KEYWORDS: Telescopes, Stars, Matrices, Data modeling, Design, Control systems, Signal filtering, Performance modeling, Detection and tracking algorithms, Error analysis
With the aim of improving the star tracking performance of ground-based telescopes, we deal with the design of model predictive control architecture so as to properly lead their axes while mitigating possible external disturbances affecting the control task. The proposed architecture is composed of two layers, namely, (i) a trajectory generator that determines, based on the astronomic computation, the telescope position and speed references to be tracked while ensuring that all the telescope physical constraints, in terms of speed and acceleration, are never violated; (ii) an model predictive control (MPC) controller that guarantees the optimal tracking of the desired reference behavior by providing the torque inputs for telescope axes for the achievement of star observation task. The control architecture is tailored for the tracking control problem of Telescopio Nazionale Galileo (TNG), located at La Palma (Spain). To this end, by leveraging real data measurements in specific operative scenarios, a 12-order linear system describing the TNG dynamics is identified, via the non-iterative subspace method, for the design of the second layer. Validation results confirm the goodness of the dynamical model in predicting the TNG behavior within the operative range of (80 and 90 deg) altitude position. The effectiveness of the proposed MPC-based control architecture is proven via an ad-hoc virtual testing simulation platform implemented in MATLAB and Simulink and tailored for the identified TNG model. Virtual testing results, involving the real scientific target TYC 1731-916-1, confirm the capability of the proposed solution in ensuring optimal star tracking while mitigating the wind external disturbances forces. Finally, a comparison analysis w.r.t. the state-of-the-art control approaches, i.e., Linear-Quadratic-Gaussian and Proportional-Integrator-Derivative controller, and a robustness analysis w.r.t. the model mismatch between the MPC prediction model and the simulated TNG dynamics are provided to disclose the improved tracking performance achievable via the proposed MPC-based control architecture.
This paper focuses on the designing of tracking control strategies for ground-based telescopes by also comparing model-based solutions with more classical alternatives. Within this framework, we synthesize a double-layer control architecture consisting of: i) a position control layer, which combines a Kalman filter observer and Linear-Quadratic-Gaussian-Proportional-Integral (LQG-PI) controller to compute the appropriate speed profile guaranteeing a reliable tracking of a given telescope position trajectories; ii) a speed control layer, which ensures the optimal tracking of the computed speed profile by driving the torque of the telescope. Moreover, a trapezoidal speed pre-processor is embedded in our control architecture with the aim of computing the appropriate telescope axes position trajectories: this ensures that all the telescope physical constraints, in terms of speed and acceleration, are not always violated. Virtual simulations, carried out via an ad-hoc simulation platform, implemented in Matalb&Simulink and tailored for the specific case study Telescopio Nazionale Galileo (TNG) located at La Palma island, disclose the effectiveness of the hierarchical control architecture for a representative set of star trajectories. Validation phase also considers several realistic conditions and takes into account input disturbance such as the Von-Karman wind disturbance model. Finally, a comparison analysis with a PID-based control architecture is provided to discuss about the advantages and benefits of the proposed optimal control solution.
Telescopio Nazionale Galileo (TNG) has successfully deployed its new Telescope Control System (TCS). This paper focuses on the technical details of the upgrade, highlighting key improvements and showcasing the enhanced functionality and reliability of the new TCS. The development and deployment were carefully planned, incorporating 3D simulations and overlapping with other maintenance operations to minimize the impact on observational time. With new advanced features, such as a modular architecture and the use of a graphical programming language, the TCS enables easy on-the-fly testing of control algorithms for future developments.
MORFEO is a post-focal adaptive optics module that forms part of the first light instrument suite for the Extreme Large Telescope (ELT). The project is now in the Final Design Phase. In this paper, we report the status of the project.
MAVIS passed the Preliminary Design Review in March 2023 and kick started its phase C early June. We are aiming at a Final Design Review in December 2024. I will report on the state of MAVIS design, as well as general project updates, schedule, procurement, risks. We are working on early procurement (Long Lead Item review held on October 2023) as well as on a number of prototype activities I will report on.
VSTPOL is a project to provide a new polarimetric capability to the VST. With its 2.6m primary mirror and 1 degree × 1 degree field of view, the upgrade will make the VST the first large wide field survey telescope with optical polarimetry, filling a specific niche in the astronomical instrumentation landscape. The polarimetric mode will replace the electro-mechanical system that hosts the ADC, which currently sits unused, so that the filter can be accommodated without compromising the ordinary optical configuration. The upgrade requires the design of the mechanical interface to the telescope structure and optics, and the integration of the instrument electronic and software systems. In this paper we present an overview of the approach adopted for the project management and system engineering towards the design of the polarimetric mode addition. In particular, this includes the activities related to the definition of schedule, product and work breakdown structure, deliverables, technical requirements analysis and interfaces.
The Simonyi Survey Telescope (SST) at the Rubin Observatory, is nearing completion. Ensuring precise image quality is essential for fulfilling the observatory’s ambitious scientific goals. To this end, the Active Optics System (AOS) will correct various factors, including gravity-induced aberrations, temperature gradients, and hysteresis. During the commissioning phase, achieving precise alignment of the telescope is critical, particularly given the wide field of view. Small errors can lead to unacceptable off-axis aberrations, especially towards the field’s edge. This paper presents an analysis tool of the impact of these aberrations on the in focus PSF moments as detected in the science field. We introduce a simplified model of the optical system under generic misalignments, designed to quickly calculate the distribution of aberrated PSF across the field. By comparing the results obtained from this model with reference data simulated using accurate ray tracing software, we can assess its accuracy and employ it to infer the state of the optical system. This work will provide an additional aid for the Rubin team during the commissioning activities.
MAVIS is an instrument being built for the ESO’s VLT AOF (Adaptive Optics Facility on UT4 Yepun). MAVIS stands for MCAO Assisted Visible Imager and Spectrograph. It is intended to be installed at the Nasmyth focus of the VLT UT4 and is made of two main parts: an Adaptive Optics (AO) system that cancels the image blurring induced by atmospheric turbulence and its post focal instrumentation, an imager and an IFU spectrograph, both covering the visible part of the light spectrum. The MAVIS project has completed PDR and is currently in the final design stage of development. We present the integrated framework, and the software tool developed the reliability, availability, maintainability, and hazards analysis, examples of RAMS analysis and the impact on the design and development of MAVIS. Additionally, we present how the RAMS framework integrates with MAVIS model-based system engineering and project management frameworks and tools.
MORFEO is the Multi-Conjugate Adaptive Optics Relay for the Extremely Large Telescope (ELT) that will provide multi-conjugate correction of the incoming wavefront by means of three deformable mirrors: one on the telescope and two in the instrument optical train. The wavefront sensing is based on six laser guide stars projected on a constellation of 45 arcseconds and three natural guide stars selected into the 2,7 arcminutes corrected FOV. The current design of the Real Time Computer (RTC) devoted to the deformable mirrors control is reported in the following. According to the ELT architecture, the RTC consists of a Hard Real-Time Core (HRTC) and a Soft Real-Time Cluster (SRTC). The former is in charge of acquiring data from the wavefront sensors and controlling the deformable mirrors and jitter mirrors. It adopts the HEART platform and will be provided by the Herzberg Astronomy and Astrophysics - NRC Canada - which is joining to the Consortium. The SRTC, based on the ESO-provided RTC Toolkit, provides the interface for the Instrument Control System Software. It performs all the supervisory and monitoring tasks, in addition to the auxiliary loops for optimization of correction. This paper will discuss the state of the updated design of the RTC after the Preliminary Design Review (PDR) towards the final design of the subsystem. It will provide an in-depth description of the distributed architecture adopted by the system, with a particular focus on the architecture of the SRTC. Detailed insights into the design considerations, challenges encountered, and solutions implemented in the SRTC architecture will be presented to provide a comprehensive understanding of the system’s current state and future direction. Part of the research activities described in this paper were carried out with contribution of the Next Generation EU funds within the National Recovery and Resilience Plan (PNRR), Mission 4 - Education and Research, Component 2 - From Research to Business (M4C2), Investment Line 3.1 - Strengthening and creation of Research Infrastructures, Project IR0000034 – “STILES - Strengthening the Italian Leadership in ELT and SKA”.
The Instrument Control Software of SOXS (Son Of X-Shooter), the forthcoming spectrograph for the ESO New Technology Telescope at the La Silla Observatory, has reached a mature state of development and is approaching the crucial Preliminary Acceptance in Europe phase. Now that all the subsystems have been integrated in the laboratories of the Padova Astronomical Observatory, the team operates for testing purposes with the whole instrument at both engineering and scientific level. These activities will make use of a set of software peculiarities that will be discussed in this contribution. In particular, we focus on the synoptic panel, the co-rotator system special device, on the Active Flexure Compensation system which controls two separate piezo tip-tilt devices.
We present the advancements in the development of the scheduler for the Son Of X-shooter (SOXS, 1,2) instrument at the ESO-NTT 3.58-m telescope in La Silla, Chile. SOXS is designed as a single-object spectroscopic facility and features a high-efficiency spectrograph with two arms covering the spectral range of 350-2000 nm and a mean resolving power of approximately R=4500. Its primary purpose is to conduct UV-visible and near-infrared follow-up observations of astrophysical transients, drawing from a broad pool of targets accessible through the streaming services of wide-field telescopes, both current and future, as well as high-energy satellites. The instrument is set to cater to various scientific objectives within the astrophysical community, each entailing specific requirements for observation planning, a challenge that the observing scheduler must address. A notable feature of SOXS is that it will operate at the European Southern Observatory (ESO) in La Silla, without the presence of astronomers on the mountain. This poses a unique challenge for the scheduling process, demanding a fully automated algorithm that is autonomously interacting with the appropriate databases and the La Silla Weather API, and is capable of presenting the operator not only with an ordered list of optimal targets (in terms of observing constraints) but also with optimal backups in the event of changing weather conditions. This requirement imposes the necessity for a scheduler with rapid-response capabilities without compromising the optimization process, ensuring the high quality of observations and best use of the time at the telescope. We thus developed a new highly available and scalable architecture, implementing API Restful applications like Docker Containers, API Gateway, and Python-based Flask frameworks. We provide an overview of the current state of the scheduler, which is now ready for the approaching on-site testing during Commissioning phase, along with insights into its web interface and preliminary performance tests.
VSTPOL enhances VST’s capabilities by adding optical polarimetry via a linear polarized filter. This will make the VST the first large wide-field survey telescope with optical polarimetry. The project addresses the need for optical follow-up observations of Cherenkov Telescope Array (CTA) sources and transients. This paper describes software upgrades required for the new polarimetric mode. The current instrument control software, based on ESO VLT software 2011, manages pointing, acquisition, and active optics. The polarimetric mode necessitates two additional motorized movements: inserting the filter and selecting polarization while tracking the object. Traditionally, VLT systems use a Local Control Unit (LCU) on VxWorks for motor control, but this system is outdated. Since compatibility with modern hardware is crucial, we resorted to a PLC-based system, which are unsupported by the installed VLTSW. Fortunately, the ICS Fieldbus Extension allows for a dedicated Device Control Environment (DCE). This DCE, using an updated VTLSW release, acts as a gateway to control electronics, minimizing system-wide impact and reducing update-related risks.
MAVIS is the new MCAO Assisted Visible Imager and Spectrograph for ESO’s Very Large Telescope. It is intended to be installed at the Nasmyth focus of UT4 “Yepun” telescope and it is composed of two main parts: a multi conjugate adaptive optics module and its post focal instrumentation, an imager and an IFU spectrograph, both operating in the visible spectrum. The project is now in the final design phase, and it is expected to be commissioned in 2030. In this paper we focus on the interface between the Instrument Control System Software (ICSS) and the Soft Real-Time Computer (SRTC). ICSS is in charge of controlling all the motorized functions, managing the scientific exposures, monitoring the status of the system and coordinating the sequence of operations; on the other hand, RTC receives data from from the wavefront sensors (8 LGS and 3 NGS) to compute the corrections to be applied by the two-post focal deformable mirrors and 8 LGS jitter mirrors. ICSS will be based on the new ESO ELT software framework, which is still under development; SRTC will be based on the new ESO RTC Toolkit, also under development. We present the first design of the common interface between ICSS and SRTC, focusing mainly on the communication processes (commands and data) and which are the most critical points we had to face.
The Real-Time Computer of the Multi-Conjugate Adaptive Optics Relay module for the ESO Extremely Large Telescope (MORFEO@ELT) is the subsystem that computes the atmosphere tomography based on the wavefront captured by nine sensors and controls the shape of three deformable mirrors. Implementing the MORFEO RTC presents many technical challenges due to the high data throughput generated by the system sensors and the heavy processing power required for the real-time mirrors’ shape computation. To meet ESO requirements, the ESO RTC Toolkit will be used to build the soft RTC subsystem, while the Hard RTC will be based on a custom architecture. In this paper, we will discuss some activities undertaken to progress toward the Final Design of the SRTC. Specifically, a physical design is proposed for the MORFEO RTC to meet the computational and network requirements. This design will include both the computing cluster and network physical design. To validate the architecture’s functionalities, some prototyping activities have been initiated: Firstly, a subset of the SRTC components has been created to test the main end-to-end data path, i.e. from the source (wavefront sensor) to the permanent storage (telemetry storage), and through the gateway to the consumer data tasks. Additionally, the core and computationally intensive data tasks will be prototyped using simulated data to benchmark different implementation strategies and various hardware solutions. Finally, the distributed system will be prototyped in a virtual or physical environment. These prototyping platforms will be useful in the final design and development stages to test module functionalities and the system and sub-system interfaces.
The MCAO Assisted Visible Imager and Spectrograph (MAVIS) is a new high-resolution instrument operating in the visible band (370-935 nm) that will be installed at the Nasmyth A focus of the ESO VLT UT4. The system is characterized by an Adaptive Optics Module (AOM), a Calibration Unit, an Imager and an IFU Spectrograph. The project recently passed the Preliminary Design Review and is currently in the Final Design phase which is expected to end in December 2024, according to the current schedule. In this paper we present the improvements in the AOM control electronics architecture, the new control cabinets layout and the strategy adopted to cable the AO sub-modules.
The VST (VLT Survey Telescope) is a 2.6m telescope installed in the ESO Observatory of Cerro Paranal, equipped with a wide-field imaging camera operating in the visible band (OmegaCAM). One of the goals of the Cherenkov Telescope Array Plus (CTA+) program, included in the EU Recovery Plan (PNRR), is to upgrade this ground-based optical facility adding a new polarimetric mode to allow the follow-up and monitoring of the CTA transient sources. The VSTPOL design aims to replace the actual electro-opto-mechanical system connected to the back side of the primary mirror cell of the telescope with a new system, consisting of two motorized functions: a linear exchanger mechanism to switch between the traditional imaging mode and the new polarimetric mode; a rotating device equipped with a polarimetric filter, replacing the unused ADC functionality, that enables tracking to compensate for the field rotation, following the movement of the OmegaCAM. Here we present the VSTPOL control electronics architecture, based on the new ESO electronics standards. All the control electronics are hosted in a wall-mountable and properly cooled enclosure installed on-board of the telescope: Commercial Off-The-Shelf (COTS) industrial components (e.g. Beckhoff PLC and EtherCAT fieldbus modules) represent the core of the system to increase the overall reliability and maintainability.
SOXS (Son Of X-Shooter) is the new single object spectrograph for the ESO New Technology Telescope (NTT) at the La Silla Observatory, able to cover simultaneously both the UV-VIS and NIR bands (350-2000 nm). The instrument is currently in the integration and test phase, approaching the Preliminary Acceptance in Europe (PAE) before shipment to Chile for commissioning. After the assembly and preliminary test of the control electronics at INAF - Astronomical Observatory of Capodimonte (Napoli), the two main control cabinets of SOXS are now hosted in Padova, connected to the real hardware. This contribution describes the final electronic cabinets layout, the control strategy and the different integration phases, waiting for the Preliminary Acceptance in Europe and the installation of the instrument in Chile.
The Son Of X-Shooter (SOXS) will be the specialized facility to observe any transient event with a flexible scheduler at the ESO New Technology Telescope (NTT) at La Silla, Chile. SOXS is a single object spectrograph offering simultaneous spectral coverage in UV-VIS (350-850 nm) and NIR (800-2000 nm) wavelength regimes with an average of R∼4500 for a 1” slit. SOXS also has imaging capabilities in the visible wavelength regime. Currently, SOXS is being integrated at the INAF-Astronomical Observatory of Padova. Subsystem- and system-level tests and verification are ongoing to ensure and confirm that every requirement and performance are met. In this paper, we report on the integration and verification of SOXS as the team and the instrument prepare for the Preliminary Acceptance Europe (PAE).
The SOXS spectrograph, designed for the ESO NTT telescope, operates in both the optical (UV-VIS: 350-850 nm) and NIR (800-2000 nm) bands. This article provides an overview of the final tests conducted on the UV-VIS camera system using a telescope simulator. It details the system’s performance evaluation, including key metrics such as gain, readout noise, and linearity, and highlights the advancements made in the upgraded acquisition system. The testing process, conducted in the Padua laboratory, involved comprehensive simulations of the telescope environment to ensure the results closely resemble those expected at the ESO-NTT telescope. The successful completion of these tests confirms the system’s readiness for deployment to Chile, where it will be installed on the NTT telescope, marking a significant milestone in the SOXS project.
Since the start of operations in 2011, the VLT Survey Telescope (VST) has been one of the most efficient wide-field imagers in the optical bands. However, in the next years the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) will be a game-changer in this field. Hence, the timing is appropriate for specializing the VST with additions that can make it unique in well-defined scientific cases. VSTPOL is a project that aims to provide the addition of wide-field polarimetric capabilities to the VST telescope, making it the first large survey telescope for linear optical polarimetry. Actually, while there are quite a number of optical telescopes, the telescopes providing polarimetric instrumentation are just a few. The number of relatively large mirror polarimetric telescopes is small, although they would be specifically needed e.g. to support many science cases of the Cherenkov Telescope Array (CTA) that, in the southern hemisphere, is co-located with the VST. The VST telescope is equipped with a single instrument, the OmegaCAM wide-field imaging camera operating in the visible bands with a field of view of 1° × 1°. The polarimetric mode will be implemented through the insertion of a large rotatable polarizer installed on the field-corrector optics, which will be exchangeable with the non-polarimetric corrector optics. The limiting polarimetric systematic errors due to variable atmospheric conditions and instrumental polarization can be corrected down to a level of ∼ 10−3 by leveraging the large amount of unpolarized stars within each field-of-view. By the user point of view, VSTPOL will be an additional mode for the VST wide-field imaging camera.
SOXS (Son Of X-Shooter) will be the new medium-resolution (R 4500 for 1” slit), high-efficiency, wide-band spectrograph for the ESO NTT at La Silla Observatory, Chile. It will be dedicated to the follow-up of any kind of transient events, ensuring fast time, high efficiency, and availability. It consists of a central structure (common path) that supports two spectrographs optimized for the UV-Visible and a Near-Infrared range. Attached to the common path is the Acquisition and Guiding Camera system (AC), equipped with a filter wheel that can provide science-grade imaging and moderate high-speed photometry. The AC Unit was integrated and aligned during the summer months of 2022 and has since been mounted in the NTT’s telescope simulator. This work gives an update on the Acquisition Camera Unit status, describes the Image Quality Tests that were performed, and discusses the AC Optical Performance.
SOXS (Son Of X-Shooter) is the new ESO instrument that is going to be installed on the 3.58-m New Technology Telescope at the La Silla Observatory. SOXS is a single object spectrograph offering a wide simultaneous spectral coverage from U- to H-band. Although such an instrument may have potentially a large variety of applications, the consortium designed it with a clear science case: it is going to provide the spectroscopic counterparts to the ongoing and upcoming imaging surveys, becoming one of the main follow-up instruments in the Southern hemisphere for the classification and characterization of transients. The NTT+SOXS system is specialized to observe all transients and variable sources discovered by imaging surveys with a flexible schedule maintained by the consortium, based on a remote scheduler which will interface with the observatory software infrastructure. SOXS is realized timely to be highly synergic with transients discovery machines like the Vera C. Rubin Observatory. The instrument has been integrated and tested in Italy, collecting and assembling subsystems coming from all partners spread over six countries in three continents. The first preparatory activities in Chile have been completed at the telescope. This article gives an updated status of the project before the shipping of the instrument to Chile.
In this paper we report about the preliminary design of the Real Time Computer (RTC) for the MORFEO@ELT (formerly MAORY@ELT) Multi-Conjugate Adaptive Optics module for the ESO Extremely Large Telescope. The ELT MCAO module MORFEO provides high sky coverage, large field, diffraction limited correction in the near infrared. It relies on the use of a constellation of six Laser Guide Stars (LGS) and up to three Natural Guide Stars (NGS) for tomographic atmospheric turbulence sensing, and multiple mirrors (ELT M4 and up to two post-focal deformable mirrors) for correction. In particular, we will discuss the overall RTC architecture, the main control strategy, including provision for vibrations compensation, auxiliary loops and tasks for optimization of correction. We will also briefly describe our product and quality assurance plans.
The paper describes the design of the NGS WFS sub-module of MAVIS, an instrument for the VLT UT4 that aims to provide diffraction limited imaging and spectroscopy at visible wavelengths. In this framework the NGS WFS provides means for the tomographic measurement of the lower-orders of the atmospheric turbulence allowing MAVIS to reach the required performances in terms of sky coverage and resolution. We present the optical design and performance of the NGS WFS probes and acquisition camera, the actuators embedded in the subsystem and their control hardware. Finally, we show the mechanical arrangement of the submodule.
MAVIS will be part of the next generation of VLT instrumentation and it will include a visible imager and a spectrograph, both fed by a common Adaptive Optics Module. The AOM consists in a MCAO system, whose challenge is to provide a 30” AO-corrected FoV in the visible domain, with good performance in a 50% sky coverage at the Galactic Pole. To reach the required performance, the current AOM scheme includes the use of up to 11 reference sources at the same time (8 LGSs + 3 NGSs) to drive more than 5000 actuators, divided into 3 deformable mirrors (one of them being UT4 secondary mirror). The system also includes some auxiliary loops, that are meant to compensate for internal instabilities (including WFSs focus signal, LGS tip-tilt signal and pupil position) so to push the stability of the main AO loop and the overall performance. Here we present the Preliminary Design of the AOM, which evolved, since the previous phase, as the result of further trade-offs and optimizations. We also introduce the main calibration strategy for the loops and sub-systems, including NCPA calibration approach. Finally, we present a summary of the main results of the performance and stability analyses performed for the current design phase, in order to show compliance to the performance requirements.
MORFEO (formerly known as MAORY) is a post-focal adaptive optics module that forms part of the first light instrument suite for the Extreme Large Telescope (ELT). The project passed the Preliminary Design Review in two stages in April and July 2021 and is now entering the Final Design Phase. In this paper we report the status of the project.
The MCAO Assisted Visible Imager and Spectrograph (MAVIS) is a new instrument being built for the ESO’s Very Large Telescope (VLT). It will operate at the Nasmyth focus of “UT4” telescope and it is composed of two main parts: a Multi - Conjugate Adaptive Optics (MCAO) module and two post focal scientific channels, an imager and an integral field spectrograph, both operating in the visible spectrum. The project is approaching the final steps of the preliminary design phase and it is expected to have the first light in 2027. We present the status of the Instrument Control Software (ICSS). In particular, we focus on the software architecture and the interaction between ICSS and real-time computer (RTC), telescope control system (TCS) and VLT Laser Guide Stars Facility (4LGSF). Besides the complexity of the instrument, we present a software architecture that is simple and still maintains modularity, guaranteeing the overall functionality of the instrument.
MORFEO (formerly known as MAORY) is the multi-conjugated adaptive optics module for the ESO’s Extremely Large Telescope (ELT). It will serve the first light instrument MICADO. We present the current preliminary design of the Instrument Control Software (ICSS) illustrating the most demanding requirements ICSS has to deal with and how we are going to integrate the MORFEO ICSS architecture with the control software framework ESO is developing for new instruments.
MAVIS (MCAO Assisted Visible Imager and Spectrograph) is a new instrument that will operate on the UT4 of the ESO Very Large Telescope (VLT), delivering comparable angular resolution in the optical to that delivered by ELTs in the infrared. The MAVIS core is represented by a multi-conjugate Adaptive Optics Module (AOM) designed to feed an Imager, a Spectrograph and a visiting instrument, all operating in the visible range. The project is now in the preliminary design phase and will be commissioned in 2027 according to the current plan. We present the current status of the MAVIS AOM instrument control electronics that will manage all the motorized functions and auxiliary sensors, focusing on the main design concepts and the preliminary prototyping activities. The design includes ESO standards and Commercial Off-The-Shelf (COTS) industrial components organized in a modular architecture to simplify the AOM preliminary integration activities, planned simultaneously in different sites. Important guidelines to the design are the attention to the overall reliability and maintainability and the minimization of risks. Almost all the motorized functions are implemented adopting preassembled industrial motorized stages. For the tracking axes, a prototyping activity has been envisaged during the design phases, in order to assess the adopted solutions are compatible with the positioning and tracking requirements.
SOXS (Son Of X-Shooter) is a single object spectrograph offering a simultaneous spectral coverage from U- to H-band, built by an international consortium for the 3.58-m ESO New Technology Telescope at the La Silla Observatory. It is designed to observe all kind of transients and variable sources discovered by different surveys with a highly flexible schedule maintained by the consortium, based on the Target of Opportunity concept. SOXS is going to be a fundamental spectroscopic partner for any kind of imaging survey, becoming one of the premier transient follow-up instruments in the Southern hemisphere. This paper gives an updated status of the project, when the instrument is in the advanced phase of integration and testing in Europe, prior to the activities in Chile.
An accurate alignment of the optical surfaces of a telescope is essential to guarantee an optimal image quality since even small displacements introduce aberrations increasing towards the edges of the field. This effect is especially detrimental in wide-field imagers. This work proposes the derivation of a fully analytical model of the wavefront error as a function of the most likely system misalignments. An accurate response of the telescope under a predefined set of misaligned conditions is obtained through simulations in Zemax OpticStudio. The resulting data is combined through an integrated modeling approach, obtaining a map of the aberrations as a function of a vector of perturbations applied to the optical system. The analytical wavefront error allows for a quick and accurate assessment of the theoretical PSF across the entire image field. As a case study, the example of the Rubin Observatory is adopted, featuring an 8.4m primary mirror and a large field of view.
In wide-field telescopes, relatively small misalignments in the optical system can cause large aberrations. The nominal system is normally designed to show a good optical performance over the whole field of view but, in presence of misalignments, the symmetry is broken and the aberrations increase towards the edge of the field. No new aberrations arise, but the known aberrations behave differently and originate multiple nodes, according to the Nodal Aberration Theory. The effects, in terms of image quality degradation, can be especially deleterious for wide-field imagers. This issue can be studied in detail by the ray-tracing programs that are normally adopted for the optical design. Nevertheless, these codes are not optimal for applications where a high execution speed is needed. Here, an application of PSF reconstruction for a wide-field telescope by using an integrated modeling approach is presented. Ray-tracing data are adopted as input to build a fully analytical model. The example of the VST telescope (1x1 deg field of view) is discussed as a case study.
The axes servo control of optical telescopes and antennas acts in two typical phases: the slew to a new target and the subsequent accurate tracking of the source. Although the tracking error minimization is paramount, a good design of the slewing phase is needed as well. In fact, saturations of velocity and acceleration can easily occur during telescope slew, introducing non-linearities in the control system which may lead to undesired behaviors. Also, sudden accelerations may trigger vibrations of the telescope structure, which may increase the slew time or even prevent a stable target acquisition. In this paper, a command pre-processor is adopted to provide recursively a valid path to reach the assigned target, never exceeding the specified rate and acceleration limits. Different generation methods are considered, with different degrees of smoothness and slewing time. Numerical simulations show their main features in different test cases, for both radio and optical telescopes.
Every night the VST Telescope Control Software logs large text files including information on the telescope and instrument operations, executed commands, failures, weather conditions and anything is relevant for the instrument maintenance and the identification of problem sources. These log files are a precious tool, daily used by the observatory personnel for the analysis of any issue raised by the telescope operators during the night. One of the most frequent use of these data is then to trace back telescope, instrument or enclosure problem sources and analyze them. Consequently, these _les are often analyzed looking only for specific issues and for solving well identified problems, in the framework of dedicated and focused efforts. Thus, a minimal part of the information is useful for this kind of daily maintenance. Nevertheless, the log files contain a gold mine of other data, which often make sense only when analyzed on a long time span. This paper describes a 5-year effort, started in 2015, for the systematic collection and analysis of log files, aiming at the identification of useful long-term trends and statistics which are normally overlooked in the daily telescope life. The specific case of the active optics open-loop corrections is discussed as case study.
SOXS (Son Of X-Shooter) is a single object spectrograph, characterized by offering a wide simultaneous spectral coverage from U- to H-band, built by an international consortium for the 3.6-m ESO New Technology Telescope at the La Silla Observatory, in the Southern part of the Chilean Atacama Desert. The consortium is focussed on a clear scientific goal: the spectrograph will observe all kind of transient and variable sources discovered by different surveys with a highly flexible schedule, updated daily, based on the Target of Opportunity concept. It will provide a key spectroscopic partner to any kind of imaging survey, becoming one of the premier transient follow-up instruments in the Southern hemisphere. SOXS will study a mixture of transients encompassing all distance scales and branches of astronomy, including fast alerts (such as gamma-ray bursts and gravitational waves), mid-term alerts (such as supernovae and X-ray transients), and fixed-time events (such as the close-by passage of a minor planet or exoplanets). It will also have the scope to observe active galactic nuclei and blazars, tidal disruption events, fast radio bursts, and more. Besides of the consortium programs on guaranteed time, the instrument is offered to the ESO community for any kind of astrophysical target. The project has passed the Final Design Review and is currently in manufacturing and integration phase. This paper describes the development status of the project.
KEYWORDS: Control systems, Electronics, Near infrared spectroscopy, UV-Vis spectroscopy, Spectroscopes, New and emerging technologies, Telescopes, Lanthanum, Near infrared, Manufacturing
The forthcoming SOXS (Son Of X-Shooter) will be a new spectroscopic facility for the ESO New Technology Telescope in La Silla, focused on transient events and able to cover both the UV-VIS and NIR bands. The instrument passed the Final Design Review in 2018 and is currently in manufacturing and integration phase. This paper is focused on the assembly and testing of the instrument control electronics, which will manage all the motorized functions, alarms, sensors, and electric interlocks. The electronics is hosted in two main control cabinets, divided in several subracks that are assembled to ensure easy accessibility and transportability, to simplify test, integration and maintenance. Both racks are equipped with independent power supply distribution and have their own integrated cooling systems. This paper shows the assembly strategy, reports on the development status and describes the tests performed to verify the system before the integration into the whole instrument.
During the last few years we have been working on a modernization plan for the Telescopio Nazionale Galileo (TNG) Control System1,2. On October 2019 we had the opportunity to execute the first step of this process. The telescope was going to be stopped for one month due to M1 mirror being aluminized, so we could change the azimuth control system, that had been thoroughly tested during the summer, with no additional observational time loss. In this paper we present the new control system based on the CompactRIO platform from National Instruments, the switching process between the old and the new control systems, and a performance comparison between them.
The servo control algorithms of the TNG, developed in the nineties, have been working for more than 20 years with no major updates. The original hardware was based on a VME-bus based platform running a real time operating system, a rather popular choice for similar applications at the time. Recently, the obsolescence of the hardware and the lack of spares pushed the observatory towards a complete replacement of the electronics that is now being implemented in steps, respecting the basic requirement of never stopping the observatory night operations. Within the framework of this major hardware work, we are taking the opportunity to review and update the existing control schemes. This servo control update, crucial for the telescope performance, envisages a new study from scratch of the controlled plant, including a re-identification of the main axes transfer functions and a re-design of the control filters in the two nested position and speed loops. The ongoing work is described, including preliminary results in the case study of the azimuth axis and our plans for possible further improvements.
SOXS (Son Of X-Shooter) will be a unique spectroscopic facility for the ESO-NTT 3.5-m telescope in La Silla (Chile), able to cover the optical/NIR band (350-1750 nm). The design foresees a high-efficiency spectrograph with a resolutionslit product of ~4,500, capable of simultaneously observing the complete spectral range 350 - 1750 nm with a good sensitivity, with light imaging capabilities in the visible band. This paper outlines the status of the project.
The communication presents an innovative method for the diagnosis of reflector antennas in radio astronomical applications. The approach is based on the optimization of the number and the distribution of the far field sampling points exploited to retrieve the antenna status in terms of feed misalignments, this to drastically reduce the time length of the measurement process and minimize the effects of variable environmental conditions and simplifying the tracking process of the source. The feed misplacement is modeled in terms of an aberration function of the aperture field. The relationship between the unknowns and the far field pattern samples is linearized thanks to a Principal Component Analysis. The number and the position of the field samples are then determined by optimizing the Singular Values behaviour of the relevant operator.
The paper presents an innovative method for the diagnosis of reflector antennas in radio astronomical applications,
which optimizes the number and the location of the far field sampling points exploited to retrieve the antenna status in
terms of feed misalignments. In this way the measurement time length process is drastically reduced to minimize the
effects of the time variations of the measurement setup, as well as the idle time forced by the maintenance activity. The
effects of the feed misalignment are modeled in terms of an aberration function, properly expanded on a set of basis
functions in order to preserve the linear relationship between the unknown parameters defining the antenna status and the
far field pattern, assumed measured in amplitude and phase. Thanks to the optimization of the Singular Values behavior
of the relevant linear operator, in its discrete form, the number and the position of the samples is found. The numerical
analysis shows the effectiveness of the method in the simple case of a phase aperture affected by tilt only, even if the
approach can be extended also to higher order aberrations. The performances are estimated with a comparison with a
standard approach, based on the acquisition of the far field pattern by means of a uniform Cartesian grid defined
according the Nyquist criterion and requiring a number of field samples significantly larger.
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