KEYWORDS: Systems engineering, Interfaces, Computer aided design, Observatories, Systems modeling, Standards development, Safety, Reliability, Databases, Control systems
The objective of the systems engineering effort is to ensure the successful development and operability of the TMT system, by defining clear policies and procedures for architecture definition, requirements management, interface management, integration management, and verification. This paper shows the tailored implementation of the systems engineering approach which is intended to ensure that the system meets all requirements while being affordable, producible, and maintainable over the observatory’s life, while maintaining acceptable risk. This paper also describes the evolution of this approach in the last decade at TMT and the reasoning behind that evolution.
The Giant Magellan Telescope project established Key Performance Parameters (KPPs) for measuring, tracking, and managing the evolution of expected observatory performance through construction and commissioning. The KPPs are inherently statistical variables. The performance of the as-built observatory depends on environmental and operational parameters. Just as importantly, its performance also depends on not fully predictable programmatic processes and technical uncertainties associated with design and construction. Mitigation of technical risks and management response to realized technical risks have critical impact on achieved performance through decisions allocating project resources to remedy potentially impaired performance. While the requirements capture the objective values of KPPs, relaxed threshold values represent the minimum acceptable performance that must be achieved in support of the scientific objectives of the observatory. Properly defined threshold values may reduce project risk exposure and aid project management in building and delivering the observatory on time and on budget. This paper reports our statistical approach to determine the KPP threshold values the project can accomplish with high confidence level in the face of programmatic and technical uncertainties. The method identifies the technical risks threatening KPPs and carefully characterizes them to ensure their suitability for further evaluation. This paper also demonstrates a Monte Carlo approach to using recognized project and subsystem risks to bound the probability density functions for performance, cost, and schedule impacts, which are in turn applied to each KPP error budget to determine threshold values. The analysis is integrated into the project’s statistical risk and contingency estimation framework.
The maintenance concept provides the basis for overall dependability design requirements for Extremely Large Telescopes (ELTs), such as the European Southern Observatory’s ELT, the Thirty Meter Telescope (TMT), and the Giant Magellan Telescope (GMT). The maintenance concept contains the planning of the maintenance and support policy for the complete operational system of the ELTs. The way in which the maintenance concept was developed in the ELTs is shown, and the similarities and differences in the way the operational objectives will be achieved is identified. The methodology is based on explaining seven common points (maintenance philosophy/levels; maintenance types and strategies; designing for dependability: reliability, availability, and maintainability; organizational structure and responsibilities for maintenance operations; maintenance and configuration management; key performance indicators for operations; and challenges, opportunities, and lessons learned) and condensing the knowledge during the process of generation and application of the maintenance concept.
In the advanced design, construction, and commissioning phases of GMTO project, the critical role of systems engineering is tracking and managing expected observatory performance and ensuring that the scientific goals of the Giant Magellan Telescope (GMT) are met. GMTO’s approach to this role is defining Key Performance Parameters (KPPs) to measure technical performance. A set of KPPs have been established to assess the performance of the telescope through construction and Assembly, Integration, Verification, and Commissioning (AIVC). Each KPP has a threshold value representing the minimum acceptable performance, and an objective value representing the desired operational performance. KPPs are used to prioritize maturation plans for technologies and novel system-level design strategies. The KPPs directly characterize the performance of the telescope by ensuring focal plane (image), exit pupil (wavefront) and light collecting capabilities of the telescope. The paper demonstrates that the chosen KPPs properly represent key science capabilities, as image size, sensitivity, photometric, and astrometric accuracy. It is also shown how detailed error budgets link the KPPs to component technical specifications that in turn are closely monitored by simulations. Integrated modeling is crucial for the performance-based systems engineering approach of defining and then evaluating the objective and threshold levels for the KPPs. As described in other GMTO paper at this conference, contributions from individual subsystems and components are modeled to determine their effect on system performance. We describe how GMTO has implemented KPPs and is now using them to guide and coordinate technical development.
Since 2015, W. M. Keck Observatory has been considering the possibility of conducting nighttime operations without any staff on the summit of Maunakea. A combination of methods has been used to assess the risk of this change in operations from different perspectives. System experts were surveyed to determine potential gaps in functionality that could create risk when operating or troubleshooting systems remotely. A hazard and risk analysis of use cases that describe nightly operations was conducted to identify risks to people, observatory equipment, and science quality and quantity that arise from the absence of people on the summit during the night. Risks were also identified by mining the night time fault reporting data from 2010-2016 to determine instances where hands on presence has been required on the summit to address issues. In the current state, these known issues would result in lost time and potential risk to equipment. The risk responses developed to address these risks have identified requirements on existing systems and for new capabilities to support unattended nighttime operations at WMKO.
KEYWORDS: Observatories, Systems engineering, Gemini Observatory, Reliability, Keck Observatory, Telescopes, Systems modeling, Document management, Process engineering, Visual process modeling
Remote operation of observatories has been a topic of interest for many years. This paper discusses a general approach to determining what it will take to transition from on-site summit nighttime operation to remote nighttime operation of a facility. It is informed by involvement in projects at Canada-France-Hawaii Telescope, Gemini Observatory, and W. M. Keck Observatory. While these projects had differences, they all shared the goals of upgrading an operating observatory that is on sky every night to improve efficiency of operations without negative impact on science. The approach combines project management (PMI) and systems engineering (INCOSE) methodologies and tools to develop an understanding of the impact on operations, determine scope and requirements for new capabilities as well as additional functionality for existing systems, identify and manage risks, and how to incrementally move toward remote operation by integrating changes into current operations along the way.
In 2015, W. M. Keck Observatory conducted a study of the feasibility of conducting nighttime operations on Maunakea without any staff on the mountain. The study was motivated by the possibility of long term operational costs savings as well as other expected benefits. The goals of the study were to understand the technical feasibility and risk as well as to provide labor and cost estimates for implementation. The results of the study would be used to inform a decision about whether or not to fund and initiate a formal project aimed at the development of this new unattended nighttime operating capability. In this paper we will describe the study process as well as a brief summary of the results including the identified viable design alternative, the risk analysis, and the scope of work. We will also share the decisions made as a result of the study and current status of related follow-on activity.
As part of the image quality (IQ) assessment and improvement initiative being carried out at the 3.6m Canada
France Hawaii Telescope (CFHT) on Mauna Kea, Hawaii, our objective in the work reported here is to obtain
a systematic assay of thermal sources within the dome and in the summit environment around the observatory,
and therefore mitigate their contributions to convective instability leading to 'dome seeing'. Toward this, we
undertook a nighttime overflight to capture thermal images with a calibrated infrared camera of the outer
structures of CFHT and the neighboring observatories on the summit ridge, as well as of a significant area
of the surrounding terrain. The same thermal camera was then used to image heat sources within the dome.
Using a convective heat transfer model, all these measured surface temperatures were converted to heat fluxes,
and thus used to build a thermal assay of the dome. In addition, using button type temperature loggers, we
simultaneously recorded the nighttime dome skin temperatures of CFHT and two other observatories over a
weeklong period to evaluate nighttime supercooling of the dome skin due to radiation to the cold night sky. As a
complementary goal we compared the efficacy of different paints and coatings used in observatories to minimize
this effect. Though similar studies have been carried out at other observatories, the results are rarely available
in published literature. Therefore, here we explain our methodologies, along with a detailed discussion of our
results and inferences to serve as a useful resource to the larger observing community.
In 2007, the Canada-France-Hawaii Telescope (CFHT) undertook a project to enable the remote control of the
observatory at the summit of Mauna Kea from a control room in the Headquarters building in Waimea. Instead of
having two people operating the telescope and performing the observations from the summit, this project will allow one
operator to remotely control the observatory and perform observations for the night. It is not possible to have one person
operate from the summit, as our Two Person Rule requires at least two people for work at the summit for safety reasons.
This paper will describe how systems engineering concepts have shaped the design of the project structure and
execution.
With the advent of Queue observing at the Canada-France-Hawaii Telescope (CFHT), much emphasis has been placed
on minimizing the overheads in the observing process. Ensuring telescope focus is a necessary overhead, but taking the
focus sequences required to keep focus during the night adds significant time. In order to nearly eliminate this overhead
without sacrificing good telescope focus, the necessary focus position for each instrument has been modeled as a
function of telescope temperature and position on the sky. The correct focus position is calculated instead of measured,
so focus updates are practically instantaneous. The model coefficients are updated with new data regularly. Automatic
focus using calculated focus positions has been implemented for MegaCam, WIRCam and ESPaDOnS.
C. Juramy, E. Barrelet, K. Schahmaneche, P. Bailly, W. Bertoli, C. Evrard, P. Ghislain, A. Guimard, J.-F. Huppert, D. Imbault, D. Laporte, H. Lebbolo, P. Repain, R. Sefri, A. Vallereau, D. Vincent, P. Antilogus, P. Astier, J. Guy, R. Pain, N. Regnault, R. Attapatu, T. Benedict, G. Barrick, J.-C. Cuillandre, S. Gajadhar, K. Ho, D. Salmon
We present the first results of the SuperNova Direct Illumination Calibration Experiment (SNDICE), installed
in January 2008 at the Canada France Hawaii Telescope. SNDICE is designed for the absolute calibration of
the instrumental response of a telescope in general, and for the control of systematic errors in the SuperNova
Legacy Survey (SNLS) on Megacam in particular. Since photometric calibration will a critical ingredient for
the cosmological results of future experiments involving instruments with large focal planes (like SNAP, LSST
and DUNE), SNDICE functions also as a real-size demonstrator for such a system of instrumental calibration.
SNDICE includes a calibrated source of 24 LEDs, chosen for their stability, spectral coverage, and their power,
sufficient for a flux of at least 100 electron/s/pixel on the camera. It includes also Cooled Large Area Photodiode
modules (CLAPs), which give a redundant measurement of the flux near the camera focal plane. Before installing
SNDICE on CFHT, we completed a full calibration of both subsystems, including a spectral relative calibration
and a 3D mapping of the beam emitted by each LED. At CFHT, SNDICE can be operated both to obtain a
complete one-shot absolute calibration of telescope transmission in all wavelengths for all filters with several
incident angles, and to monitor variations on different time scales.
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