The European Solar Telescope (EST) will be built at the Observatorio del Roque de los Muchachos, a site known for its excellent atmospheric seeing conditions. The fundamental design of EST lies on two premises to improve the local seeing: placing the primary mirror as far as possible from the ground layer and using an open-air configuration. In this setting, the telescope will benefit from undisturbed wind allowing natural ventilation. These considerations aim to optimize the site conditions; however, the design itself may introduce local seeing. As the design evolves from conceptual to preliminary phase, the shape of the EST has profoundly changed, and the fundamental aspects shall be re-evaluated. In this article, strategic aspects of the current design are studied, including elements from the telescope structure, the pier, and the enclosure. These trade-offs considered the local seeing as a driving force seeking to optimize the optical performance and provide feedback to the current design of EST. This study uses transient Computational Fluid Dynamics (CFD) to estimate the air temperature and refractive index as it flows over the observatory and the telescope. The air refractive index inside the optical path is then analyzed using postprocessing scripts to obtain appropriate seeing metrics. Predominant wind directions and median wind speed at the site together with environmental conditions and different telescope orientations were used to thoroughly analyze the local seeing conditions. Optical results enabled the characterization of the spatial distribution of turbulence, assimilating it to a Kolmogorov law. These results are valuable input for the telescope’s error budget in terms of local seeing.
Computational Fluid Dynamics (CFD) and conjugate heat transfer models have been developed and/or updated to validate thermal requirements for the TMT International Observatory enclosure Heating, Ventilation and Air Conditioning (HVAC) system, azimuth and cap drive systems, interstitial space volume, as well as the Summit Facilities tunnel, mechanical room, utility room, and cooler exhaust. The resulting thermal environment is assessed and linked to performance, wherever applicable.
This paper provides an update on the progress in designing, prototyping, modeling, and manufacturing the TMT first light AO systems and their AO components. Key highlights encompass the completion of the preliminary design of the Laser Guide Star Facility, the fabrication of the NFIRAOS deformable mirrors, the study of the petalling modes impact and associated mitigations for TMT, and the development of the first light verification plan, and assessment of the expected performance.
The Laser Guide Star Facility (LGSF) system of the Thirty Meter Telescope (TMT) will generate up to 8 artificial laser guide stars in the mesospheric sodium layer with the brightness, beam quality, and asterism geometries as required by both the TMT first light AO system and future AO instruments. It includes the sodium lasers mounted on the telescope elevation structure below the primary mirror, the conventional beam transfer optics system to transport the beams up to the telescope top end, and the formatting and launching optics to project the required laser guide star asterism to the sky using a center launch telescope located behind the secondary mirror. In this paper, we will present the recent successful completion of the LGSF preliminary design, including: the optical, mechanical, electronics, safety, control, and software designs; the systems engineering; the modeling activities; and the next steps for the system’s final design phase including prototyping.
Petalling modes characterize the differential piston between the petals of the telescope’s aperture, typically separated by the secondary mirror support spiders. Since the discovery of petalling modes by the VLT in low wind conditions, addressing these modes has become a focal point, pertinent to nearly all telescopes equipped with high-performance adaptive optics systems. These modes are poorly sensed by mainstream wavefront sensors (WFS). There are three primary factors contributing to petalling modes in general. Firstly, turbulence discontinuity occurs across the spiders due to temperature non-uniformity, particularly in low wind conditions. This issue is partly mitigated by applying low emissivity coating, pioneered by the VLT. Computational fluid dynamics models used to assess the dome seeing aid in quantifying the residual effect. Secondly, phasing and stacking errors may arise in segmented mirrors. For TMT, the impact is negligible owing to the small width of the support spiders (22.5 cm) and highly redundant phasing sensors in the Alignment and Phasing System. Lastly, measurement noise may propagate to these modes, which we have observed when controlling two deformable mirrors in classic adaptive optics (AO) mode with a single pyramid WFS. Employing modal control with truncated modes is a simple and effective mitigation strategy without a notable performance penalty. Nevertheless, having a mechanism that can measure and control the petalling modes will provide reassurance of the AO system’s performance. In this paper, we present a novel hybrid iterative petalling sensor (HIPS) that utilizes modal based phase retrieval on time averaged PSFs from diffraction-limited tip/tilt/focus and full aperture low-order wavefront sensors, which breaks the even mode ambiguity. We successfully demonstrated this algorithm in both static and end-to-end closed-loop AO simulations.
Conjugate heat transfer modeling is used to estimate the front temperature distribution, thermal deformation, and differential pressure distribution of the GMT primary mirror (M1) segments. The modeling framework validates segment temperature and thermal deformation requirements and supports the M1 optical testing underway. This paper presents the various framework models, the predicted baseline performance, and a sensitivity analysis of the impact of several heat sources on the expected thermal deformation, including simulations specific to optical testing.
An aerothermal modeling framework was developed for the entire TMT International Observatory Laser Guide Star Facility, consisting of several standalone conjugate heat transfer models: laser head, laser bench array, optical path pointing arrays, beam transfer duct, top end including the laser telescope assembly, and several electronics cabinets, resolving all interior components. The primary goals were to evaluate the focus error from the thermal lens deformation, to evaluate beam jitter from the optical path difference maps along the beam path, and to obtain the temperature of all exterior surfaces. The framework provided performance sensitivity to specific inputs/assumptions and lead to improved design that meets performance requirements.
The TMT International Observatory CFD model, procedure to obtain thermal boundary conditions, input/output and statistical performance analysis tools have been updated and enhanced. Zero-wind effects, component wind jitter relative to the telescope structure and heat transfer coefficient statistics have been included. Sensitivity studies are performed, and conclusions are drawn.
The Giant Magellan Telescope project has invested in creating a series of computational fluid dynamics (CFD) models to analyze how aero-thermodynamic effects impact the telescope optical performance. We use several models that feed into each other for the goal of accurately determining temperature induced collimation errors. We start with thermal network modeling, using one-dimensional approximations for a long period of time. The second is a detailed CFD model of the entire telescope. This model generates a transient, three-dimensional temperature distribution within the telescope structure over a timespan ranging from a few hours to several days in a cyclical nature. These temperature maps are fed into a structural model of the telescope, using finite element and finite volume analysis, which calculates how the structural components deform in response to the temperature spatial variability. They also provide more accurate surface temperatures for dome seeing estimates. This combined thermo-mechanical model serves to quantify the telescope optical misalignment with respect to the ambient temperature diurnal variation. These thermal deformations are then fed to the telescope optical model, which conducts the ray tracing through the optics to the telescope focal plane, ultimately yielding the associated image quality. This paper outlines the computational framework developed for these purposes and showcases some of the results obtained.
The Giant Magellan Telescope Project relies on a comprehensive integrated modeling (IM) tool to evaluate Observatory Performance Modes (OPM), ranging from Seeing Limited to Adaptive Optics. The development of the integrated model is driven by the need to accurately estimate errors that affect the science instrument data products and mitigate technological risks associated with the telescope. The IM end-to-end simulation models combine structural dynamics, optics, and control models seamlessly in a unified framework. Computational fluid dynamics analysis produces a set of time series representing most of the disturbance sources affecting the telescope performance (namely, dome seeing, wind loads, and structural thermal deformations) under different boundary conditions. Conceiving and managing such a tool imposes several challenges. Firstly, due to the wide range of scientific and engineering expertise required. Furthermore, developing a realistic system representation while dealing with the computational aspects is critical, particularly in adaptive optics OPMs, where the system complexity (vast number of degrees of freedom combining slow and fast dynamic behaviors demanding high sampling rates) can make simulations impractically long. This paper presents the architecture of the GMT integrated model tailored for the Natural Guide Star and Laser Tomography Adaptive Optics OPMs. The features of the computing framework that integrates the domain-specific models into a unified model are also approached. We also show end-to-end simulation results illustrating the interaction between the control loops composing those adaptive optics modes.
The TMT Laser Guide Star Facility (LGSF) system is responsible for generating the artificial guide stars in the mesospheric sodium layer with the brightness, beam quality and asterism geometries required by both the first light AO system and future AO instruments. It includes the sodium lasers mounted on the elevation structure, the beam transfer optics to transport the beams up to the telescope top end, and the formatting and launching optics to project the required laser guide star asterism to the sky using a center launch telescope. In this paper, we will present the LGSF preliminary design including the design trade-offs, the optical, mechanical, electronics and software design, as well as the modeling activities.
The GMT strategy for advancing subsystem design using aerothermal modeling is presented. The focus is not on the models themselves but on the procedure used to answer specific questions posed to the GMT System Engineering Integrated Modeling team by the various subsystem groups. Work in progress from an aerothermal point of view will be presented in several major subsystems. The scheduling challenges and resource management, both computational and human, to ensure timely responses are also addressed.
The scientific performances of the Giant Magellan Telescope (GMT) Observatory are divided into Observatory Performance Mode (OPM) formally defined in the GMT Observatory Requirement Document (ORD) as a direct flow down from the GMT Science Requirement document (SRD). There are 3 main OPM categories: Natural Seeing, GLAO, and High Angular Resolution (e.g., NGAO, LTAO) that branched out into several sub-categories. For each OPM, system engineering has defined image quality metric standards: Key Performance Parameters (KPP) that acts as bounds to the Observatory overall performance within which design parameters are traded. During the course of the project, system engineering must assess the compliance of the current design solutions with respect to the KPPs. The GMT project has build an exhaustive integrated modeling computing framework allowing for bottom-up end-to-end modeling of the entire GMT Observatory. This integrated modeling framework brings together finite element, control, optical, thermal and fluid dynamics models. This paper introduces the integrated modeling framework and describes the whole process that is setting up bottom-up end-to-end simulations of GMT OPMs. For example, analytical error budgets and the project risk registers are used to identify and to down select the most relevant parameters and features of the telescope design that must be included into the GMT integrated model while keeping the size of the simulation manageable from a computing load standpoint. The paper also reports on how the model validation unfold with model audits at both system and subsystem levels using software management best practices. Finally, simulation results for several OPMs are presented and discussed in terms of their statistical meaning with respect to the foreseen on-sky estimation of the KPPs during the Assembly, Integration and Validation phase of the project.
KEYWORDS: Systems engineering, Interfaces, Computer aided design, Observatories, Systems modeling, Standards development, Safety, Reliability, Databases, Control systems
The objective of the systems engineering effort is to ensure the successful development and operability of the TMT system, by defining clear policies and procedures for architecture definition, requirements management, interface management, integration management, and verification. This paper shows the tailored implementation of the systems engineering approach which is intended to ensure that the system meets all requirements while being affordable, producible, and maintainable over the observatory’s life, while maintaining acceptable risk. This paper also describes the evolution of this approach in the last decade at TMT and the reasoning behind that evolution.
Environmental effects on the Image Quality (IQ) of the Thirty Meter Telescope (TMT) are estimated by aero-thermal numerical simulations. This study summarizes the state of the art of optical turbulence modeling and presents an update of the ongoing effort to minimize prediction time and computational resources by extrapolating the convergence of TMT’s IQ metric in the spatial resolution limit with quantifiable uncertainty, in order to be able to conduct trade studies and assess IQ sensitivity to various thermal gradient inputs.
This paper presents the state-of-the-art techniques employed in aerothermal modeling to respond to the current observatory design challenges, and in particular those of the US Extremely Large Telescope Program (USELTP). It reviews the various aerothermal simulation techniques, the synergy between modeling outputs and observatory integrating modeling and recent applications. Finally, it addresses planned improvements, the development of new ideas, attacking new challenges and how it all ties to the AIAA “CFD 2030 Vision”.
System engineering at GMTO is using a comprehensive integrated model that integrates seamlessly, in a unified framework, finite element, optics, and control models. A computational fluid dynamics (CFD) model of the observatory is also used to estimate dome seeing, wind jitter, structural thermal deformations, and observatorywide design optimization. The GMT integrated modeling group realizes various studies for different subsystems of the project that provides the basis for the subsystem level design trades. It also assists system engineering by performing top-down and bottom-up requirements verification, error budget derivation, and operational strategies optimization. Integrated modeling will also support system engineering during the assembly, integration, verification, and commissioning phase of the project. For example, system engineering relies on the integrated model to estimate the key performance parameters (KPP) of the project. The KPP are performance metrics that will be used to validate the completion of the observatory and to confirm its readiness with respect to the start of science observation. In the paper, we give a system-level overview of the integrated model, including a description of each sub-model and of the framework that binds them together. The paper also describes how system engineering is using the integrated model for the derivation of the error budgets and of the top-down requirements flowing down from the science requirements to the lower level of subsystem engineering requirements; and how as the design of the subsystems progress, integrated modeling is then used to validate, bottom-up, the same requirements from subsystem engineering requirements back up to the science requirements with respect to the observatory performance metrics.
Validation of Computational Fluid Dynamics (CFD) solutions using experimental data is critical as CFD simulations are regularly used for site characterization and design analysis of Extremely Large Telescopes (ELT). Site testing data for wind, temperature and optical turbulence are used to validate the GMT CFD model configuration for the construction site at Las Campanas Peak in Northern Chile. CFD simulations, both steady-state and unsteady, combined with the corresponding seeing models are performed and estimates of the Ground Layer (GL) optical turbulence are calculated. Comparisons with wind, temperature and optical turbulence profiles are made that show a good match between simulated and observed data.
The Giant Magellan Telescope (GMT) will be one of the most powerful ground-based telescopes in the world upon commissioning at the Las Campanas Observatory (LCO) in Chile. The GMT enclosure protects the telescope, and its systems, from the external environment and plays a crucial role in delivering high quality celestial imagery. This paper describes the development and application of a 3D finite element model of the GMT enclosure and key internal components. This model was developed by Boeing Research & Technology (BR&T), under contract from the Giant Magellan Telescope Organization (GMTO), to characterize the complex interplay of convective, radiative and conductive heat transfer between components within the GMT enclosure and the surrounding environment. The primary intent of this analysis tool is to provide GMT engineers with input conditions for detailed conjugate heat transfer and aero-optic simulations. These simulations will support GMTO’s optimization of their enclosure design to maximize image quality and daily imaging time with minimal use of active thermal controls.
Environmental effects on the Image Quality (IQ) of the Thirty Meter Telescope (TMT) are estimated by aero-thermal numerical simulations. The current study constitutes an update of the ongoing effort to minimize simulation time and to make the computation tractable with available computational resources, to understand the subsequent physical and numerical limitations, and finally to develop the approach to mitigate the issues experienced. In particular, the paper describes a mesh and time-step independence study as well as the parameters that influence the slope of the Optical Path Difference (OPD) structure function and the TMT Normalized Point Source Sensitivity Image Quality metric in the context of thermal seeing.
High spatial resolution thermal unsteady CFD simulations of LSST are performed and processed to provide image degradation due to dome seeing in FWHM. An analysis of the sensitivity of the image quality to certain important geometric features and aerothermal properties is presented. More specifically, the influence of the LSST vent light baffles and windscreen, the wind speed and the surface temperature of components such as the primary and secondary mirrors, the camera, the telescope structure and dome exterior is assessed and conclusions are drawn. The secondary mirror and camera surface temperatures are found to be among the most critical in minimizing LSST dome seeing.
A detailed Computational Fluid Dynamics (CFD) model for the Giant Magellan Telescope (GMT) telescope has been developed and used to simulated and analyze the aero-optical environment around the observatory. The developed model accounts for the major observatory components such as the primary (M1) and secondary (M2) mirrors, the M2 supporting truss, other subcomponents of the telescope mount, and enclosure building along with the auxiliary and site support buildings on the summit. A large topographical area around the installation site is included. This study evaluates three different lower enclosure designs; a closed soffit, an open soffit and a perforated ring-wall (partially closed soffit). Timevarying CFD simulations provide detailed flow and temperature fields along the optical path, which are subsequently used to compute optical parameters such as Optical Path Difference (OPD) maps and Point Source Sensitivity normalized (PSSn), the GMT Image Quality (IQ) metric. Results show that enclosure-induced turbulent flow patterns and refractive index variations have a greater influence on optical performance compared to flow and thermal behavior external to the enclosure. Instantaneous and mean PSSn values obtained for the three soffit configurations show minor differences, indicating that the lower enclosure design has minimal impact on observatory optical performance for the simulated operating conditions.
The Observatorio del Roque de Los Muchachos (ORM) on the Canary island of La Palma has been selected as the alternate site for the Thirty Meter Telescope (TMT). Several potential locations on the summit needed to be investigated in terms of Ground Layer (GL) strength. Moreover, the presence of existing observatories necessitated a study of the interaction between these observatories and TMT. Lack of localized site testing and the nature of the terrain led to the use of Computational Fluid Dynamics (CFD) simulations combined with a seeing model for GL optical turbulence estimates. Three candidate locations for TMT at ORM were investigated under certain wind directions using steady-state simulations. For the most likely candidate the influence of TMT on two nearby telescopes, Gran Telescopio Canarias (GTC) and Telescopio Nationale Galileo (TNG), and vice-versa was also explored and conclusions were drawn.
KEYWORDS: Thirty Meter Telescope, Computer simulations, Device simulation, Space telescopes, Spatial resolution, Telescopes, Monte Carlo methods, Turbulence, Observatories, Optical spheres
Environmental effects on the Image Quality (IQ) of the Thirty Meter Telescope (TMT) are estimated by aero-thermal numerical simulations. These simulations utilize Computational Fluid Dynamics (CFD) to estimate, among others, thermal (dome and mirror) seeing as well as wind jitter and blur. As the design matures, guidance obtained from these numerical experiments can influence significant cost-performance trade-offs and even component survivability. The stochastic nature of environmental conditions results in the generation of a large computational solution matrix in order to statistically predict Observatory Performance. Moreover, the relative contribution of selected key subcomponents to IQ increases the parameter space and thus computational cost, while dictating a reduced prediction error bar. The current study presents the strategy followed to minimize prediction time and computational resources, the subsequent physical and numerical limitations and finally the approach to mitigate the issues experienced. In particular, the paper describes a mesh-independence study, the effect of interpolation of CFD results on the TMT IQ metric, and an analysis of the sensitivity of IQ to certain important heat sources and geometric features.
The Laser Guide Star Facility (LGSF) system of the Thirty Meter Telescope (TMT) will generate the artificial laser guide stars required by the TMT Adaptive Optics (AO) systems. The LGSF uses multiple sodium lasers to generate and project several asterisms from a laser launch telescope located behind the TMT secondary mirror. The laser beams are transported from a location below the primary mirror to the launch telescope using conventional optics to relay the beams along the telescope structure. The beams and relay optics are enclosed into hermetic ducts for safety reasons and to protect the optics against the environment. A Computational Solid Fluid Dynamics (CSFD) model of the LGSF ducts has been developed. It resolves the duct thickness, laser beam transfer lenses, mirrors and their framework for most of the laser beam path that is subject to significant temperature gradients and/or large vertical change. It also resolves the air inside the duct and its thermal interaction with the aforementioned components through conjugate heat transfer. The thermal interaction of the laser beam with the optics is also captured. The model provides guidance to the LGSF design team and a first estimate of the laser beam stability performance and requirement compliance. As the telescope structure design has evolved in the recent years, a new optical path has been proposed for the LGSF. Both the original and the new optical paths are compared against optical, mechanical and other telescope performance related criteria. The optical performance criteria include a first order analysis of the optical turbulence generated within the ducts. In this study simulations of the thermal environment within the ducts of the two candidate paths are performed and conclusions are drawn.
KEYWORDS: Telescopes, Domes, Large Synoptic Survey Telescope, Cameras, Device simulation, Systems modeling, Monte Carlo methods, Thermal modeling, Performance modeling, 3D modeling
Begin Dome seeing is a critical effect influencing the optical performance of ground based telescopes. A previously reported combination of Computational Fluid Dynamics (CFD) and optical simulations to model dome seeing was implemented for the latest LSST enclosure geometry. To this end, high spatial resolution thermal unsteady CFD simulations were performed for three different telescope zenith angles and four azimuth angles. These simulations generate time records of refractive index values along the optical path, which are post-processed to estimate the image degradation due to dome seeing. This method allows us to derive the distribution of seeing contribution along the different optical path segments that composed the overall light path between the entrance of the dome up to the LSST science camera. These results are used to recognize potential problems and to guide the observatory design. In this paper, the modeling estimates are reviewed and assessed relative to the corresponding performance allocation, and combined with other simulator outputs to model the dome seeing impact during LSST operations.
The thermal behavior of the Thirty Meter Telescope (TMT) Telescope Structure (STR) and the STR mounted subsystems
depends on the heat load of the System, the thermal properties of component materials and the environment as
well as their interactions through convection, conduction and radiation.
In this paper the thermal environment is described and the latest three-dimensional Computational Solid Dynamics
(CSD) model is presented. The model tracks the diurnal temperature variation of the STR and the corresponding
deformations. The resulting displacements are fed into the TMT Merit Function Routine (MFR), which converts them
into translations and rotations of the optical surfaces. They, in turn, are multiplied by the TMT optical sensitivity matrix
that delivers the corresponding pointing error. Thus the thermal performance of the structure can be assessed for
requirement compliance, thermal drift correction strategies and look-up tables can be developed and design guidance can
be provided.
Results for a representative diurnal cycle based on measured temperature data from the TMT site on Mauna Kea and
CFD simulations are presented and conclusions are drawn.
KEYWORDS: Systems engineering, Observatories, Computer aided design, Control systems, Data modeling, Systems modeling, Performance modeling, Databases, Interfaces, Thirty Meter Telescope
This paper provides an overview of the system design, architecture, and construction phase system engineering processes of the Thirty Meter Telescope project. We summarize the key challenges and our solutions for managing TMT systems engineering during the construction phase. We provide an overview of system budgets, requirements and interfaces, and the management thereof. The requirements engineering processes, including verification and plans for collection of technical data and testing during the assembly and integration phases, are described. We present configuration, change control and technical review processes, covering all aspects of the system design including performance models, requirements, and CAD databases.
An extensive campaign of aero-thermal modeling of the Thirty Meter Telescope (TMT) has been carried out and
presented in other papers. This paper presents a summary view of overall heat balance of the TMT observatory. A key
component of this heat balance that can be managed is the internal sources of heat dissipation to the ambient air inside
the enclosure. An engineering budget for both daytime and nighttime sources is presented. This budget is used to ensure
that the overall effects on daytime cooling and nighttime seeing are tracked and fall within the modeled results that
demonstrate that the observatory meets its performance requirements.
In the daytime heat fluxes from air-conditioning, solar loading, infiltration, and deliberate venting through the enclosure
top vent are included along with equipment heat sources.
In the nighttime convective heat fluxes through the open aperture and vent doors, as well as radiation to the sky are
tracked along with the nighttime residual heat dissipations after cooling from equipment in the observatory. The diurnal
variation of thermal inertia of large masses, such as the telescope structure, is also included.
Model results as well as the overall heat balance and thermal management strategy of the observatory are presented.
Unsteady wind loads due to turbulence inside the telescope enclosure result in image jitter and higher-order image degradation due to M1 segment motion. Advances in computational fluid dynamics (CFD) allow unsteady simulations of the flow around realistic telescope geometry, in order to compute the unsteady forces due to wind turbulence. These simulations can then be used to understand the characteristics of the wind loads. Previous estimates used a parametric model based on a number of assumptions about the wind characteristics, such as a von Karman spectrum and frozen-flow turbulence across M1, and relied on CFD only to estimate parameters such as mean wind speed and turbulent kinetic energy. Using the CFD-computed forces avoids the need for assumptions regarding the flow. We discuss here both the loads on the telescope that lead to image jitter, and the spatially-varying force distribution across the primary mirror, using simulations with the Thirty Meter Telescope (TMT) geometry. The amplitude, temporal spectrum, and spatial distribution of wind disturbances are all estimated; these are then used to compute the resulting image motion and degradation. There are several key differences relative to our earlier parametric model. First, the TMT enclosure provides sufficient wind reduction at the top end (near M2) to render the larger cross-sectional structural areas further inside the enclosure (including M1) significant in determining the overall image jitter. Second, the temporal spectrum is not von Karman as the turbulence is not fully developed; this applies both in predicting image jitter and M1 segment motion. And third, for loads on M1, the spatial characteristics are not consistent with propagating a frozen-flow turbulence screen across the mirror: Frozen flow would result in a relationship between temporal frequency content and spatial frequency content that does not hold in the CFD predictions. Incorporating the new estimates of wind load characteristics into TMT response predictions leads to revised estimates of the response of TMT to wind turbulence, and validates the aerodynamic design of the enclosure.
KEYWORDS: Telescopes, Device simulation, Monte Carlo methods, Observatories, Computer aided design, Camera shutters, Systems modeling, Interfaces, Computer simulations, Thirty Meter Telescope
Aero-thermal simulations are an integral part of the design process for the Thirty Meter Telescope (TMT). These simulations utilize Computational Solid-Fluid Dynamics (CSFD) to estimate wind jitter and blur, dome and mirror seeing, telescope pointing error due to thermal drift, and to predict thermal effects on performance of components such as the primary mirror segments. Design guidance obtained from these simulations is provided to the Telescope, Enclosure, Facilities and Adaptive Optics groups. Computational advances allow for model enhancements and inclusion of phenomena not previously resolved, such as transient effects on wind loading and thermal seeing due to vent operation while observing or long exposure effects, with potentially different flow patterns corresponding to the beginning and end of observation. Accurate knowledge of the Observatory aero-thermal environment will result in developing reliable look-up tables for effective open loop correction of key active optics system elements, and cost efficient operation of the Observatory.
The Maunakea Spectroscopic Explorer (MSE; formerly Next Generation Canada-France-Hawaii Telescope) is a dedicated, 10m aperture, wide-field, fiber-fed multi-object spectroscopic facility proposed as an upgrade to the existing Canada-France-Hawaii Telescope on the summit of Mauna Kea. The enclosure vent configuration design study is the last of three studies to examine the technical feasibility of the proposed MSE baseline concept. The enclosure vent configuration study compares the aero-thermal performance of three enclosure ventilation configurations based on the predicted dome thermal seeing and air flow attenuation over the enclosure aperture opening of a Calotte design derived from computational fluid dynamics simulations. In addition, functional and operation considerations such as access and servicing of the three ventilation configurations is discussed.
Dome and mirror seeing are critical effects influencing the optical performance of ground-based telescopes.
Computational Fluid Dynamics (CFD) can be used to obtain the refractive index field along a given optical path and
calculate the corresponding image quality utilizing optical modeling tools. This procedure is validated using
measurements from the Keck II and CFHT telescopes.
CFD models of Keck II and CFHT observatories on the Mauna Kea summit have been developed. The detailed models
resolve all components that can influence the flow pattern through turbulence generation or heat release. Unsteady
simulations generate time records of velocity and temperature fields from which the refractive index field at a given
wavelength and turbulence parameters are obtained.
At Keck II the Cn2 and l0 (inner scale of turbulence) were monitored along a 63m path sensitive primarily to turbulence
around the top ring of the telescope tube. For validation, these parameters were derived from temperature and velocity
fluctuations obtained from CFD simulations.
At CFHT dome seeing has been inferred from their database that includes telescope delivered Image Quality (IQ). For
this case CFD simulations were run for specific orientations of the telescope respect to incoming wind, wind speeds and
outside air temperature. For validation, temperature fluctuations along the optical beam from the CFD are turned to
refractive index variations and corresponding Optical Path Differences (OPD) then to Point Spread Functions (PSF) that
are ultimately compared to the record of IQ.
The Large Synoptic Survey Telescope (LSST) optical design calls for a large annular 3.4 m diameter meniscus convex aspheric Secondary Mirror (M2). The M2 has a mass of approximately 1.5 metric tons and the optimized mirror support system consists of 72 axial actuators, mounted at the mirror back surface, and 6 tangent link lateral supports mounted around the outer edge. A fully integrated M2 Finite Element Model (FEM) including the mirror and the support systems has been developed to investigate the performance of the M2 assembly and to determine the image degradation due to dynamic wind loading. Detailed wind response analysis was performed based on the input from Computational Fluid Dynamics (CFD) simulations. Image quality calculations of the time history responses and Power Spectrum Density (PSD) are addressed.
This paper describes Computational Fluid Dynamic (CFD) analyses combined with thermal
analyses for modeling the effects of passive ventilation, enclosure-building configuration and
topography on the optical performance of the Large Synoptic Survey Telescope (LSST). The
primary purpose of the analyses was to evaluate the seeing contribution of the major enclosure-facility
elements and to select the features to be adopted in the baseline design from among
various configurations being explored by the LSST project and the contracted architectural
design team.
In addition, one of several simulations for different telescope orientations is presented including
various wind-telescope relative azimuth angles. Using a post-processing analysis, the effects of
turbulence and thermal variations within the airflow around the buildings and inside the
telescope-enclosure configuration were determined, and the optical performance due to the
thermal seeing along the optical path was calculated.
Studies of astronomical seeing at the Canada France Hawaii Telescope (CFHT) site, from both inside and outside the
dome, show that the full potential of the excellent seeing conditions at the CFHT site has never been fully exploited.
These studies indicate that this is due to the classical unvented hemispherical CFHT dome. Tests have been performed
to identify the causes of the “pathologies” revealed by these seeing studies and to find ways of mitigating them. In
particular, we have investigated installing vents in the dome skin to improve air exchange between outside and inside the
enclosure. A number of vent geometries were tested using water tunnel models at the University of Washington
Aerodynamics Laboratory (UWAL). Relative flushing times for various dome slit to prevailing wind directions were
compared for the different vent geometries. The general flow characteristics observed with these low Reynolds number
tests were compared with computational fluid dynamics (CFD) simulations of the CFHT dome performed in
collaboration with the Thirty Meter Telescope (TMT) project, as well as low-speed wind-tunnel tests and visualization of
the flow around the actual observatory building.
Thermal modeling of the Thirty Meter Telescope (TMT) was conducted for evaluations of thermal performances by finite element (FE) and optical analysis tools. The thermal FE models consist of the telescope optical assembly systems, instruments, laser facility, control and electronic equipments, and telescope structural members. A three-consecutive-day thermal environment data was implemented for the thermal boundary created by Computational Fluid Dynamics (CFD) based on the environment conditions of the TMT site. Temporal and spatial temperature distributions of the optical assembly systems and the telescope structure were calculated under the environmental thermal conditions including air convections, conductions, heat flux loadings, and radiations. With the calculated temperature distributions, the thermo-elastic analysis was performed to predict thermal deformations of the telescope structure and the optical systems. The line of sight calculation was made using the thermally induced deformations of the optics and structures. Merit function routines (MFR) were utilized to calculate the Optical Path Difference (OPD) maps after repositioning the optics based on a best fit of M1 segment deformations. The goal of this thermal modeling is to integrate the mechanical and optical deformations in order to simulate the thermal effects with the TMT site environment data from CFD.
KEYWORDS: Thermal modeling, Telescopes, Solar radiation models, Systems modeling, Thermography, Monte Carlo methods, 3D modeling, Domes, Device simulation, Thirty Meter Telescope
The Performance Error Budget of the Thirty Meter Telescope (TMT) suggests that nearly one third of the total image degradation is due to aero-thermal disturbances (mirror and dome seeing, dynamic wind loading and thermal deformations of the optics, telescope structure and enclosure). An update of the current status of aero-thermal modeling and Computational Fluid-Solid Dynamics (CFSD) simulations for TMT is presented.
A fast three-dimensional transient conduction-convection-radiation bulk-air-volume model has also been developed for the enclosure and selected telescope components in order to track the temperature variations of the surfaces, structure and interstitial air over a period of three years using measured environmental conditions. It is used for Observatory Heat Budget analysis and also provides estimates of thermal boundary conditions required by the CFD/FEA models and guidance to the design.
Detailed transient CFSD conjugate heat transfer simulations of the mirror support assemblies determine the direction of heat flow from important heat sources and provide guidance to the design.
Finally, improved CFD modeling is used to calculate wind forces and temperature fields. Wind loading simulations are demonstrated through TMT aperture deflector forcing. Temperature fields are transformed into refractive index ones and the resulting Optical Path Differences (OPDs) are fed into an updated thermal seeing model to estimate seeing performance metrics. Keck II simulations are the demonstrator for the latter type of modeling.
Modeling is an integral part of systems engineering. It is utilized in requirement validation, system verification, as well as for supporting design trade studies. Modeling highly complex systems poses particular challenges, including the definition and interpretation of system performance, and the combined evaluation of physical processes spanning a wide range of time frames. Our solution is based on statistical interpretation of system performance and a unique image quality metric developed by TMT. The Stochastic Framework and Point Source Sensitivity allow us to properly estimate and combine the optical effects of various disturbances and telescope imperfections.
KEYWORDS: Actuators, Mirrors, Turbulence, Servomechanisms, Adaptive optics, Telescopes, Data modeling, Systems modeling, Wind energy, Control systems design
The principal dynamic disturbances acting on a telescope segmented primary mirror are unsteady wind pressure
(turbulence) and narrowband vibration from rotating equipment. Understanding these disturbances is essential
for the design of the segment support assembly (SSA), segment actuators, and primary mirror control system
(M1CS). The wind disturbance is relatively low frequency, and is partially compensated by M1CS; the response
depends on the control bandwidth and the quasi-static stiffness of the actuator and SSA. Equipment vibration is
at frequencies higher than the M1CS bandwidth; the response depends on segment damping, and the proximity
of segment support resonances to dominant vibration tones. We present here both disturbance models and
parametric response. Wind modeling is informed by CFD and based on propagation of a von Karman pressure
screen. The vibration model is informed by analysis of accelerometer and adaptive optics data from Keck. This
information is extrapolated to TMT and applied to the telescope structural model to understand the response
dependence on actuator design parameters in particular. Whether the vibration response or the wind response
is larger depends on these design choices; "soft" (e.g. voice-coil) actuators provide better vibration reduction
but require high servo bandwidth for wind rejection, while "hard" (e.g. piezo-electric) actuators provide good
wind rejection but require damping to avoid excessive vibration transmission to the primary mirror segments.
The results for both nominal and worst-case disturbances and design parameters are incorporated into the TMT
actuator performance assessment.
Atmospheric optical turbulence is the main driver of wavefront distortions which affect optical telescope performance.
Therefore, many techniques have been developed to measure the optical turbulence strength along the line of sight.
Based on data collected with the MASS (Multi Aperture Scintillation Sensor), we show that a large sample of such
measurements can be used to assess the average three dimensional turbulence distribution above ground.
The use of, and a more sophisticated instrumental setup for, such turbulence tomography will be discussed.
KEYWORDS: Telescopes, Convection, Thermal modeling, Thermal analysis, Finite element methods, Actuators, Mirrors, Systems modeling, Space telescopes, Thirty Meter Telescope
Thermal performances of the Thirty Meter Telescope (TMT) structure were evaluated by finite element thermal models.
The thermal models consist of the telescope optical assembly systems, instruments, laser facility, control and electronic
equipments, and structural members. Temporal and spatial temperature distributions of the optical assembly systems and
the telescope structure were calculated under various thermal conditions including air convections, conductions, heat flux
loadings, and radiations. In order to capture thermal responses faithfully, a three-consecutive-day thermal environment
data was implemented. This thermal boundary condition was created by CFD based on the environment conditions of the
corresponding TMT site. The thermo-elastic analysis was made to predict thermal deformations of the telescope
structure at every hour for three days. The line of sight calculation was made using the thermally induced structural
deformations. Merit function was utilized to calculate the OPD maps after repositioning the optics based on a best fit of
M1 segment deformations. The goal of this thermal analysis is to establish creditable thermal models by finite element
analysis to simulate the thermal effects with the TMT site environment data. These thermal models can be utilized for
estimating the thermal responses of the TMT structure. Thermal performance prediction of the TMT structure will guide
us to assess the thermal impacts, and enables us to establish a thermal control strategy and requirements in order to
minimize the thermal effects on the telescope structure due to heat dissipation from the telescope mounted equipment
and systems.
Core components of systems engineering are the proper understanding of the top level system requirements, their
allocation to the subsystems, and then the verification of the system built against these requirements. System
performance, ultimately relevant to all three of these components, is inherently a statistical variable, depending on
random processes influencing even the otherwise deterministic components of performance, through their input
conditions. The paper outlines the Stochastic Framework facilitating both the definition and estimate of system
performance in a consistent way. The environmental constraints at the site of the observatory are significant design
drivers and can be derived from the Stochastic Framework, as well. The paper explains the control architecture capable
of achieving the overall system performance as well as its allocation to subsystems. An accounting for the error and
disturbance sources, as well as their dependence on environmental and operational parameters is included. The most
current simulations results validating the architecture and providing early verification of the preliminary TMT design are
also summarized.
KEYWORDS: Telescopes, Thermal modeling, Device simulation, Systems modeling, Finite element methods, Thermography, Mirrors, Monte Carlo methods, Solar radiation models, Temperature metrology
In a previous study we had presented a summary of the TMT Aero-Thermal modeling effort to support thermal seeing
and dynamic loading estimates. In this paper a summary of the current status of Computational Fluid Dynamics (CFD)
simulations for TMT is presented, with the focus shifted in particular towards the synergy between CFD and the TMT
Finite Element Analysis (FEA) structural and optical models, so that the thermal and consequent optical deformations of
the telescope can be calculated.
To minimize thermal deformations and mirror seeing the TMT enclosure will be air conditioned during day-time to the
expected night-time ambient temperature. Transient simulations with closed shutter were performed to investigate the
optimum cooling configuration and power requirements for the standard telescope parking position.
A complete model of the observatory on Mauna Kea was used to calculate night-time air temperature inside the
enclosure (along with velocity and pressure) for a matrix of given telescope orientations and enclosure configurations.
Generated records of temperature variations inside the air volume of the optical paths are also fed into the TMT thermal
seeing model.
The temperature and heat transfer coefficient outputs from both models are used as input surface boundary conditions in
the telescope structure and optics FEA models. The results are parameterized so that sequential records several days long
can be generated and used by the FEA model to estimate the observing spatial and temporal temperature range of the
structure and optics.
The LSST camera is located above the LSST primary/tertiary mirror and in front of the secondary mirror in the shadow
of its central obscuration. Due to this position within the optical path, heat released from the camera has a potential
impact on the seeing degradation that is larger than traditionally estimated for Cassegrain or Nasmyth telescope
configurations. This paper presents the results of thermal seeing modeling combined with Computational Fluid
Dynamics (CFD) analyzes to define the thermal requirements on the LSST camera.
Camera power output fluxes are applied to the CFD model as boundary conditions to calculate the steady-state
temperature distribution on the camera and the air inside the enclosure. Using a previously presented post-processing
analysis to calculate the optical seeing based on the mechanical turbulence and temperature variations along the optical
path, the optical performance resulting from the seeing is determined. The CFD simulations are repeated for different
wind speeds and orientations to identify the worst case scenario and generate an estimate of seeing contribution as a
function of camera-air temperature difference. Finally, after comparing with the corresponding error budget term, a
maximum allowable temperature for the camera is selected.
KEYWORDS: Telescopes, Convection, Finite element methods, Thermal modeling, Thermal analysis, Space telescopes, Electronics, Control systems, Systems modeling, Thirty Meter Telescope
Thermal analysis for the Thirty Meter Telescope (TMT) structure was performed using finite element analysis in
ANSYS and I-DEAS. In the thermal analysis, the telescope structural parts with simplified optical assembly systems
were modeled for various thermal conditions including air convections, conductions, heat flux loadings, and radiations.
Thermal responses of the TMT telescope structure were predicted and the temperature distributions of the optical
assembly systems were calculated under sample thermal loading conditions. The thermo-elastic analysis was made to
obtain the thermal deformation based on the resulting temperature distributions. The line of sight calculation was made
using the thermally induced structural deformations. The goal of this thermal analysis is to establish thermal models by
the FEA programs to simulate for an adequate thermal environment. These thermal models can be utilized for estimating
the thermal responses of the TMT structure. Thermal performance prediction of the TMT structure will be able to guide
us to control and maintain the system from the "seeing" effects.
Thermal analysis for the Thirty Meter Telescope (TMT) optics (the primary mirror segment, the secondary mirror, and
the tertiary mirror) was performed using finite element analysis in ANSYS and I-DEAS. In the thermal analysis, each of
the optical assemblies (mirror, mirror supports, cell) was modeled for various thermal conditions including air
convections, conductions, heat flux loadings, and radiations. The thermal time constant of each mirror was estimated
and the temperature distributions of the mirror assemblies were calculated under the various thermal loading conditions.
The thermo-elastic analysis was made to obtain the thermal deformation based on the resulting temperature distributions.
The optical performance of the TMT optics was evaluated from the thermally induced mirror deformations. The goal of
this thermal analysis is to establish thermal models by the FEA programs to simulate for an adequate thermal
environment. These thermal models can be utilized for estimating the thermal responses of the TMT optics. In order to
demonstrate the thermal responses, various sample time-dependent thermal loadings were modeled to synthesize the
operational environment. Thermal responses of the optics were discussed and the optical consequences were evaluated.
KEYWORDS: Telescopes, 3D modeling, Finite element methods, Systems modeling, Buildings, Fluctuations and noise, Motion models, Astronomical telescopes, Astronomy, Thirty Meter Telescope
Telescope-Enclosure-Soil Interaction could result in additional telescope movement due to two main sources: (i)
enclosure windshake and (ii) vibrations of machinery located at enclosure, summit and utility facilities. To analyze and
minimize these vibrations, a novel FE model was developed based on existing FE models for the TMT enclosure and
telescope structures. This integrated structural model adequately represents propagation of vibrations from the source to
the telescope structure through surrounding soil/rock region. The model employs 3-D linear-elastic harmonic analysis
using commercial FE code ANSYS. Special attention was devoted to adequate modeling of reflecting and non-reflecting
boundary conditions. Based on the FE model developed, we examined the effects of soil/rock stiffness and damping
upon telescope vibrations and, ultimately, seeing quality. The effects of location, intensity and spectral content of main
sources of machinery vibrations were also investigated.
The Thirty Meter Telescope (TMT) project has been collecting data on five candidate sites since 2003. This paper
describes the site testing portion of the TMT site selection program and the process and standards employed
by it. This includes descriptions of the candidate sites, the process by which they were identified, the site
characterization instrument suite and its calibration and the available results, which will be published shortly.
KEYWORDS: Mirrors, Telescopes, Modulation transfer functions, Domes, Monte Carlo methods, Refraction, Systems modeling, Wavefronts, Thermal modeling, Thirty Meter Telescope
Mirror and dome seeing are critical effects influencing the optical performance of ground based telescopes. The Thirty
Meter Telescope project has been utilizing a combination of optical simulations and Computational Fluid Dynamics to
model the dome and mirror seeing. A set of optical modeling tools has been developed in MATLAB to post-process high
spatial resolution thermal CFD results and calculate image degradation due to dome seeing and mirror seeing. The same
tools can provide the distribution of seeing contribution along optical path in order to recognize potential problems and
guide the observatory design. The method, including limiting assumptions for the optical modeling tools are discussed.
KEYWORDS: Telescopes, Monte Carlo methods, Mirrors, Systems modeling, Performance modeling, Thermal modeling, Error analysis, Observatories, Temperature metrology, Thirty Meter Telescope
This presentation describes a strategy for assessing the performance of the Thirty Meter Telescope (TMT). A Monte
Carlo Simulation Framework has been developed to combine optical modeling with Computational Fluid Dynamics
simulations (CFD), Finite Element Analysis (FEA) and controls to model the overall performance of TMT.
The framework consists of a two year record of observed environmental parameters such as atmospheric seeing, site
wind speed and direction, ambient temperature and local sunset and sunrise times, along with telescope azimuth and
elevation with a given sampling rate. The modeled optical, dynamic and thermal seeing aberrations are available in a
matrix form for distinct values within the range of influencing parameters. These parameters are either part of the
framework parameter set or can be derived from them at each time-step. As time advances, the aberrations are
interpolated and combined based on the current value of their parameters. Different scenarios can be generated based on
operating parameters such as venting strategy, optical calibration frequency and heat source control.
Performance probability distributions are obtained and provide design guidance. The sensitivity of the system to design,
operating and environmental parameters can be assessed in order to maximize the % of time the system meets the
performance specifications.
A large ground-based astronomical telescope project, like the Thirty Meter Telescope (TMT), is rivaling space projects
in technical complexity, design and construction time span, budget, as well as organizational diversity and geographical
distribution. A unique challenge in large ground based projects is implementing appropriate systems engineering
methods and tools in the absence of the strong institutional backdrop that space projects can rely on. This paper provides
a critical overview of the established system engineering practice in the TMT project, including requirements
engineering, document and configuration control, as well as performance allocation and estimation. In particular, we
introduce a new performance metric, the Point Source Sensitivity (PSS), and show how it is superior to the 80%
enclosed energy diameter measure. The overall strategy for estimating the performance of TMT is outlined, showing
how the various elements of performance modeling, reported in detail in other papers, fit together to provide a
probabilistic assessment of the achievable image quality of the observatory. An overview of the estimated system
performance is presented with critical analysis of the major factors limiting the seeing limited observations.
The performance requirements of the Thirty Meter Telescope (TMT) dictate, among others, a thorough understanding of
the flow field inside and around the observatory. Mirror and dome seeing as well as dynamic wind loading on the optics,
telescope structure and enclosure constitute significant sources of image degradation. A summary of the current status of
Computational Fluid Dynamics (CFD) simulations for TMT is presented, with special attention given to the choice of
thermal boundary conditions.
Detailed simulations of the mirror support assemblies determine the direction of heat flow from important heat sources
and provide feedback to the design. They also provide estimates of the heat transfer coefficients for the solid thermal
models.
A transient radiation model has also been developed for the enclosure and telescope surfaces in order to estimate the heat
flux exchange with the air volume. It also provides estimates of the effective emissivity for the solid thermal models.
Finally, a complete model of the observatory on a candidate summit is used to calculate air velocity, pressure and
temperature for a matrix of given telescope orientations and enclosure configurations. Calculated wind velocity spectra
above M1 and around M2 as well as the wind force on the enclosure are used as inputs in the TMT integrated dynamic
model. The temperature and flux output of the aforementioned thermal models are used as input surface boundary
conditions in the CFD model. Generated records of temperature variations inside the air volume of the optical paths are
fed into the TMT thermal seeing model.
Mirror and dome seeing are critical effects influencing the optical performance of large ground based telescopes. Computational Fluid Dynamics (CFD) and optical models that simulate mirror seeing in the Thirty Meter Telescope (TMT) are presented. The optical model used to quantify the effects of seeing utilizes the spatially varying refractive index resulting from the expected theoretical flow field, while the developed CFD post-processing model estimates the corresponding CN2 distribution. The seeing effects corresponding to a flat plate are calculated. Plots of seeing versus different temperature differences, velocities and plate lengths are generated. The discussion presented contains comparisons of the results from the two models with published empirical relations.
We present a study of the impact of short term variations (up to hours) of the physical conditions at a site on the atmospheric seeing conditions. This study includes ground layer seeing estimates through the use of computational fluid dynamics (CFD) simulations as well as observational data originating from the site testing program of the Thirty-Meter-Telescope (TMT). We discuss a case scenario and compare this and general trends to the CFD predictions.
The Thirty Meter Telescope project is designing a 30m diameter ground-based optical telescope. Unsteady wind loads on the telescope structure due to turbulence inside the telescope enclosure impact the delivered image quality. A parametric model is described that predicts the optical performance due to wind with sufficient accuracy to inform relevant design decisions, including control bandwidths. The model is designed to be sufficiently computationally efficient to allow rapid exploration of the impact of design parameters or uncertain/variable input parameters, and includes (i) a parametric wind model, (ii) a detailed structural dynamic model derived from a finite element model, (iii) a linear optical response model, and (iv) a control model. Model predictions with the TMT structural design are presented, including the parametric variation of performance with external wind speed, desired wind speed across the primary mirror, and optical guide loop bandwidth. For the median
mountaintop wind speed of 5.5 m/s, the combination of dome shielding, minimized cross-sectional area, and control results in acceptable image degradation.
Mirror and dome seeing greatly influence the optical performance of large ground-based telescopes. This study describes
a strategy for modeling the effects of passive ventilation on the optical performance of the Thirty Meter Telescope
(TMT). Computational Fluid Dynamic (CFD) analyses are combined with thermal analyses to model the effects of
turbulence and thermal variations within the airflow around the TMT telescope-enclosure configuration. An analytical
thermal model based on Newton's cooling law and incorporating a conduction heat flux and a radiation term is used to
track the primary mirror temperature throughout the night. A semi-empirical seeing model is used to relate mirror
temperature and wind speed to seeing. Different external wind speeds, mirror heat fluxes and ambient thermal temporal
gradients are investigated and comparisons are made.
KEYWORDS: Mirrors, Telescopes, Turbulence, Space telescopes, Optical instrument design, Systems modeling, Performance modeling, Secondary tip-tilt mirrors, Wind measurement, Control systems
A parametric model of the dynamic performance of an optical telescope
due to wind-buffeting is presented. The model is being developed to
support the design of next generation segmented-mirror optical telescopes through enabling rapid design iterations and allowing a more thorough exploration of the design space. A realistic performance assessment requires parametric descriptions of the wind, the structural dynamics, active control of the structure, and the optical response. The current model and its assumptions are presented, with the primary emphasis being on the parameterization of the wind forces. Understanding the temporal spectrum and spatial distribution of wind disturbances inside the telescope enclosure is one of the most challenging aspects in developing the overall parametric model. This involves integrating information from wind tunnel tests, computational fluid dynamics, and measurements at existing observatories. The potential and limitations of control to mitigate the response are also discussed, with realistic constraints on the control bandwidth obtained from the detailed structural model of a particular point design. Finally, initial results are presented on performance trends with a few key parameter variations.
A sound system engineering approach and the appropriate tools to support it are essential in achieving the scientific and financial objectives of the Thirty Meter Telescope project. Major elements of the required tool set are those providing estimates for the performance of the telescope. During the last couple of years, the partners in the consortium developed a wide range of modeling and simulation tools with various levels of fidelity and flexibility. There are models available for time domain and frequency domain simulations and analysis, as well as for lower fidelity, parametric investigations of design trade-offs and for high fidelity, integrated modeling of structure, optics and control. Presented are characteristic simulation results using the existing preliminary point designs of the TMT, with emphasis on the telescope performance degradation due to wind buffeting. Under the conditions modeled, the wind induced image jitter and image quality degradation was found comparable to good atmospheric seeing.
KEYWORDS: Telescopes, Mirrors, Finite element methods, Large telescopes, Integrated modeling, Space telescopes, Systems modeling, Computational fluid dynamics, Integrated optics, Thirty Meter Telescope
Wind loading is one of the critical parameters influencing the performance of large telescopes, with potentially more dramatic consequences for proposed future giant telescopes. This study describes a strategy for modeling the effects of wind loading on extremely large telescopes such as the Thirty Meter Telescope (TMT). The optical performance of the telescope is estimated by an integrated model, which incorporates the telescope structure, optics, and control. To model the dynamic force variation on the telescope, a Finite Element Analysis (FEA) model of the telescope is created along with an unsteady Computational Fluid Dynamics (CFD) model of the airflow around the enclosure-telescope configuration, which should have a suitable level of geometric fidelity. Numerical simulations using the CFD model are performed for a chosen wind speed and telescope orientation (azimuth, zenith), through which the dynamic force pattern on the primary and secondary mirrors as well as on the secondary support structure can be determined. Finally the force pattern is applied to the FEA model. This can be achieved either by applying temporally and spatially filtered white noise forces with random distribution deducted from the CFD analysis, or by considering the dynamic force pattern itself from the unsteady CFD calculations. Since the FEA and CFD models usually have different resolution requirements and consequently different, non-uniform spatial sampling grids, a key part of the interface is the conversions necessary to transfer the forces from CFD surface cells to structural nodes.
Numerical simulations of airflow over various potential sites for extremely large telescopes have been performed. Information such as wind speed, turbulence levels (fluctuating velocity RMS), wake lengths, boundary (ground) layer thickness and the effects of topographically induced turbulence on "seeing" can be retrieved, thus providing an essential evaluation tool in the site selection process. We present a sample set of simulations carried out over possible site locations for a 20-30m-telescope project. Simulations at several different sites located in Chile were performed in terms of wind speed levels and the effects of the local topographic features on the flow in the summit region, namely turbulent intensity and boundary layer thickness, under the prevailing wind conditions. Results indicate that the turbulent boundary layer thickness, defined as the region of considerable turbulent intensity levels, ranges from 10m to ~400m, depending on peak location and wind direction, for summit wind speeds varying between 4 and 12 m/s.
Computational fluid dynamics (CFD) can provide critical information in the design of enclosures for extremely large telescopes (ELTs). The issues of air exchange, dome "seeing," wind loading on telescope structures, and structurally induced turbulence can all be addressed by CFD calculations at a small fraction of the cost and effort required to obtain similar information from wind or water tunnel tests. Information of these and other enclosure and dome "seeing" issues are essential in establishing effective enclosure designs and in implementing integrated models that will optimize telescope performance. In this presentation we provide sample results from a preliminary reconnaissance of some representative enclosure designs under a variety of initial conditions. In particular, results will be shown for a nominal ELT enclosure of 90 m diameter and for the enclosure used for the Gemini South telescope. Both designs were evaluated under a variety of operating conditions that include different venting conditions, telescope zenith angle, and relative wind direction.
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