintenance plan and program.
In this paper the Instrument Adapter-Rotators, twelve of which are installed at the observatory, have been chosen to
show how a preventive maintenance plan has been developed, implemented and executed and what the results are.
In the first part the most common problems are shown and some larger interventions are described and listed. It explains
the tests that have been developed to follow the status of the systems by measuring key parameters such as position
error, motor current, torque and encoders status in order to detect at an early stage any degradation in performance
parameters.
Depending on the test results preventive actions can be planned well ahead of serious failures, making optimum use of
scheduled technical time periods and consequently reducing loss of observing time.
Finally some statistic charts show how problems have been reduced as a result of the preventive maintenance plan
We report on observations with MACAO-VLTI to feed the VLT Interferometer in November 2003. The purpose of this observing run was to optimize the feed to the VLTI by varying certain parameters of the curvature AO system and of the interferometer instrument VINCI. All along the main concern about this instrument combination was the differential piston introduced by 2 independent AO systems. A special so-called “piston removal algorithm” has been developed especially for this purpose. Each DM Influence Function is carefully characterized and a pure piston mode is defined to compensate piston over the pupil produced by a given voltage set. Piston is reduced by ~20 using this algorithm. It was found that decreasing the system main gain, while reducing strehl ratio, also reduces high frequency vibrations on the DM and therefore OPD variations. A control frequency of 420 Hz instead of the nominal 350 Hz was found to improve substantially the coupling by reducing the excitation of the DM resonance (~700Hz). On bright stars, an improvement of a factor of 30 in the flux injection into the VINCI fibers was measured. Following these tests a successful observation of the active nucleus of NGC 1068 was performed leading to a visibility of 40.4±5.4% on an average baseline of 45.84 m. The K magnitude in the 60 mas central source is 9.2±0.4. The results already put some interesting constraints on the inner torus and central engine of the nucleus of NGC 1068 but mostly show that the combination MACAO-VLTI and VINCI opens the realm of extragalactic astronomy to interferometry.
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