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Conference 13099
Modeling, Systems Engineering, and Project Management for Astronomy XI
16 - 18 June 2024 | Room G312, North - 3F
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Session 1:
Integrated and Optics Modelling I
16 June 2024 • 08:30 - 10:10 Japan Standard Time | Room G312, North - 3F
Session Chairs:
Scott C. Roberts, NRC-Herzberg Astronomy & Astrophysics (Canada), Sébastien Elias Egner, European Southern Observatory (Germany)
13099-1
16 June 2024 • 08:30 - 08:50 Japan Standard Time | Room G312, North - 3F
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Lentil is a Python package for developing high-performance diffraction simulations. Lentil provides a framework for modeling wave propagation of light through optical systems. Unlike traditional Fourier optics approaches relying on the Fast Fourier Transform (FFT), Lentil evaluates the Discrete Fourier Transform (DFT) directly to numerically model diffraction. This approach improves computational efficiency and reduces memory usage, particularly when modeling large apertures, highly misaligned or aberrated systems, or small features demanding fine sampling. Lentil offers generalized diffraction propagation routines using the DFT that improve simulation performance substantially, with additional optimizations for modeling segmented apertures. Lentil also implements a hybrid propagation algorithm blending physical and geometric optics, improving performance in simulations where representing large tilts is required. Additionally, Lentil includes tools for modeling wavefront errors, radiometry, and focal plane arrays. Lentil is freely available as open-source software.
13099-2
16 June 2024 • 08:50 - 09:10 Japan Standard Time | Room G312, North - 3F
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The Mid-infrared ELT Imager and Spectrograph (METIS) is one of the first-light scientific instruments for the ELT with over 75 optical components. The science cases of METIS impose tight stability requirements on the optical performance. To assess whether the optical performance is harmed by micro-vibrations, the effect of numerous vibration sources on the optical stability are analyzed. We present the analysis approach and results for METIS. This includes finite element analysis to obtain transfer functions, compute rigid body motion response of optical elements and assess the optical impact by ray-tracing.
13099-3
16 June 2024 • 09:10 - 09:30 Japan Standard Time | Room G312, North - 3F
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Pyxel is an opensource python-based framework to simulate images including instrumental effects with a focus on detector modelling (CCDs & EM-CCDS, CIS, Hybrid-CMOS, APDs, MKIDs etc.). Right from the start of its development at ESA, Pyxel has been conceived to easily integrate and pipeline models from different contributors and in this way foster collaboration in the instrumentation community. We give an overview of the framework focusing on the main improvements and evolution since v1.0 and examples of new features. On top of the many models that were added to the framework, the pipeline hosts now to two new model groups “scene generation” and “data processing” to make the framework even more self-consistent.
13099-4
16 June 2024 • 09:30 - 09:50 Japan Standard Time | Room G312, North - 3F
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We present our numerical simulation approach for the End-to-End (E2E) model applied to various astronomical spectrographs, such as SOXS (ESO-NTT), CUBES (ESO-VLT), and ANDES (ESO-ELT), covering multiple wavelength regions. The E2E model aim at simulating the expected astronomical observations starting from the radiation of the scientific sources (or calibration sources) up to the raw-frame data produced by the detectors. The comprehensive description includes E2E architecture, computational models, and tools for rendering the simulated frames. Collaboration with Data Reduction Software (DRS) teams is discussed, along with efforts to meet instrument requirements. The contribution to the cross-correlation algorithm for the Active Flexure Compensation (AFC) system of CUBES is detailed.
13099-5
16 June 2024 • 09:50 - 10:10 Japan Standard Time | Room G312, North - 3F
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HARMONI is the first light visible and near-IR integral field spectrograph for the ELT. It covers a large spectral range from 470 nm to 2450 nm with resolving powers from 3300 to 18000 and spatial sampling from 60 mas to 4 mas. It can operate in two Adaptive Optics modes - SCAO (including a High Contrast capability) and LTAO - or with NOAO.
To model the optical performance we include manufacturing and alignment tolerances alongside other static and dynamic effects. Diffraction of both image and pupil become significant when the spectrograph slit width matches the diffraction limited point spread function. A set of Zemax OpticStudio macros and Python scripts are used to bring together the subsystem models that make up HARMONI and combine them to include all these effects.
We present an overview of our approach to modelling this complex instrument and key results predicting the optical performance of HARMONI.
Break
Coffee Break 10:10 - 10:40
Session 2:
Project Management
16 June 2024 • 10:40 - 12:20 Japan Standard Time | Room G312, North - 3F
Session Chairs:
Takeshi Okuda, Joint ALMA Observatory (Japan), Melissa Archuleta, National Radio Astronomy Observatory (United States)
13099-6
16 June 2024 • 10:40 - 11:00 Japan Standard Time | Room G312, North - 3F
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The Mid-infrared ELT Imager and Spectrograph (METIS) is one of the four first-light scientific instruments for the Extremely Large Telescope (ELT) and is designed and built by a consortium of 13 partners, including ESO, and led by NOVA in the Netherlands. The project is now in its manufacturing, assembly, integration and test phase (MAIT).
The METIS project is bigger and more complex than previous VLT projects which has increased the number of management challenges. This paper presents the management organization of METIS and it discusses various lessons learned and the plans for the phases to come.
13099-7
16 June 2024 • 11:00 - 11:20 Japan Standard Time | Room G312, North - 3F
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The Advanced Instrumentation Technology Centre (AITC) at the Australian National University (ANU) is the largest instrumentation research, design and development facility for astronomy and space in Australia with a track record spanning decades of expertise in those fields. The ANU AITC is also part of the Astralis Instrumentation Consortium. At the AITC, we combine our extensive knowledge and expertise in optics, mechanics, electronics, detectors, control, software, astronomy, and space technologies to design and build cutting edge instruments for customers around the world.
This paper presents the operating model that the AITC has developed to manage its complex and diverse project portfolio. The model integrates the AITC’s project management, system engineering and product assurance frameworks, and combines them with the AITC quality management structure. Some examples of issues addressed over the past 4 years are presented, as well as the strengths and challenges uncovered by a recent independent review of the AITC operational procedures by ANU Enterprise.
13099-8
16 June 2024 • 11:20 - 11:40 Japan Standard Time | Room G312, North - 3F
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The Astralis Instrumentation Consortium (Astralis) provides Australia’s national capability for optical astronomy instrumentation by combining expertise and resources from the Australian National University, Macquarie University and University of Sydney. Established in 2018 with support from Astronomy Australia Ltd. (AAL), Astralis has been in operation for over 5 years, and has been building instruments for the world’s largest telescopes.
Here we present our review of the first five years of Astralis, including the benefits of building instruments in a national wide consortium environment, the challenges we have overcome, and the future of the Consortium.
13099-9
16 June 2024 • 11:40 - 12:00 Japan Standard Time | Room G312, North - 3F
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Gemini Observatory conducted a technical assessment and feasibility study for the GLASS Implementation Feasibility Study 2020 project. The study aimed to improve image quality and telescope efficiency and determine cost-effectiveness. The paper outlines the project management and systems engineering structure that will be implemented to integrate the GLASS into the facility. A robust systems engineering and project management foundation is crucial due to the project's technical complexity and resource constraints.
13099-10
16 June 2024 • 12:00 - 12:20 Japan Standard Time | Room G312, North - 3F
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The Atacama Large Millimeter/submillimeter Array (ALMA) is the world’s leading millimeter/submillimeter observatory. This paper presents: a) a history of the establishment of the ALMA 2030 Development Roadmap; b) a brief description of the Wideband Sensitivity Upgrade (WSU) project, the first of the ALMA 2030 development program, and how the WSU system is being defined; c) how the contributions from the ALMA partnership are developing the WSU ; and d) the challenges, both technical and programmatic, of managing a massive development project as part of the existing development program, while at the same time keeping the operation of the observatory.
Break
Lunch Break 12:20 - 13:40
Session 3:
Systems Engineering Methods
16 June 2024 • 13:40 - 15:20 Japan Standard Time | Room G312, North - 3F
13099-11
16 June 2024 • 13:40 - 14:00 Japan Standard Time | Room G312, North - 3F
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The technologies in the eXtended Reality (XR) field have been rapidly developing in the last few years, allowing for their effective implementation in many different applications.
This paper studies the integration of virtual and mixed reality elements in a concurrent engineering environment. More specifically, eXtended Reality tools will be employed in the Concurrent Design Facility that is being developed at the Capodimonte Astronomical Observatory in Naples, in the scope of the National Recovery and Resilience Plan project "STILES - Strengthening the Italian leadership in ELT and SKA".
The XR environment will aid in the definition of the design, allowing the participants of a concurrent engineering session to inspect and manipulate complex 3D models, enabling detailed examinations of components, interfaces and potential issues. This immersive experience helps to identify design flaws and possible criticalities during various phases of the instrument life.
The best way to properly integrate these tools in the design process, with the aim of effectively supporting the concurrent approach philosophy of effort and time efficiency is under study.
13099-12
16 June 2024 • 14:00 - 14:20 Japan Standard Time | Room G312, North - 3F
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Digitally supported Systems Engineering, or Model Based Systems Engineering (MBSE) methodologies usage in full scale space science missions development in Europe is so far limited to a few cases and several factors limit a wider adoption: from lack of clear methodology, to limitations in tooling, to lack of clarity on contractual aspects.
To tackle some of these limitations, a progressive implementation of MBSE practices in Science missions at the European Space Agency has been adopted, starting with the Euclid mission and continued with PLATO and ARIEL. We present an assessment of the experience in the PLATO mission with the usage of two main MBSE approaches: i) SysML model and ii) a Mission Parameters Database used for all performance and pipeline development. We review the lessons learned from the experience in Euclid, and the implementation in PLATO, and identify areas for development to reach standardization of practices in Europe.
13099-13
16 June 2024 • 14:20 - 14:40 Japan Standard Time | Room G312, North - 3F
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The Thirty Meter Telescope project involves complex systems engineering, necessitating efficient tools for the effective management of SE processes and products. This paper explores the utilization of Atlassian Jira whose flexibility surpasses traditional methods like Excel by providing a common, collaborative database for all stakeholders, enabling concurrent updates and facilitating easy search, filter, and reporting capabilities.
This paper details the incorporation of processes for task tracking, verification, risk management, hazard assessment, CAD issue tracking, and configuration management into Jira. Establishing traceability between related tickets fosters small group and system-wide collaboration, and ensures that important information is not lost, forgotten, or incorrectly duplicated.
Customizing Jira and optimizing its features has contributed to efficient management of TMT systems engineering processes and products. Leveraging its functionalities, we have fostered a more robust and traceable design by enhancing collaboration through greater transparency and accessibility. Jira has proven to be a valuable asset in the comprehensive management of complex projects.
13099-14
16 June 2024 • 14:40 - 15:00 Japan Standard Time | Room G312, North - 3F
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In this paper we will make a revision of the usage of MBSE for an astronomy-oriented instrument. We will in particular trade the benefit Versus the overhead with respect of the traditional System engineering method.
We will compare different ground-based instruments for different telescope size in different project phases. We will try then to underline where MBSE have been useful and where the criticalities of this method emerged in order to draw a possible roadmap to exploit the maximum benefit achievable by this method.
In detail we will focus on four main aspects. In the first part We will compare different requirement management approaches. Second, we will focus on the Interface management which is one of the most critical elements of the system engineering discipline. We will then compare the product traditional product modelling (excel based) with respect to a database oriented one. Finally, we will assess the use cases management. We will compare traditional Versus MBSE in order to allow the reader to identify which of the two approaches better fits with its needs.
13099-15
16 June 2024 • 15:00 - 15:20 Japan Standard Time | Room G312, North - 3F
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Lately, the Italian astronomical community has begun the transition to MBSE. This tool has been largely applied to the development of the Cassegrain U-Band Efficient Spectrograph (CUBES) designed to provide high instrumental efficiency ( > 37%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral resolving power of R > 20, 000 (with a lower-resolution, sky-limited mode of R ∼ 7, 000). Here, MBSE has been used in 3 areas: requirements management, activities modeling, and generation of system structure documents, like PBS or BoM.
Requirements management controls the flow-down process to have a coherent list of requirements. This is achieved using derived properties and tailored numbering.
Activities modeling uses traditional MBSE techniques while mimicking the software templates for calibration and observation.
To generate system structure documents, the system structure is generated in Cameo using the outputs from the subsystems, granting high coherency between the model and the actual design state.
The interaction with non-Cameo users relies on Excel files, accessible to all interested parties and usable by Cameo to export and import information.
Break
Coffee Break 15:20 - 15:50
Session 4:
Systems Engineering Management I
16 June 2024 • 15:50 - 17:30 Japan Standard Time | Room G312, North - 3F
13099-16
16 June 2024 • 15:50 - 16:10 Japan Standard Time | Room G312, North - 3F
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We reached the 20-year anniversary of this forum. At the onset of the third decade, we will see a new generation of extremely large telescopes with their extremely large instruments and the correspondently largest challenges ever encountered in our field: constructing and operating these machines to discover celestial objects that are unreachable today. The excitement is not only for the astronomers. Rigorous, proven and efficient system engineering and project management are the pre-requisites to build such discovery machines. Our community will be asked to address a new range of problems and provide elegant sustainable solutions. This paper reviews the past 20-years of papers at this conference to assess how successful we have been in formalizing our development processes, and whether these formalized life-cycle models and methodologies have delivered the value added we hoped for. Our survey has revealed design and management trends and also highlighted possible shortages and gaps in the current practices. Our goal is to build a bridge between current models and practices and propose new methodologies and processes which can support the research ambitions of future astronomers.
13099-17
16 June 2024 • 16:10 - 16:30 Japan Standard Time | Room G312, North - 3F
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This paper will describe how we have tailored the standard systems engineering approaches taken for space instrumentation and implemented these in the large consortium structure needed for the Ariel mission payload development. This has been done in order to try to maximise the efficiency of the consortium work and to allow as close to a seamless flow of information as possible. Through working together over the eight years of the project so far, and through the previous experience in the teams of working in such a consortium, many methodologies and techniques have been developed and iterated to allow robust yet pragmatic management of the organization.
We will outline the key tools being deployed by the payload management, systems engineering and product assurance teams in the consortium. These tailored tools include those for capturing all product documentation, action item tracking, review management, engineering parameter tracking, requirements and verification management, product assurance key information and for project management information capture. We will also detail the methods for communication and coordination between the consortium team and the ESA team.
13099-18
16 June 2024 • 16:30 - 16:50 Japan Standard Time | Room G312, North - 3F
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The ELT construction programme reached a few months ago the 50% completion in terms of earned value. The detailed design phase of the ELT is being finalized and many subsystems are already under construction (some close to be delivered to ESO). However, as part of the final design consolidation, there was still room for optimizing the diffraction-limited performance of the telescope. This paper presents several system-level activities that have been undertaken with this goal in mind and describes the objectives, the work done, as well as the results that have been obtained so far.
13099-19
16 June 2024 • 16:50 - 17:10 Japan Standard Time | Room G312, North - 3F
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The ELT Phasing and Diagnostic Station (PDS), is a challenging multi-purpose opto-mechanical system providing metrology tools to phase the gigantic segmented primary mirror of the ELT and hosting the sensors required to verify Adaptive Optics assisted diffraction limited image quality at the ELT. The project, which is one of the most important internal development endeavors at ESO, has undergone a major restructuring in early 2021 before starting its final design phase which has been successfully completed in 2023. In the same period all procurement activities concerning critical long lead items have been launched.
The present contribution first introduces the project in the context of the ELT construction program, outlining the new project structure and the project management tools employed for planning and progress monitoring. Subsequently, the main system engineering processes used within the project will be described. Finally, the paper reports on the main technical results obtained during the final design phase and the plans for the assembly, integration and test of the system.
13099-20
16 June 2024 • 17:10 - 17:30 Japan Standard Time | Room G312, North - 3F
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ANDES is a high-resolution spectrograph for the ELT that will explore various scientific topics. We used the MBSE approach with the Cameo Systems Modeler tool to design the instrument during the Phase B-One, which ended with the SAR in 2023. We created a system model that helped us with requirements, interfaces, verification, validation, and trade-off analysis. We also developed a standard of procedures for the MBSE methodology in the astronomical field, which can be useful for future instruments. We share our benefits, challenges, lessons, and best practices of using MBSE for ANDES.
Monday Plenary Session
17 June 2024 • 08:30 - 10:00 Japan Standard Time | National Convention Hall, 1F
Join us for the Monday morning plenary talks.
Break
Coffee Break 10:00 - 10:30
Session 5:
Series Production/Information and Configuration and Quality Management
17 June 2024 • 10:30 - 12:30 Japan Standard Time | Room G312, North - 3F
Session Chairs:
Masahiro Sugimoto, National Astronomical Observatory of Japan (Japan), Gerhard Pieter Swart, SKA Observatory (United Kingdom)
13099-22
17 June 2024 • 10:50 - 11:10 Japan Standard Time | Room G312, North - 3F
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Within the ESA PLATO M3 mission, the Telescope Optical Unit (TOU) is the opto-mechanical unit, is a fully refractive optical system. The 26 TOU Flight Models and 5 spares to be delivered to the upper level, the PLATO Camera, make it a serial production for TOUs. The First Flight Models (FM) production faced many initial challenges from a Product Assurance point of view related to MAIV activities, while moving forward these challenges decreased. Discrepancies and non-conformities associated with, mainly, but not only, materials and processes, cleanliness and contamination control, safety, qualifications/validations will be the object of this proceeding. Thus, showing that serial production adds one more variable to possible failures, but at the same time, when root causes are corrected and solved, yields less difficulties in subsequent FMs MAIV.
13099-23
17 June 2024 • 11:10 - 11:30 Japan Standard Time | Room G312, North - 3F
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The Vera C. Rubin Observatory is one of the first observatories to apply Model-Based Systems Engineering in all major aspects of the project. This paper describes the evolution of the processes, methodologies and tools developed and utilized by the Rubin Observatory Team. It specifically focuses on the Rubin Systems Engineering Processes for Image Quality tracking, Computerized Maintenance Management System (CMMS) selection, Failure Reporting, Analysis, Corrective Action System (FRACAS) handling, and Hazard Mitigation Analysis. Here, we share updates on each topic’s workflows, experiences, and difficulties with the community.
13099-24
17 June 2024 • 11:30 - 11:50 Japan Standard Time | Room G312, North - 3F
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For the ELT, a total of 931 M1 Segment Assemblies will be manufactured. These will be of 133 different types, 7 copies each, with different optical and mechanical properties. The manufacturing of the segment support, the glass blank and the polishing will be done by industrial partners. ESO will be responsible for the shipment of the Segment Assemblies to Chile, for the integration of the edge sensors and their electronics, and for the cleaning and coating. After performing several health- and quality-checks, the Segment Assemblies will be temporarily stored in the warehouse, before being installed at the telescope and eventually recoated around every 2 years. The telescopes and instruments for optical astronomy are usually prototypes, while a new approach is required to manage such a series production of crucial components, which differ in small but significant aspects. In this paper, we will present the processes we have developed to manage to manage the series production of M1 Segment Assemblies for the ELT, starting from the reception of the Segment Assemblies in Chile, inspection, installation of sub-components, health-checks, storage and installation at the telescope.
13099-25
A comprehensive trade study of asset and maintenance management tools for the Thirty Meter Telescope
17 June 2024 • 11:50 - 12:10 Japan Standard Time | Room G312, North - 3F
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Controlling work processes and inventories at the Thirty Meter Telescope (TMT) is an important function to ensure there is minimal impact to nighttime operations due to downtime or hardware failures. Whilst telescopes such as the TMT are complex machines, tools used to control assets and maintenance activities should not be. The purpose of such a tool should be to guarantee successful outcomes via efficient inputs. We share our method for determining the criteria and tool selection for TMT’s management of assets, inventory, and maintenance activities. Our proposed method integrates technical, functional, and organizational elements that factored into the weightings. The application of a weighted score system enables quantitative comparison between each possibility, ensuring the selected tool meets the needs of TMT, thus maximizing the benefits provided by an effective maintenance management tool.
13099-26
17 June 2024 • 12:10 - 12:30 Japan Standard Time | Room G312, North - 3F
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MOSAIC is a second-generation ELT (Extremely Large Telescope) instrument. The instrument has started phase B, and apart from technical and financial requirements, MOSAIC has the additional requirement to investigate and minimise its environmental impact. The first step is to estimate the carbon footprint (and other effects) in a ‘Life Cycle Cost and Sustainability Analysis’, for the instrument development up to Preliminary Acceptance in Chili. This paper presents such an estimate.
Break
Lunch Break 12:30 - 13:40
Session 6:
Modeling as a Driver of Observatory Design - Joint Session with AS103 and AS108
17 June 2024 • 13:40 - 17:30 Japan Standard Time | Room G219, North - 2F
Session Chairs:
Breann N. Sitarski, NASA Goddard Space Flight Ctr. (United States), Bernhard Lopez, Cherenkov Telescope Array Observatory gGmbH (Germany)
13094-23
17 June 2024 • 13:40 - 14:00 Japan Standard Time | Room G219, North - 2F
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The authors describe the Giant Magellan Telescope CO2-based refrigeration system used to thermally condition the 8.4-meter diameter borosilicate primary mirror segments. The thermal control architecture, the motivations for specific design choices, and the associated control strategies are discussed in detail. The work presented here is part of an effort to build a full-scale prototype mirror cell into which a mirror segment will soon be installed and optically tested at the Richard F. Caris Mirror Lab on the campus of the University of Arizona.
13094-25
17 June 2024 • 14:20 - 14:40 Japan Standard Time | Room G219, North - 2F
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The National Science Foundation’s Daniel K. Inouye Solar Telescope (DKIST) is the largest solar telescope in the world, utilizing a 4-m off-axis primary mirror. The resulting mount size, long optical pathways, various moving components, and complex thermal design leaves DKIST with a very tight optical error budget that is susceptible to vibration-related degradation. There has been an ongoing survey to identify and address vibration sources affecting the optical path of the telescope during DKIST construction and operations. Improvements in this effort within the last year have enabled us to distinguish and categorize several vibration sources, in order to prioritize solutions for those with the highest impact on image motion. Presented herein are recent examples of sources with significant impact, including the details on how we tracked and identified them, and the solutions that were implemented in order to reduce jitter. As DKIST continues operations, future vibration mitigation efforts will be supported by additional data from other instruments in order to identify opportunities for optimization and further isolate localized vibration within our optics systems.
13094-26
17 June 2024 • 14:40 - 15:00 Japan Standard Time | Room G219, North - 2F
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External environmental conditions lead to thermal deformations of the primary reflector of the 50-m diameter Large Millimeter Telescope Alfonso Serrano (LMT). This paper describes efforts to improve the night-time performance of the telescope at millimeter-wavelengths and allow extension of scientific observations into daylight hours, using the LMT's active surface to counteract the effects of thermal gradients within the antenna structure. Several approaches to stabilizing the LMT’s thermal behavior will be described, including operation of a ventilation system in the antenna backup structure and a real-time metrology system to measure and correct large-scale, thermally induced, surface deformations.
13094-27
17 June 2024 • 15:00 - 15:20 Japan Standard Time | Room G219, North - 2F
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CFD and conjugate heat transfer models have been developed and/or updated to validate thermal requirements for the TMT enclosure HVAC system, azimuth and cap drive systems, interstitial space volume, as well as the Summit Facilities tunnel, mechanical room, utility room, and chiller exhaust. The resulting thermal environment is assessed and linked to performance, wherever applicable.
13094-28
17 June 2024 • 15:20 - 15:40 Japan Standard Time | Room G219, North - 2F
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The Dominion Radio Astrophysical Observatory’s John A. Galt 26 m radio telescope serves multiple roles for the Canadian radio astronomy community. The attributes of this telescope make it ideal for spectropolarimetric studies of the interstellar medium, however instrumental conversion of unpolarized radiation into a polarized signal can corrupt the astronomical signal as the telescope undergoes various loading conditions.
To characterize these effects, a finite element (FE) model of the telescope was constructed, based on available blueprints and supplemented by manual measurements. To validate this FE model, vibration measurements were conducted over four days in September 2022 by NRC-Herzberg engineers. The telescope was instrumented with accelerometers, and vibrations were excited using the step-release and impulse hammer methods. This paper will briefly review the model development and analytical predictions, will describe the instrumentation plan and experimental approach used, and will summarize key results from these tests, in particular the first several vibration modes of the telescope.
Coffee Break 15:40 - 16:10
13099-27
17 June 2024 • 16:10 - 16:30 Japan Standard Time | Room G219, North - 2F
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The European Solar Telescope (EST), based on a Gregorian on-axis 4.2-meter solar telescope, will be part of the next generation of large aperture solar telescopes.
Due to the open-dome configuration of EST, the primary and secondary mirrors will be directly exposed to ambient conditions, which means that, during operation, the active optics system is crucial to counteract the effect of thermal loads and wind low frequency fluctuations. The correction of misalignments arising from gravity loads, primary mirror figure errors and other potential low order wavefront errors is also within the scope of this system.
This contribution describes the status of the active optics system of EST at the Preliminary Design Phase and demonstrates the feasibility of the strategy, which considers as active compensators M1, M2 and M3.
13099-28
17 June 2024 • 16:30 - 16:50 Japan Standard Time | Room G219, North - 2F
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Leighton Chajnantor Telescope (LCT) will be moved to the new site at Chajnantor Plateau, Chile in 2024. The new site has high wind speed and large temperature difference, which leads to strong wind disturbance and beam offset for LCT due to the lack of a dome and the deformation of the primary reflector. To achieve a high pointing control accuracy, we propose a composite feedforward/feedback control policy (FFCP), which integrates disturbance observer-based feedforward control policy (DOB-FCP) and the robust feedback control policy (RFCP) to compensate the wind disturbance and compress the negative effect caused by the beam offset respectively. The results of simulation experiments on the synthesized model of LCT’s pointing control system reveal that the proposed FFCP can significantly reduce the pointing error during the observations.
13099-29
17 June 2024 • 16:50 - 17:10 Japan Standard Time | Room G219, North - 2F
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The integrated modeling group at GMTO maintains a detailed FE model (mesh) of the entire telescope from foundation to top-end. Representations derived from this model are a very important component of simulations studying the effects of vibrations and misalignments due to wind, gravity, temperature variations, drives, actuators, utilities, and instruments on the image formation process.
13099-30
17 June 2024 • 17:10 - 17:30 Japan Standard Time | Room G219, North - 2F
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Self-induced vibrations along with wind-induced jitter are considered as most limiting factors for the performance of the Giant Magellan Telescope (GMT).
The status of dynamic analysis in context of the latest GMT mount design activities will be reported. Particular attention is paid to the vibration error budget, which is used to manage active disturbances in order to meet demanding tracking performance requirements. The vibration budget is based on tracking simulation results combined with contributions from different jitter and vibration sources such as drives, utility wraps, cabinets and many other subsystems. The Mount Transfer Function (MTF) concept as an important tool for analysis of vibration paths from the source to the image motion is introduced and its application in multiple use cases with both modeled and measured disturbances is illustrated.
Tuesday Plenary session
18 June 2024 • 08:30 - 10:00 Japan Standard Time | National Convention Hall, 1F
Join us for the Tuesday morning plenary talks.
Break
Coffee Break 10:00 - 10:30
Session 7:
Reliability, Availability, Maintainability, Safety
18 June 2024 • 10:30 - 12:30 Japan Standard Time | Room G312, North - 3F
Session Chairs:
Simonetta Chinellato, INAF - Osservatorio Astronomico di Padova (Italy), Takeshi Okuda, Joint ALMA Observatory (Japan)
13099-31
18 June 2024 • 10:30 - 10:50 Japan Standard Time | Room G312, North - 3F
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MICADO is a cryogenic near infrared Multi-AO-Imaging- Camera and Spectrometer developed for the first light operations at the ELT. It will operate in a Standalone configuration with a SCAO module, while will work together with the MORFEO relay optics and MCAO system in a later phase of the project.
The lifetime requirement of minimum ten years, together with other demanding requirements about its availability and reliability triggered a meticulous FMECA analysis mainly focused on developing robust maintenance strategies.
In this paper, we outline the assumptions and the boundaries of the MICADO RAM analysis, and we describe the preventive and predictive maintenance strategies, which we considered to minimize the risk of instrument downtime in the high cost operational context of the ELT. We describe how RAM aspects drove some design choices as well as the selection and use of components.
13099-32
18 June 2024 • 10:50 - 11:10 Japan Standard Time | Room G312, North - 3F
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I intend to discuss the deviations from the traditional space-based RAMS principles. These deviations are necessary to make our RAMS analysis more practical and relevant to our specific system. I will outline the practicality and reasons behind these deviations, highlighting their positive impact on our system's performance. Additionally, I plan to initiate a discussion on the RAMS requirements for our system. This dialogue will focus on optimizing and tailoring these requirements to better suit the unique needs and challenges of our system. And maybe include the obsolescence planning.
13099-51
18 June 2024 • 11:10 - 11:30 Japan Standard Time | Room G312, North - 3F
Show Abstract +
PLATO (PLAnetary Transits and Oscillations of stars) is an M3 medium-class space mission in ESA’s Cosmic Vision program aiming to detect and study a large number of extrasolar planetary systems. Its launch is planned at the end of 2026 from Europe’s Spaceport in French Guiana. The PLATO Payload consists of 26 wide field-of-view Cameras, each observing a specific part of the sky, associated data processing units and power supply units. The 24 Normal-Cameras will provide a very high-resolution photometric measurement of light from a large number of stars, while the other two Fast Cameras will provide the colour information and will deliver the pointing data to the AOCS (Attitude and Orbital Control System). The Cameras will be integrated into an optical bench. Each of them is composed of the Telescope Optical Unit (TOU), the Focal Plane Assembly (FPA) and the Front-End Electronics (FEE). Currently, the serial production of the Cameras has already started facing critical key points, non-conformities and challenging problems. The status of the Product Assurance activities during the serial production for which the first flight models are being delivered after the AIT phase is reported.
13099-34
18 June 2024 • 11:30 - 11:50 Japan Standard Time | Room G312, North - 3F
Show Abstract +
Complexity and costs of operations are almost part of the game in the design of a modern instrument for ground-based telescopes. MORFEO (Multi-conjugate adaptive Optics Relay For ELT Observations), formerly known as MAORY is the first light MCAO instrument for the ELT and its design has been driven also from the Reliability, Availability, and Maintainability point of view since its early phases. Now entering the Final Design Review particular attention has been considered in evaluation resources for maintenance, both preventive and corrective, to reach the high level of availability requested by ELT requirements. After a general view of the philosophy adopted for the RAM analysis of MORFEO, the case of the Low ORer sensor subsystem is proposed to show how requirements flow-down can be proactively used to ensure that the low-level characteristics, such as LRU accessibility, spare parts, and straightforwardness of maintenance operations can be addressed since the design phase.
13099-35
18 June 2024 • 11:50 - 12:10 Japan Standard Time | Room G312, North - 3F
Show Abstract +
The Multi Conjugate Adaptive Optics (M-CAO) Assisted Visible Imager and Spectrograph (MAVIS) is a multi-purpose instrument committed by ESO that will be installed at the ESO VLT Yepun telescope (UT4). It is a general-purpose instrument (with both a spectrograph and an imager) with an angular resolution close to the diffraction limit, thanks to an high-performance Adaptive Optics Module (AOM), that will provide the necessary correction for atmospheric turbulence. The AOM design is quite complex, and a strict Reliability, Availability and Maintainability (RAM) analysis is required to ensure the required operation time and lifetime availability of MAVIS, as required by ESO. A companion paper will present the RAM approach at MAVIS system level, while here we will focus on the AOM ensemble. We will outline the complex design of MAVIS AOM and the challenges that it poses from the RAM point of view, starting from the Reliability Block Diagram (RBD) model and the Failure Mode and Criticality Analysis (FMECA), thus supporting the design in avoiding/mitigating possible sources of failures, thus increasing the reliability of the instrument. We will also outline MAVIS maintenance strategy.
13099-36
18 June 2024 • 12:10 - 12:30 Japan Standard Time | Room G312, North - 3F
Show Abstract +
The National Science Foundation’s (NSF) Daniel K. Inouye Solar Telescope (DKIST) is a four-meter off-axis telescope on the island of Maui, Hawai'i. To ensure that hazard reduction was considered throughout the design process a Hazard Analysis Team (HAT) was formed and met regularly.
A hazard analysis process was developed and followed throughout the design, construction, integration, and early operations. During this time, the process was improved to better handle the inter-system hazards and make use of new tools for tracking hazards and methods for on-line collaboration were added to aid continuing management of hazards.
Break
Lunch/Exhibition Break 12:30 - 13:40
Session 8:
Integrated and Optics Modelling II
18 June 2024 • 13:40 - 15:20 Japan Standard Time | Room G312, North - 3F
Session Chairs:
Mitchell Troy, Jet Propulsion Lab. (United States), Masahiro Sugimoto, National Astronomical Observatory of Japan (Japan)
13099-37
18 June 2024 • 13:40 - 14:00 Japan Standard Time | Room G312, North - 3F
Show Abstract +
The NRC integrated modelling (NRCim) toolset has been developed at the NRC Herzberg Astronomy and Astrophysics Research Centre (HAA) for many years and has been used to predict complex system performance for several projects (eg. TMT primary mirror, NFIRAOS, IRIS, GPI). Although extensive software validation has been completed to ensure the validity of the NRCim results, there has not previously been an opportunity to measure the delivered performance of an instrument and complete an experimental validation of the NRCim toolset. With the recent assembly and testing of the SPIDERS instrument (Subaru Pathfinder Instrument for Detecting Exoplanets & Retrieving Spectra), our team at HAA has used the NRCim toolset to predict the performance of the SPIDERS instrument and subsequently completed directly measurements of the performance in the presence of prescribed disturbances. The measurements of the SPIDERS performance are compared with the NRCim-predicted performance providing a direct validation of the NRCim toolset.
13099-38
18 June 2024 • 14:00 - 14:20 Japan Standard Time | Room G312, North - 3F
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This study focuses on optimizing the thermal performance of the Visible Extragalactic background RadiaTion Exploration by CubeSat (VERTECS), a 6U CubeSat with a 3U telescope for observing Extragalactic Background Light. Aside from dealing with satellite survivability in the space environment, the payload includes a CMOS sensor which requires operational temperatures of less than 0°C to minimize the noise due to temperature dependent dark current in observation data. The payload telescope lens optical system is designed to operate within a temperature range of -10°C to 35°C. The thermal analysis considers solar radiation, internal heat dissipation, and external factors in various orbital scenarios. The investigation identifies potential temperature fluctuations and proposes passive thermal control strategies, including enhanced coatings and radiators. By implementing tailored strategies, this research enhances the reliability and longevity of 6U CubeSat missions, advancing small satellite technology in space exploration and scientific research.
13099-39
18 June 2024 • 14:20 - 14:40 Japan Standard Time | Room G312, North - 3F
Show Abstract +
The Nancy Grace Roman Telescope (RST) is a NASA observatory designed to unravel the secrets of dark energy and dark matter, search for and image exoplanets, and explore many topics in infrared optics. Scheduled to launch in no earlier than October 2026, this 2.4 meter aperture telescope has a field of view 100 times greater than the Hubble Space Telescope. The mission is currently in its construction phase, where integrated modeling between thermal, structural, and optical models of the observatory is necessary to demonstrate science quality images over the range of operational parameters. This presentation discusses the most recent integrated modeling analysis cycle for Roman, including model correlation with our instrument level testing. We include a discussion on improved processes of the handling of the various flows of data between the modeling disciplines and discipline specific monte-carlo analysis predictions. We will finish with the predicted uncertainties and expected performance for our upcoming observatory alignment verification test using machine learning algorithms.
13099-40
18 June 2024 • 14:40 - 15:00 Japan Standard Time | Room G312, North - 3F
Show Abstract +
Stray light (SL) control is an important aspect in the development of optical instruments. Iterations are necessary between design and analysis phases, where ray tracing simulations are performed for performance prediction. This process involves trial and error, requiring to be able to perform rapid evaluation of SL properties. The limitation is that accurate SL simulations require sending many rays, which can be time consuming. In this paper, we use deep learning to improve the accuracy of SL maps even when obtained with very few rays. Two different deep learning methods are used. The training process is performed by generating a large database of artificial SL maps, with different noise levels reproduced with a Poisson distribution. Once the training completed, we show that the autoencoder performs the best and improves significantly the accuracy of SL maps. Even with extremely small number of rays, it recovers complex SL patterns which are not visible on raw ray traced maps. This method thus enables more efficient iterations between design and analysis. It is also useful for developing SL correction algorithms, as it requires tracing SL maps under large number of illumination co
13099-41
18 June 2024 • 15:00 - 15:20 Japan Standard Time | Room G312, North - 3F
Show Abstract +
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 IM end-to-end simulation models combine structural dynamics, optics, and control models seamlessly in a unified framework.
Conceiving and managing such a tool imposes several challenges 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 unpractically 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.
Break
Coffee Break 15:20 - 15:50
Session 9:
Systems Engineering Management II
18 June 2024 • 15:50 - 17:30 Japan Standard Time | Room G312, North - 3F
Session Chairs:
Gelys Trancho, Thirty Meter Telescope (United States), Sébastien Elias Egner, European Southern Observatory (Germany)
13099-42
18 June 2024 • 15:50 - 16:10 Japan Standard Time | Room G312, North - 3F
Show Abstract +
We present the experiences acquired in the last decade by analyzing and evaluating the impact of more than 800 technology grants for technology developments awarded by the Astrophysics Division at NASA Headquarters. These studies have demonstrated a healthy infusion rate of these funded technologies and provided insights into the lifecycle of technology development components, and systems, which remain over a decade and in some cases up to two decades.
13099-43
18 June 2024 • 16:10 - 16:30 Japan Standard Time | Room G312, North - 3F
Show Abstract +
The Canadian Hydrogen Observatory for Radio-transient Detectors (CHORD) will consist of 640 six-meter diameter antennas made of composite (fiberglass) material. The antennas will be built at the Dominion Radio Astrophysical Observatory (DRAO) in Kaleden, BC, Canada, managed by the National Research Council of Canada.
NRC has been developing the composite based single piece reflector technology over the past decade in an R&D environment. For CHORD construction, NRC has been involved in the composite dish fabrication and assembly of the components. To meet the scientific goals, high degree of repeatability is the key in this project. That begins from the mold manufacturing to dish manufacturing to assembling components to alignment of the antennas.
In this article, we present the product breakdown structures, top level requirements, error definitions, performance verification, production safety plan, verification of the errors, quality engineering plans etc. It is important to point out that the systems engineering efforts are only limited to the production of the CHORD antennas only.
13099-44
18 June 2024 • 16:30 - 16:50 Japan Standard Time | Room G312, North - 3F
Show Abstract +
ASTRON, the Netherlands Institute of Radio Astronomy has embarked on a continuing journey of improving its project management and systems engineering practices. Daring to experiment with novel approaches, learning from them and implementing the lessons in practice play a pivotal role herein. By now, these efforts have led to a wide range of improvements, including the introduction of lean systems engineering with a preference for modelling over documentation, an iterative approach to development building upon a minimum viable product and increasingly complex prototypes, an agile approach to planning and teamwork, close involvement of stakeholders in the development process and a continuous professional development of our systems engineers and project managers.
As a result, we observe higher instrument quality, increased stakeholder satisfaction and more transparency in project progress and costs.
13099-45
18 June 2024 • 16:50 - 17:10 Japan Standard Time | Room G312, North - 3F
Show Abstract +
The Large Lenslet Array Magellan Spectrograph (LLAMAS) is a fiber-fed spectrograph developed for the Magellan Telescope at the Las Campanas Observatory, currently in verification at the MIT Kavli Institute. Verification planning is the problem of deciding how to allocate resources in the process of system verification, in order to achieve a desired level of confidence in system performance. Traditional methods may result in too many resources spent on tests which do not raise the confidence of performance sufficiently. This paper leverages advancements in uncertainty quantification and optimal Bayesian experimental design in order to determine verification test plans that minimize resources (time and cost) and maximize certainty of system performance. Optimal verification plans are presented, and compared to the historical and ongoing V&V approach for LLAMAS.
13099-46
18 June 2024 • 17:10 - 17:30 Japan Standard Time | Room G312, North - 3F
Show Abstract +
Early mission decisions, when information is sparse, define most of the downstream cost. This becomes particularly problematic when uncertainties will not be revealed until later in the design lifecycle. A resilient architecture is one that is adaptable to uncertainty, permitting cost-effective architectural changes as uncertainties reveal themselves. Adopting a resilient architectural framework requires adherence to three principles. First, maintain a broad architectural landscape to avoid premature descoping. Second, understand what is uncertain and when it will be revealed. Third, identify those architectural elements that allow cost-effective modification once those uncertainties become known.
A framework is proposed for designing a resilient HWO architecture. Uncertainties in advanced knowledge of exo-Earth targets, needed spectral bands to mitigate ambiguity in habitability, technical limits of starlight suppression techniques, and servicing capabilities and cost. Pre-cursor science and technology advancements drive architecture definition more than the converse: it is better to plan for, then react to, uncertainty.
Session PS1:
Posters - Series Production/Information, Configuration and Quality Management
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13099-47
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The construction of the ELT is now in full swing. This is true both for the construction of the Dome and Main Structure (DMS) in Chile, but also for all the other sub-systems manufactured by industrial partners in Europe. While the DMS is entirely managed by the industrial consortium, the shipment to Chile and the installation at the telescope of the other sub-systems is mostly under the responsibility of ESO. The shipment of these components from Europe to Chile has started recently and will soon reach a level of ~10'000 components/month. All these components will need to be tracked during their shipment, incoming inspections will need to be performed, health-checks and integration with other components will need to be done. The components will then be stored temporarily at the warehouse, before being installed at the telescope. We will present the approach for the logistics, infrastructure, and the tools set up to manage the status and location of all these components and to keep the link to their associated latest documentation.
13099-48
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Manufacturing and assembling the CTA Medium-Sized Telescopes (MST) involves a complex, geographically widely distributed engineering collaboration, which has to integrate all stakeholders, provide effective decision-making procedures, and establish reliable and efficient material and information flow. An essential ingredient to mastering the challenges is the digitalization of manufacturing planning, coordination and progress tracking processes based on a PLM system. The PLM system provides fully traced engineering data and digital workflow for e.g. reviews and sign-offs, and for managing changes and non-conformities. Digitalizing the manufacturing process enables optimizing logistics and automating workflow. It creates “vision sharing” for all involved parties and ensures faster and better decisions. Production sites can include remote suppliers for critical reviews and decisions without delaying production and assembly processes. The presentation introduces the PLM-based manufacturing process and reports experience gained from tendering, producing and quality-checking the first parts.
13099-49
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
In this paper the experience in building the receiving units, for the Atacama Large Millimeter/sub-millimeter Array (ALMA), with a specific focus on Product and Quality Assurance, will be presented.
Product and Quality Assurance plays a fundamental role in the production of reliable instruments in a repeatable way. This requires intense focus during the assembly process, therefore all components on the workbench at this stage need to be in perfect condition.
13099-52
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The Enhanced X-ray Timing and Polarimetry (eXTP) mission is a flagship astronomy mission led by the Chinese Academy of Sciences (CAS) and scheduled for launch in 2029. The Large Area Detector (LAD) is one of the instruments on board eXTP and is dedicated to studying the timing of X-ray sources with unprecedented sensitivity.
The development of the eXTP LAD involves a significant mass production of elements to be deployed in a significant number of countries (Italy, Austria, Germany, Poland, China, Czech Republic, France).
This feature makes the Manufacturing, Assembly, Integration and Test (MAIT), Verification and Calibration the most challenging and critical tasks of the project.
An optimized Flight Model (FM) implementation plan has been drawn up, aiming at a production rate of 2 modules per week. This plan is based on the interleaving of a series of parallel elementary activities in order to make the most efficient use of time and resources and to ensure that the schedule is met.
Session PS2:
Posters - RAMS
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13099-53
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The Gemini InfraRed Multi-Object Spectrograph (GIRMOS) is a high-resolution integral-field spectrograph and imager being built by a consortium of Canadian universities and institutions, along with the International Gemini Observatory and KASI. The team needed a cost-effective way to bring a degree of Product and Quality Assurance to bear on instrument development without the availability of a dedicated team. Support from the TMT Systems Engineering Team enabled the GIRMOS team to tailor and scale their approach to fit within the available resources of a much smaller project. This FMEA method more easily allowed geographically distributed subsystem teams to work independently within an agreed-upon FMEA framework that rolled up into a System-level analysis. The TMT FMEA framework reduced the effort involved in all the follow-on work that used the same data set, namely sparing analysis, reliability and uptime analyses, and accelerated life testing.
13099-54
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The road to increasingly more challenging systems in astronomy is resulting in as much bigger challenges to the safety. As well for the instrumentation, these big “systems” collaborate and share the same environment, and, as for the AO module MORFEO and the MICADO, some subsystems are strongly embedded, even if they are designed by different consortia. Therefore, the designers are thinking to more sophisticated electro-mechanical systems to assure the safety and communication of information between the instruments. The MORFEO consortium is investigating on the possibility to use industrial safety modules, architecturally integrated in the overall electronic control system. The paper goes through a comparison between the in-house designed safety solution, widely used in the past, and the industrial safety systems and the implementation of these technology in the ground-based astronomy in order to better understand the effects on the robustness from a safety-driven point of view.
13099-55
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The work presented here is a proceeding on the CUBES hardware RAM analysis up to the successful Preliminary Design Review and some forthcoming updates from the ongoing Final Design phase. The work has been developed during the design phases in order to assess the dependability of the System, as part of the Very Large Telescope, and to verify the compliance with the System requirements. The goal has been the identification of the criticalities and potential failure and the definition of the basics of maintainability in view of the last phases of the project, with the aim to keep the system in operation with high availability. Furthermore, the document provides the functional analysis of the System and a complete FMECA, with a deep focus on the influence of the “degraded modes” on the reliability.
13099-57
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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RAM analysis is crucial for the success of any measurement campaign and must be implemented at the earliest design phase of building an astronomical instrument. ANDES (ArmazoNes high Dispersion Echelle Spectrograph) currently in phase B will be the high-resolution spectrograph for the ELT formerly known as ELT-HIRES. Its design in the extended version foresees four spectrographs fed by fibers and operating both in seeing and diffraction-limited (adaptive optics assisted) mode. Due to these properties strictly related to flexibility and modularity, a RAM approach focused on different scientific data requirements permits a High availability for the main data acquisition modes. To implement this process, the product tree, active elements, modularity, component duty cycles, and degraded modes were defined in the earlier phases. In this way, RAM requirements contribute to defining design. This process avoids missing the control of particular aspects like maintenance accessibility, cost of operations, and downtime due to maintenance. The paper presents the process and how it is implemented in the ANDES project, thereby suggesting a design solution for the instrument.
13099-58
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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MAVIS is an instrument being built for the ESO’s VLT AOF (Adaptive Optics Facility, UT4 Yepun). MAVIS stands for MCAO Assisted Visible Imager and Spectrograph. It is intended to be installed at the Nasmyth focus of the VLT AOF 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 recently 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.
13099-59
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Safety analysis methodically assesses potential hazards and risks associated with a system. It encompasses an evaluation of all potential sources of harm, including equipment failures, human errors, and external factors, aiming to identify vulnerabilities and devise risk mitigation strategies. This proceeding presents safety analysis techniques and results for the Cassegrain U-Band Efficient Spectrograph (CUBES), a Cassegrain spectrograph for the Very Large Telescope (VLT), with a specific focus on its safety aspects. These techniques, including Failure Mode, Effects, Criticality Analysis (FMECA), and Hazard Analysis (HA), are employed to uncover and prioritize safety issues. Furthermore, this analysis relies on the Safety and Hazard Assessment Report and Safety Verification Report. CUBES, as a complex instrument, falls into multiple hazard classes, each with unique risks. Thus, this safety analysis plays a crucial role in ensuring the project’s success and safe operation.
Session PS3:
Posters - Managing Upgrades
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13099-60
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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This paper will describe the SMA's transition plan to the wSMA (wideband SMA). During this transition period, it will be required that the engineering and science teams operate and conduct scientific experiments with two different instrumentation packages. The wSMA upgrade will result in the SMA to be a more productive and efficient observatory.
13099-61
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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Upgrading telescope control systems is critical for maintaining astronomical observation quality. However, such changes risk disrupting observations. This study presents a strategy for minimizing these disruptions, focusing on the Telescopio Nazionale Galileo (TNG) as a case study.
Our methodology involves a thorough analysis of existing TNG systems, emphasizing the reuse of structurally sound components. A 3D modeling approach ensures precise planning and feasibility evaluation. A parallel installation at TNG allows for rigorous testing and validation of new systems before full implementation, reducing operational risks.
In summary, our approach optimizes telescope control systems, minimizing the impact on astronomical observations. We demonstrate its effectiveness through the TNG case study, offering valuable insights for efficient telescope upgrades.
Session PS4:
Posters - Manufacturing, Assembly, Integration, Testing and Operating Systems
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13099-62
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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NFIRAOS (Narrow-Field InfraRed Adaptive Optics System) will be the first-light multi-conjugate adaptive optics system for the Thirty Meter Telescope (TMT). The system will be built, tested, and integrated with the first instrument, IRIS (Infrared Imaging Spectrograph), at Herzberg Astronomy and Astrophysics (HAA) in Victoria BC. NFIRAOS is a complex instrument that will require careful integration planning to meet cost, schedule and performance deliverables. HAA has purpose-built a new facility for the integration of NFIRAOS. We present the key features of this building, and their roles during the assembly, integration, and test phase (AIV). NFIRAOS and IRIS will be fully operational in Victoria, including providing calibration sources, and able to close the adaptive optics (AO) loops with the IRIS On-Instrument Wavefront sensors. NFIRAOS will then be disassembled and shipped to TMT for final construction and commissioning, which requires navigating some logistical challenges.
13099-63
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
SOXS (SOn of X-Shooter) is a high-efficiency spectrograph with a mean Resolution-Slit product of about 3500 over the entire band capable of simultaneously observing the complete spectral range 350-2000 nm. It consists of three scientific arms (the UV-VIS Spectrograph, the NIR Spectrograph, and the Acquisition Camera) connected by the Common Path system to the NTT, and the Calibration Unit. During the last year, we have performed the AIV of the instrument in the integration site in Europe. It is still ongoing.
We present an overview of the flow for the validation of the scientific and technical requirements, after the integration of the sub-systems with some results as highlights. Further, we give an overview of the methodologies used for planning and managing the assembly of the sub-systems, their integration, and tests before the acceptance of the instrument in Europe (PAE). SOXS could be used as an example for the system engineering of an instrument of moderate complexity, with a large geographic spread of the team.
13099-64
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The WSS is a subsystem being constructed by the CENTRA/METIS team (Portugal) for the ESO ELT first light instrument METIS – the Mid-infrared ELT Imager and Spectrograph.
The WSS consists of three structures – the support system (ELP), the alignment system (CAS), and the access and maintenance system (RIG). In total, the WSS dimensions are approximately 6 x 6 x 6 meters. In order to assemble, integrate, and test such a large system, an integration hall of at least 2.5 times the WSS volume would be needed to accommodate clearance around the WSS (for personnel and positioning of cranes and scissor lifts) and clearance over the WSS (for overhead cranes and margin for hoisting). Such integration halls are not readily available or accessible.
In order to overcome this challenge, we have devised a 3-step strategy to assemble, integrate, and test the WSS at three different locations in three different configurations.
13099-65
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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MAVIS (MCAO Assisted Visible Imager and Spectrograph) is a new instrument for ESO’s Very Large Telescope. It is intended to be installed at the Nasmyth A focus of UT4 “Yepun” telescope with commissioning planned around the turn of this decade. The team designing MAVIS is organised in a consortium having international reach between sites in Australia, Italy, France and Germany. As the project currently progresses through the final design phase, planning for the next crucial phase is underway.
The Manufacture, Assembly, Integration and Testing (MAIT) phase will begin in early 2025 and take place in four primary locations, two in Australia and two in Italy. MAVIS is composed of different modules that interact with each other and given the complexity of the instrument different assemblies will travel across the world during this phase with the final assembly taking place in Canberra.
We present the strategy for the MAIT phase, the associated schedule considerations and the individual MAIT for the different modules. We also elaborate on the Assembly, Integration and Verification (AIV) phase that will take place once MAVIS is delivered to the Paranal Observatory in Chile.
13099-66
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Moving into the era of Extremely Large Telescopes (ELT), the size and complexity of the instruments increased significantly while constraints and requirements remain tight. NOVA follows a monolithic design strategy, meaning that the size of individual components scales with the size of the instrument. To enable the manufacturing and assembly of the largest components at the required precision, NOVA has invested heavily in a new facility for ELT-era instrumentation: NOVA Manufacturing and Assembly of eXtreme instrumentation (MAX). Here we introduce the capabilities of NOVA MAX, which includes a 5-axis CNC milling machine and a Coordinate-Measuring Machine (CMM) in a temperature-stabilized environment. The CMM is located in an ISO Class 6 cleanroom with temperature variations < 0.5K/8 hours, enabling micron-level verification and fine-tuning during assembly. This unique assembly facility is crucial when producing large size one-off instruments. We report on, amongst others, the tolerances, dimensions, and loads that can be achieved with both machines and present the first components that have been manufactured for the METIS and MICADO ELT instruments.
13099-67
Rubin Operations - Enabling collaborative ground-up budget planning across a multi-team organization
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Plans are made to be broken! Planning and budgeting is done with good intentions but the unexpected is inevitable. With a view to expecting the unexpected it makes sense to plan for change. Building on similar processes in other HEP experiments, Rubin Operations has developed a process whereby on an annual basis the spending plan is scrubbed, a bottom up clean up where the past and future get synchronized to the current known situation. This paper will deep dive into the process and the Observatory’s custom, web-based collaborative tools.
Session PS5:
Posters - MBSE
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13099-68
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
In the context of PLATO Camera Subsystem development, it has been decided to take advantage of MBSE methodologies using Enterprise Architect by Sparx Systems as tool.
A Local SysML Camera model for PLATO mission has been built from different Excel spreadsheets, i.e. Verification Control Matrices, released by Subsystems. Same approach has been used for the Camera-System itself. The complete flow-down of requirements has been created in order to easily identify and monitor any impact on the design due to changes, deviations and non-compliances.
The model can be updated at any time importing Excel spreadsheet while it can be used as source to export documentation needed during formal reviews, both as Word and Excel files.
In addition, Model architecture and constraints have been created through Block Definition Diagram and Internal Block Diagram so that structure, interfaces as well as interaction between different items, can be easily identified and monitored at both System and Subsystem level.
13099-69
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The use of model-based systems engineering (henceforth MBSE) has proved effective for early conceptual design of the Gemini North Adaptive Optics Bench – Phase A. The establishment and maintenance of the single version of the truth (i.e. the model) has helped offset some the technical challenges and risks associated with a large and technical complex project. To this extent, the AAO-Macquarie and collaborators (ONERA/LAM/ALPAO) adopted an MBSE approach for the proposed Gemini North Adaptive Optics Bench - Phase A (AURA project). We use architecture representations and system decompositions using the Systems Modeling Language (OMG SysML) elements, both functional and structural, with diagrams, allowing each project stakeholder to focus on aspects of the problem. The SysML elements can be traced to requirements and other elements, making it easier to assess risk and prevent costly mistakes discovered during development and operational phases. This paper provides an overview of the methodology, software tools and framework applied, with the hopes that this knowledge be beneficial to the system modelling of future adaptive optics systems.
13099-70
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Morfeo (Multi-conjugate adaptive Optics Relay For ELT Observations) is an adaptive optics module able to compensate the wavefront disturbances affective the scientific observation. It will be installed on the straight-through port of the telescope Nasmyth platform to serve the first-light instrument MICADO and with the provision for a future second instrument. The module underwent the Preliminary Design Review in 2021 and is expected to be commissioned in 2029.
In this paper we present a synthesis of the System Engineering approach adopted to manage the development of the instrument assessing the criticalities of phase B (preliminary design) and preliminary phase C (final design). We will discuss the evolution of the system engineering approach, identifying within the MBSE framework the evolution of the various modelling artefacts. towards the requirements. We will detail the criticalities of the system engineering with a particular focus onto the management of the interfaces between subsystems and external systems (Telescope, other instruments…).
13099-71
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Recently, the Italian astronomical community has begun adopting Model Based System Engineering (MBSE) for the development of complex instruments. A significant challenge is the establishment of a robust and flexible method to manage all system aspects, among which the interfaces. This paper presents an in-progress method to trace and verify the interfaces of ANDES, the high-resolution spectrograph for the ELT telescope. The method is part of a customization of SysML language capabilities in Cameo Systems Modeler to meet the needs of the astronomical field.
The method uses the nature of the interfaces to populate the interface blocks used to represent the interfaces in the system and to store the numerical and literal values that define the interfaces. The verification process checks if the client side is compliant with the constraints imposed by the host. This whole process employs the use of computational blocks prepared in advance and reused for each interface to lighten the set-up effort and reduce human errors.
The application of this methodology shall largely improve interfaces management leading to more efficient and safer evaluations compared to traditional methods.
13099-72
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Italian astronomical community has begun adopting Model Based System Engineering (MBSE) to develop complex instruments using Cameo Systems Modeler targeting various system engineering tasks including requirements management, system structure management, activities modelling and simulation, and many more.
Lately, the focus moved also to managing the system interfaces and the associated cabling and connectors. The proposed methodology uses interface blocks to represent the connectors and their location in the system. The interface blocks generate a proxy port owned by the structural element they are applied to. These ports are then connected to represent the interactions among parts, subsystems, and with external actors using SysML connectors. The connectors are then refined through association blocks also used to represent the cable with all their characteristics. The association blocks are linked to the structural blocks as their parts leading to their inclusion in the PBS of the subsystems.
The main output is a table listing all the cables of the system, their connectors, the system parts they connect, and other specifics of the cable like its length, weight, and so on.
13099-73
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Present status and plan of the concept study support of research at systemology support section of KEK QUP are presented. We introduce CRDF (Concurrent Research Design Facility), which is not the same but somewhat similar to the concept study facility used in space science missions. The CRDF utilizes Model-Based Development (MBD) and Model-Based Systems Engineering (MBSE) software tools. We have also developed a Concept Maturity Level (CML) checklist specifically suited for research in astronomy and other sciences to measure the level of the research concept and to guide the concept study, based on the CML framework used in space missions. We are conducting the CRDF on a few early research concepts. We will also report the present status of the support in this paper.
Session PS6:
Posters - Project Management
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13099-74
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
In this paper we present the project management approach we envisaged to master successfully all the project phases of ANDES, the forthcoming high-resolution instrument for the ESO/ELT, from the finalization of the preliminary design up to commissioning on-sky; in particular we will describe the risk management and PA/QA activities we have foreseen to assure appropriate risk mitigation and an overall high-quality standard required for the ANDES project.
13099-75
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
There is growing interest by operational ground based observatories to follow formal project management methodologies in order to better plan and execute their projects. But the rigors of industry standards are far too excessive and costly for most of these observatories and their unique infrastructure and instrument upgrade projects. Instead, we suggest extracting the best practices through careful and intentional tailoring of conventional methodologies so as to fit the authentic needs and goals of the observatory without severe transformations of their existing staff, budget, or culture. Only then will the initiative of more formal project management be embraced and the true benefits realized.
13099-76
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Atacama Large Millimeter/submillimeter Array(ALMA) Band 1 receiver covers the frequency band between 35-50 GHz. The project achieved the successful delivery of 73 Band 1 receiver units to ALMA telescope site and ready for cycle 10 observation.
This paper will delve into the implementation of Project management methodologies applied during the both receiver development and production phases. Furthermore, the paper presents the lessons learned and challenges faced, and offer for the future endeavors in applying the project management in the scientific research projects.
13099-77
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Center for the Gravitational-Wave Universe at Seoul National University has been operating its main observational facility, the 7-Dimensional Telescope (7DT) since October, 2023. Located at El Sauce Observatory in Chilean Rio Hurtado Valley, 7DT consists of 20 50-cm telescopes equipped with 40 medium-band filters of 25-nm FWHM along with camera of 61 megapixels. 7DT produces about 1 TB per night of spectral mapping image data once our planned 3 layered surveys starts in early 2024. We are expecting to generate 1 PB per year. To incorporate huge amount of data, we have a data storage for 1 PB which we will increment by 1 PB per year until 2026. We also have a high performance computation facility for real-time data reduction and analysis. We also established a high-performance network between Korea and Chile. We have been carrying out fully remote operation since October 2023 with TCSpy, a python-based operation software system developed to control multi-telescope array. In this talk, we present details of designing, planning, and executing the ground-based telescope facility project emphasizing management of human resource, project risk, and financial contingency.
13099-78
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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In this paper, we are describing the need of the protocol (for reaching safe conditions on the PLATO CAMs) activation for answering to one of the worst events that could be present during a TVAC testing campaign, the calibration and TVAC testing campaign INTA is participating in as one of the test houses for PLATO: an unexpected power outage making the vacuum pumps critically fail. The room conditions recovering in a safe way is reported on
13099-79
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
VSTPOL is a project to provide a new polarimetric capability to the VST. With its 2.6m primary mirror and 1 degree x 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.
13099-80
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Parametric cost models are useful for developing mission concepts and evaluating technology gap investments. This paper presents a preliminary extension of the Stahl Parametric Cost Model for Ground and Space telescopes for balloon missions. Also, regressions are run on the database to investigate potential cost correlations with having an off-axis telescope and schedule duration.
13099-81
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Parametric cost models are useful for developing mission concepts and evaluating technology gap investments. This paper presents a preliminary parametric cost model for x-ray telescopes developed via the same process used to develop the Stahl Parametric Cost Model for normal incidence ground and space telescopes.
13099-82
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Italian National Institute for Astrophysics (INAF) groups together 16 Observatories and Institutes. Each hosts one or more laboratories and workshops, to support technological research, operations and maintenance. This results in a vast panorama of facilities, instrumentation, equipment and skills. During a recent meeting, the INAF technological community clearly expressed the need to share information in order to more easily find tools, facilities, skills, or whatever could be of interest, to increase the working efficiency and minimize dead times and costs. We addressed this need and started developing an interactive tool called MIRTA (Interactive Map for Technological Research in INAF), aimed to effectively collect and share all this information. Its use cases can be very simple, such as, for example, solving a contingent software or technical problem or finding a specific device, or more complex, such as finding a staff member with the necessary skills to collaborate in a new or existing project.
13099-83
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The astronomy society is undergoing a massive series of disruptions. From the blooming field of artificial intelligence to worldwide pandemics and to capturing the first-time historic images of certain celestial phenomenon; permanent shifts are reshaping this science community. Project management (PM) is now the most important method for astronomy leaders in this society to handle these changes for a positive and desirable outcome. It is a challenge to be a project manager in the astronomy world which is driven by effort, when progress and results are what is required from a project manager to deliver a successful project.
Throughout the astronomy society, forward-looking observatories will set themselves up for sustainable growth. This article will talk about the observations of the authors on the challenges to apply PM principles in operational observatories and how to follow PM principles dutifully in future projects for long lasting observatories.
Session PS7:
Posters - System Modelling End-to-End
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13099-84
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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This study focuses on the simulation and optimization of robotic fiber positioner technologies identified for the conceptual MANIFEST instrument, designed to provide fiber feeds to the G-CLEF and GMACS spectrographs mounted on the Giant Magellan Telescope (GMT). The positioner technologies simulated in this study include Starbugs, Starspines, Theta-Phi, and Pick-and-Place robots. The simulation model is constructed using MATLAB software, with key model parameters considered in the simulations encompass the exclusion radius and the patrol radius. The simulations cover diverse science datasets with single fibers and IFUs. The study aims to optimize these parameters to achieve the best field completeness and survey efficiency for the GMT. The findings aid in selecting the most suitable robotic positioner technology for the GMT, as well as advancing the understanding of the capabilities and limitations of robotic fiber positioner technologies, contributing to the advancement of efficient multi-object spectroscopic surveys for astronomical telescopes.
13099-85
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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HARMONI is the first light visible and near-IR integral field spectrograph for the ELT, covering a large spectral range from 470nm to 2450nm with resolving powers from 3300 to 18000. As part of the project, CRAL has developed an instrument numerical model capable of generating synthetic detector read-outs for both calibration and science exposures. This simulator plays a key role in developing robust pipeline algorithms, elaborating instrument calibration procedures, offering feedback on the instrument's design and contributing to the validatation the instrument's scientific goals.
13099-86
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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We present a comprehensive overview of the collaborative efforts between the End-to-End (E2E) Simulator and the Data Reduction Software (DRS) team, focusing on the modeling of the U-band efficient Cassegrain spectrograph CUBES (ESO-VLT). The E2E model is a Python-based numerical simulator capable of rendering synthetic raw frames with high precision for both astronomical and calibration sources, starting from their 1-d radiation spectra up to the data produced by the detectors. Data from the E2E are processed by the prototype Data Reduction Software (pDRS), a Python library which implements the critical algorithms of the DRS. The PDRS performs wavelength calibration and extracts a 1-d spectrum from one or more reduced science exposures. The 1-d spectrum produced by the extraction routine is meant to be compared directly with the input spectrum fed to the E2E, actually “closing the loop” allowing for a real end-to-end assessment of the instrument capabilities.
13099-87
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The construction of a ground-based astronomical telescope with a ten-meter aperture in China is imminent. Connecting such telescope to single-mode fibers for light delivery to compact photonic spectrometers, enhancing radial velocity measurements, and improving optical interferometry precision pose active challenges. This research presents end-to-end simulation procedures for on-sky coupling to single-mode fibers, utilizing open-source atmospheric and adaptive optics software. The simulations, integrated into optical software, perform physical optics propagation, enabling a dynamic evaluation of fiber coupling. A comprehensive error budget determination procedure is described.
13099-88
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The computational complexity of integrated structural-thermal-optical performance models, particularly for one-of-a-kind telescope missions, often limits the maximum feasible number of analysis cycles. Applications requiring a large number of model evaluations, such as uncertainty quantification and sensitivity analysis, can become infeasible if the number of required iterations for the analysis exceeds the allocated computation time or budget. Another major obstacle to the sensitivity analysis of integrated models is the dependence between variables, as correlation between the variables changes the contribution they have on the variance in output model predictions. This paper presents a multifidelity integrated modeling methodology that incorporates both high-fidelity and low-fidelity models to reduce the model’s computational cost while retaining sufficient accuracy for sensitivity analysis. Additionally, an estimation of the closed sensitivity indices is presented for the fully integrated model, taking into account the dependence between variables in structural-thermal-optical performance models.
13099-89
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Mid-infrared ELT Imager and Spectrograph (METIS) is one of the first-light scientific instruments for the ELT. The common fore optics (CFO) sits at the heart of METIS, conditioning the beam and distributing the light across the wavefront sensor and science channels. To ensure it can reach its science goals, rigorous analysis of manufacturing and alignment tolerances is essential. For the CFO, an end-to-end tolerancing system was developed, integrating component level analyses, FEA results, as-built data to continuously optimize system performance during the design phase, as well as manufacturing and assembly phase.
13099-90
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The MeerKAT+ project will extend the current MeerKAT Radio Telescope Array at the South African
Radio Astronomy Observatory (SARAO) site in the Karoo region of South Africa. In this paper we
present the developed methodology, instrumentation, and the current status for verifying the
pointing accuracy of a single array telescope using an optical pointing telescope and a detailed
Pointing Error Budget (PEB) of the radio telescope structure.
We will focus on a description of the developed instrumentation, the measurement software, the
testing procedures, the measurement plan based upon them, and the applied steps for data
processing and analysis. The obtained results are then correlated directly to the PEB.
Furthermore, we relate the acquired results from optical pointing tests to some early radio frequency
pointing tests and conclude with a discussion.
13099-91
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The SKA MPI Demonstrator which was built at the SARAO site in the Meerkat National Park in South Africa to gain experiences for the MeerKAT Extension project. The commissioning of the SKA MPI Demonstrator was accompanied by the collection of a large amount of wind data acquired from the installed nearby weather station. Combined with the servo-relevant measurements such as torques, motor rates, position encoder readouts, temperatures from different locations it provided valuable input for characterizing the influence of wind loads on the structure. We present the results of the static and dynamic analysis of the data collected over several months: wind speed spectra, wind torque coefficients, as well as supporting unbalance and friction curves and show how this information is used in the dynamic simulations of the updated Dish structure design for the MKE project.
13099-92
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Wide Field Optical Spectrograph(WFOS) is the first light instrument of Thirty Meter Telescope(TMT), which will be one of the wide field spectrographs for optical spectroscopy and can probe the faintest limits. In order to reach the faintest limits provided by the aperture of TMT, WFOS is designed to have multi-object(~60 objects) slit-based spectrograph. Slitless spectroscopy has been popular in space based instruments, however it is not pursued in ground based observatories due to the background contamination. Here we present the feasibility of slitless mode of TMT-WFOS and the sensitivity limit for various field densities focusing on MilkyWay satellite galaxies.
13099-93
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
JASMINE is a Japanese planned space mission that aims to reveal the formation history of our Galaxy and discover habitable exoEarths. For these objectives, the JASMINE satellite performs high-precision astrometric observations of the Galactic bulge and high-precision transit monitoring of M-dwarfs in the near-infrared (1.0–1.6 microns in wavelength). For feasibility studies, we developed an image simulation software named jasmine-imagesim (JIS) to produce realistic observation images taking into account the optical point-spread function (PSF), telescope jitter, detector flat patterns, readout timing of each pixel, and various noise signals to produce realistic observation images. The simulation images confirmed that the required position-measurement precision of 4 milli-arcseconds in a single exposure for 12.5-magnitude objects can be achieved by the current baseline system, while the precision may be degraded by the telescope jitter and differences in readout timing between pixels. In this presentation, details of JIS and simulation results will be presented.
13099-94
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Wide Field Imager (WFI) instrument of the ATHENA X-ray observatory aims at spectroscopic imaging between 0.2 keV to 15 keV. The signal chain describes the photon detection and signal processing pipeline along with individual noise allocations adding to the spectral degradation to determine the energy range for WFI. We present a qualitative and quantitative overview of the WFI signal chain for requirements system engineering. The presented signal chain will effectively determine the dynamic range of WFI with respect to incoming photons, i.e. the end of life spectral resolution of ATHENA’s WFI in its current phase.
Session PS8:
Posters - System Modelling Optics
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13099-95
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Polarization differential imaging (PDI) is a key point-spread function subtraction technique that efficiently processes out starlight and reveals faint polarized structures, such as circumstellar disks and exoplanets. However, in the presence of polarization aberrations the starlight will be slightly polarized by the telescope that observes it. This results in a spatially-varying polarized speckle field on the focal plane of high-contrast imaging polarimeters. Current high-contrast polarimeters are roughly an order of magnitude from achieving the photon noise limit, and polarization aberrations are a contributing factor. This effect will be stronger in the next-generation 30m GSMTs where polarization aberrations are stronger. We present a numerical model of a high-contrast imaging polarimeter behind an AO system subject to the polarization aberrations of an GSMT-class telescope. We use this model to understand the coupling of polarization aberrations into the adaptive optics residuals that leak through to the focal plane. We report on the fundamental limits imposed by polarization aberrations on PDI and discuss mitigation strategies to compensate for this effect.
13099-96
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
In this talk we introduce RayZaler: a free-as-in-freedom opto-mechanical simulation framework. RayZaler features a ray tracer that acts upon a parametric model, stored as one or more human-readable, plain-text model files. The user defines the degrees of freedom of the model explicitly in the model files, and can use them as variables of math expressions that describe the geometry of the model. The model can be further enriched by means of Python scripts, whose functions can be referenced from the model files themselves as additional math functions.
13099-97
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
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 of the impact of these aberrations on the PSF moments as detected in the science field. Additionally, 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 as a valuable tool to infer the state of the optical system. This work will provide an additional tool as an aid for the Rubin team during the commissioning activities.
Session PS9:
Posters - System Modelling Mechanical and Thermal
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13099-98
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Giant Magellan Telescope project has invested in creating a series of computational fluid dynamics 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 accurate determining dome seeing. We start with thermal modeling, using 1-D approximations for a long periods of time. The second is a detailed computational fluid dynamic (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. T At this stage we calculate how the structural components deform in response of the temperature variations given from the thermal model. This combined thermo-mechanical model serves to quantify the telescope optical misalignment with regard to the cyclic variation in ambient temperature between day and night. These thermal deformations are feed to the telescope optical model, which conducts the ray tracing through the opt
13099-99
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The ASTRI Mini-array is a group of IACT telescopes used for gamma-ray astronomy. It is led by the Italian Institute for Astrophysics (INAF) and comprises nine telescopes. The telescopes collect Cherenkov light, produced when high-energy gamma photons interact with Earth's atmosphere. The focal plane cameras use silicon photomultipliers and fast-acquisition electronics peak detectors to detect and process the data. Each camera has 37 SiPM tiles stacked on top of a Cherenkov Imaging Telescope Integrated Read Out Chip (CITIROC) and an FPGA board. In total, there are 111 boards. The cameras require a temperature of 15°C and ±1°C uniformity (PtV), achieved by an electric thermal control system. The system uses Peltier cells and air cooling to maintain a stable temperature without liquid cooling. The thermal control system requires about 295 W of cooling power. The design of the thermal control system was modelled using a novel approach of thermal modal analysis and block simulations. Finally, Camera#0 focal plane was integrated and tested at EIE GROUP's and INAF's facilities.
13099-100
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The TMT 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.
13099-101
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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An aerothermal modeling framework was developed for the entire TMT LGSF, 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, evaluate beam jitter by obtaining 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.
13099-102
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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Conjugate heat transfer modeling is used to estimate the front temperature distribution, thermal deformation and differential pressure distribution of the GMT primary mirror cell. The modeling framework is used to validate segment temperature and thermal deformation requirements and in support of the M1 optical testing currently 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.
Session PS10:
Posters - Systems Engineering Management
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13099-103
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The Cosmic Microwave Background Stage Four Experiment (CMB-S4) is a planned DOE/NSF ground-based experiment that will probe the entire history of the cosmos by performing millimeter-wave sky surveys to produce multi-wavelength sky maps in both intensity and polarization of unprecedented quality. To meet its ambitious and transformative science goals within a reasonable survey duration, CMB-S4 employs a rigorous Systems Engineering approach to ensure tight control of instrumental sensitivity, systematic error, and instrument down-time, subject to constraints at the planned deployment sites of the Chilean Atacama desert and the South Pole. This disciplined Systems Engineering framework is essential for managing the instrumental configuration within the multi-institutional structure of the project. We present an overview of the project’s Systems Engineering approach, processes, tools, and status.
13099-104
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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As part of the strengthening of the Italian research infrastructure included in the National Resistance and Resilience Plan, a financing proposal was presented for the recovery of an ancient 19th century building located in the park of the Astronomical Observatory of Capodimonte INAF, allocating it to host INAF's first Concurrent Design Facility and the first in southern Italy. A Concurrent Design Facility (CDF) is the set of infrastructures, devices and processes that allows engineering teams with people from different backgrounds to work together, at the same time, on all the aspects of the design. This coordinated effort helps to achieve complex design definition more easily and quickly, through an engineering management protocol, compared to a “step-by-step” approach, which is the traditional method where each team works individually with only little direct interaction with each other.
Concurrent engineering is extremely efficient in terms of time and effort, especially for feasibility studies and preliminary design.
This article describes the project presented and the expected functionality of the new CDF, both from a technological and architectural recovery point of view.
13099-105
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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LiteBIRD is the JAXA’s satellite-borne, cosmic microwave background experiment which is planned to be inserted into the orbit in the early 2030s. Currently, the development is in the conceptual design phase, where the systems-engineering approach is of crucial importance. KEK QUP is responsible for providing the focal-plane detector unit (FPU) for the low-frequency telescope (LFT). We, the systemology support section of QUP, conducted the systems engineering of the focal plane detector subsystem including FPU.
We present the flow of our systems engineering processes which consist of three groups, the systems design, systems realization, and technical management processes, and show the list of the products. We present the issues we found in the processes and the measures we proposed. We need further adjustments between the customer's expectations, i.e., the requirements from JAXA, and feasible requirement allocation of the unit.
13099-106
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Presentation on the tailoring of standard systems engineering practices for the future Gemini instrument GIRMOS, which consists of four MOAO spectrographs plus one imager, in particular in terms of requirements flowdown and interface management. Special emphasis is given on the inter-dependencies with the Gemini North Adaptive Optics system GNAO. Additionally, the presentation covers the envisioned operations concept.
13099-107
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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A concurrent engineering approach to the design of astronomical instrumentation is based on experts of different backgrounds collaborating in the same environment on every aspect of the design. This strategy is very cost effective and can optimize interactions among teams, compared to the traditional approach.
For projects of the complexity that is dealt with in space or ground-based astronomy, concurrent engineering has been proven to be extremely efficient in terms of time and effort.
In this work, an analysis of the methodologies that are typical of a concurrent design approach is made, with a focus on the tools that can be adopted for an efficient coordination of all the people involved.
These tools and methodologies will be applied to the Concurrent Design Facility in construction at the Capodimonte Astronomical Observatory in Naples, in the scope of the National Recovery and Resilience Plan project "STILES - Strengthening the Italian leadership in ELT and SKA", with the aim of significantly improving the design process of the present and future classes of astronomical instrumentation.
13099-108
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We present a trade study on design changes to the Wide Field Optical Spectrometer for the Thirty Meter Telescope. WFOS is planned as a first light instrument providing imaging and multi-slit spectroscopy over the wavelength range 0.31 to 1µm across a field of view of 8.3 by 3 arcminutes. The baseline prior to the trade study used laser cut metal slit masks at the focal plane to enable observation of ~50 to 80 objects simultaneously. The configurable slit unit design uses multiple knife edges mounted on computer-controlled bars to create up to 88 reconfigurable slits, enabling the ability to adapt to seeing conditions or to respond to targets of opportunity. We detail here the decision criteria, and science case analysis used by the WFOS team to decide to change the baseline design of WFOS to incorporate a CSU.
13099-21
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
A major issue for project management, besides handling schedules and deadlines, is the process of finding and extracting the most relevant information from a variety of different software solutions used by the different stakeholders. This often leads to enormously large Excel sheets that try to identify the most up-to-date versions of the documents needed, which are extremely time-consuming to maintain, inefficient for finding information, and prone to errors.
Digital Posters
The posters listed below are available exclusively for online viewing during the week of SPIE Astronomical Telescopes+Instrumentation 2024.
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- Check the individual conference call for papers for additional requirements (i.e. extended abstract PDF upload for review or instructions for award competitions)
Related Courses
Courses at Astronomical Telescopes + Instrumentation
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See courses on topics related to Modeling, Systems Engineering, and Project Management for Astronomy.
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Pre-registration is required for SPIE Courses.