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检索条件"任意字段=Conference on Advanced Telescope and Instrumentation Control Software"

共 1190 条记录，以下是141-150 订阅

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Reactivation of the Active Mass Damping system for SOFIA to improve image stability 8

Reactivation of the Active Mass Damping system for SOFIA to ...

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conference on Ground-Based and Airborne telescopes VIII Part of SPIE Astronomical telescopes + instrumentation conference

作者： Greiner, Benjamin Brewster, Rick Mrzyglod, Anja Wagner, Joerg Univ Stuttgart Deutsch SOFIA Inst Pfaffenwaldring 29 D-70569 Stuttgart Germany NASA Ames Res Ctr Moffett Field CA 94035 USA

ISBN: (纸本)9781510636781

The Stratospheric Observatory for Infrared Astronomy (SOFIA) employs an airborne telescope with a 2.7 m primary mirror. The telescope structure is composed of carbon fibre with major parts of steel for the suspension and balancing components. It is exposed to harsh environmental conditions and subject to vibration excitation due to aircraft motions and turbulence from the airflow coming into the telescope cavity. To meet pointing requirements and improve image stability there are ongoing efforts on various components of the telescope system, one of which is the implementation of an Active Mass Damping (AMD) control system: Based on accelerometer signals, reaction mass actuators impose forces onto the support structure to dampen the vibration of optical components. The system has been designed, implemented and preliminary tested in the early years of SOFIA's scientific operation, but concerns about the structural integrity of the primary mirror and new requirements regarding software qualification have prevented the activation and further development for several years. These concerns being addressed, we are now in the process of reactivating the AMD system on the support structure of the primary mirror. Recent ground tests and in-flight jitter measurements indicate that the damping system is very efficient at eliminating the excitation of targeted structural modes of the telescope structure at 40 to 80 Hz and the first bending modes of the primary mirror at 175 Hz, resulting in a significantly improved image quality. This paper presents the analysis of those measurements and discusses options for future development.

关键词： SOFIA AMD Active Mass Damping active control vibration jitter

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A Novel Power and Communications Hub: The GMT EtherCAT and Power Hub 6

A Novel Power and Communications Hub: The GMT EtherCAT and P...

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conference on software and Cyberinfrastructure for Astronomy VI held as Part of SPIE Astronomical telescopes and instrumentation conference

作者： Ford, John M. Ranka, Trupti Salanski, Thomas Univ Arizona Steward Observ Tucson AZ 85721 USA Giant Magellan Telescope Org Pasadena CA USA

ISBN: (纸本)9781510636927

Each of the seven primary mirror cell in the GMT contains over 225 EtherCAT slaves in the cell, leading to a nightmare of cabling. Optimization of the initial construction and ongoing maintenance of the cells requires reduced complexity of wiring in the cell. Employing the concept of Power over EtherCAT and a star configuration, the resulting the EtherCAT Power and Communications Hub design reduces the wiring in the cell by 2/3, while additionally providing centralized power management and diagnosis of each actuator communications link. The design consists of an EtherCAT slave to allow the central control system to monitor and control the slaves attached to the hub, and power control circuits to provide and monitor power to each slave. In addition to providing a significant reduction in wiring complexity, the hub serves as an additional control point for power to each support actuator, enhancing mirror safety through redundant control of the actuators. This paper describes the motivation driving the requirements, the resulting requirements and design, and test results of the prototype EtherCAT and Power Hubs.

关键词： EtherCAT Power over Ethernet

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The NEID Port Adapter at WIYN: Tip-tilt control and vibration analysis 8

The NEID Port Adapter at WIYN: Tip-tilt control and vibratio...

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conference on Ground-based and Airborne instrumentation for Astronomy VIII

作者： McBride, William Rajagopal, Jayadev Percival, Jeffrey W. Timmermann, Erik Logsdon, Sarah E. Wolf, Marsha J. Everett, Mark Gong, Qian Golub, Eli Hunting, Emily Jaehnig, Kurt P. Klusmeyer, Jessica Li, Dan Liang, Ming Liu, Wilson Mahadevan, Suvrath McElwain, Michael W. Ridgway, Susan Schweiker, Heidi Smith, Michael P. Higuera, Jesus Santoro, Fernado Schwab, Christian NSFs Natl Opt Infrared Astron Res Lab 950 N Cherry Ave Tucson AZ 85719 USA Univ Wisconsin Madison Madison WI USA Penn State Univ University Pk PA 16802 USA NASA Goddard Space Flight Ctr Washington DC 20546 USA ASTRO LLC Lakewood Ranch FL USA Macquarie Univ Sydney NSW Australia

ISBN: (纸本)9781510636828

The NEID extreme precision radial velocity spectrometer is being commissioned at the WIYN 3.5 meter telescope, Kitt Peak National Observatory, Tucson Arizona. In order to meet the stringent 27 cm per second radial velocity precision, the light to NEID comes from an extremely stable fiber feed, called the NEID Port Adapter, equipped with fast tip-tilt correction. The WIYN telescope vibration environment and the Port Adapter tip-tilt and guiding system are key to achieving the 50 milliarcsecond-level centroiding stability required. Here we describe the servo system performance, along with vibration analysis and mitigation plans. This work would be relevant to upgrade and retrofit efforts as older observatories incorporate low-order wavefront correction to stabilize light to advanced spectrometers and imagers.

关键词： WIYN NEID telescope port adapter tip-tilt vibration jitter

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Remote Monitor and control Implementation via an Optical Digital Link 9

Remote Monitor and Control Implementation via an Optical Dig...

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conference on X-Ray, Optical, and Infrared Detectors for Astronomy IX as part of SPIE Astronomical telescopes + instrumentation conference

作者： Ljusic, Zoran Caputa, Krzysztof Zhao, Erning Natl Res Council Canada Dominion Radio Astrophys Observ 717 White Lake Rd Kaleden BC V0H 1K0 Canada Natl Res Council Canada Dominion Radio Astrophys Observ 717 White Saanich Rd Victoria BC V9E 2E7 Canada

ISBN: (纸本)9781510636965

The Single Pixel Feed Receiver (SPFRx) is a Sub-Element of the Square Kilometer Array (SKA) Dish Element. Its main function is receiving RF signals captured by the SKA-mid Dish (DSH) and pre-amplified by the Single Pixel Feed (SPF) Sub-Element components. The main tasks of the SPFRx hardware, firmware, and software is to perform analog to digital conversion on the incoming RF signals and to send the digital RF samples to the SKA Central Signal Processing (CSP) Element as 100G Ethernet packets. For analog to digital conversion,of SKA-mid Bands 1- 3 a 12-bit Analog to Digital Converter (ADC) is used. The ADC and its supporting electronics reside on an electronic board placed within a metal box on the telescope's indexer. A number of measures are taken to minimize Radio Frequency Interference (RFI) created by the switching elements on the board. One of the major measures is using an optical link for performing monitor and control function of the internal electronics by the Local Monitor control (LMC) module residing within the telescope's base.

关键词： SKA ADC optical RFI1

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Developing a preliminary design of FPGA based control rod system for a high temperature experimental power reactor

Developing a preliminary design of FPGA based control rod sy...

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2021 International conference on High-Temperature Reactor Technology, HTR 2021

作者： Santoso, Sigit Suryono, Tulis Jojok Maerani, Restu Atmoko, Dian Fitri Manurung, Auralius Center for Nuclear Reactor Technology and Safety-BATAN Puspiptek Area South Tangerang SetuI5310 Indonesia Center for Engineering of Nuclear Facility-BATAN 3 Puspiptek Area South Tangerang SetuI5310 Indonesia Department of Mechanical Engineering Universitas Pertamina Jakarta Selatan12220 Indonesia

An Experimental Power Reactor (Reaktor Daya Experimental, RDE) which is based on high-temperature gas-cooled reactor technology is being developed in Indonesia during recent years. As an advanced reactor design type, a fully digital- based I&C would be employed in the design of RDE reactor monitoring and control including the control rod drive system. On the other hand, some of the major issues discussed in the licensing process for such digital I&C are the possibility that a common cause failure can undermine the reactor protection function and the vulnerable to cyber-attack possibility. Therefore, a number of the defense in depth measures need to be applied to I&C systems design help to mitigate those issues. This paper discusses the design process for employing FPGA based digital system in the control rod drive system of RDE. The methodology follows the life cycle process of instrumentation and control architecture and software development which is presented in the V shape model. A generic control rod system prototype which consists of a control rod motor driver, control rod handling system, magnetic handling, and the motor system was prepared and would be used as an object in the FPGA implementation. The result of the process design conducted in this current phase study shows the implementation of FPGA-based digital technology will enable to minimize the lack of a digital based control rod drive system. However, appropriate testing and verification of the design developed are required to ensure better performance of the control rod drive system. © 2021 Institute of Physics Publishing. All rights reserved.

关键词： Life cycle

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The University of Tokyo Atacama Observatory 6.5 m telescope: Development of the telescope and the control System 8

The University of Tokyo Atacama Observatory 6.5 m telescope:...

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conference on Ground-Based and Airborne telescopes VIII Part of SPIE Astronomical telescopes + instrumentation conference

作者： Minezaki, Takeo Morokuma, Tomoki Yoshii, Yuzuru Doi, Mamoru Miyata, Takashi Kohno, Kotaro Tanaka, Masuo Motohara, Kentaro Sako, Shigeyuki Tanabe, Toshihiko Hatsukade, Bunyo Konishi, Masahiro Takahashi, Hidenori Kamizuka, Takafumi Sameshima, Hiroaki Asano, Kentaro Kato, Natsuko M. Numata, Mizuki Aoki, Tsutomu Soyano, Takao Tarusawa, Ken'ichi Nishimura, Mitsufumi Seki, Takayuki Kajitani, Naruyo Ikeda, Yuji Yoshikawa, Tomoshiro Matsumoto, Yoshitaka Nakamaru, Shintaro Univ Tokyo Grad Sch Sci Inst Astron 2-21-1 Osawa Mitaka Tokyo 1810015 Japan Univ Arizona Steward Observ 933 North Cherry AveRoom N204 Tucson AZ 85721 USA Natl Astron Observ Japan Adv Techonol Ctr 2-21-1 Osawa Mitaka Tokyo 1810015 Japan Univ Tokyo Sch Sci Inst Astron Kiso Observ 10762-30 Mitake Kiso Nagano 3970101 Japan Nishimura Co Ltd Minami Ku 10 Shirikiricho Kyoto Kyoto 6018115 Japan Kyoto Nijikoubou Co Ltd Sakyo Ku 17-203 Iwakura Minami Osagicho Kyoto Kyoto Japan Kishiro Co Ltd 2-3-20 Tenmoncho Akashi Hyogo 6730881 Japan

ISBN: (纸本)9781510636781

The University of Tokyo Atacama Observatory Project is to construct a 6.5 m infrared-optimized telescope at the summit of Co. Chajnantor (5640 m altitude) in northern Chile. The telescope optics uses a Ritchey-Chretien type layout, with an under-sized secondary mirror to reduce stray light caused by thermal emission from the telescope structure. The primary mirror is a F/1.25 lightweight borosilicate glass (Ohara E6) mirror with honeycomb structure, which is developed by Steward Observatory Richard F. Caris Mirror Lab. The telescope has two Nasmyth foci and two folded-Cassegrain foci, which can be switched by rotating a tertiary mirror. The final focal ratio is 12.2 with a field of view of 25 arcmin in diameter. The telescope mount is a tripod-disk alt-azimuth mount. Both the azimuth and elevation axes are supported by and run on hydrostatic bearings, and they are driven by friction drives with servo motors, which are controlled by the telescope control system. It also controls the hexapod mount of the secondary mirror and the pneumatic actuators of the primary mirror support to keep good image quality during the observation. An off-axis Shack-Hartmann sensor installed in each focus measures the wavefront aberration of the telescope optics, then the misalignment between the secondary and primary mirrors is corrected by adjusting the hexapod mount while other aberrations are corrected by the deformation of the primary mirror. The force distribution of the actuators for correction will be calculated by fitting the wave-front errors with a series of bending modes of the primary mirror.

关键词： TAO telescope infrared optical mount active optics control system

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The Purpose, Plan, and Progress of the Giant Magellan telescope Primary Mirror Off-Axis Segment Test Cell 8

The Purpose, Plan, and Progress of the Giant Magellan Telesc...

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conference on Ground-Based and Airborne telescopes VIII Part of SPIE Astronomical telescopes + instrumentation conference

作者： Fischer, Barbara Ranka, Trupti Aguayo, Francisco Ashby, David Bugueno, Erich Everman, Austin Ford, John Kechichian, Zaven Kenagy, Kurt Krasuski, Tomas Muller, Gary Rosenthal, Wylie Schwartz, David Soto, Jose Swett, Hector Thanasekaran, Divya Wadhavkar, Abhijit Giant Magellan Telescope Org 465 N Halstead StSuite 250 Pasadena CA 91107 USA Univ Arizona Tucson AZ 85721 USA

ISBN: (纸本)9781510636781

Large aperture telescopes require active control to maintain focus, collimation, and correct figure errors in the Primary Mirror (M1) due to gravity and thermal deformations. The Giant Magellan telescope (GMT) M1 active optics subsystem consists of the hardware and software that controls the shape, position, and thermal state of each mirror segment. Pneumatic force actuators support the weight and control the surface figure while linear position actuators control the six solid-body degrees of freedom of each mirror segment. A forced convection system comprised of fan-heat exchanger units control the mean temperature and thermal gradient of each mirror segment. The M1 Subsystem design leverages existing technology and employs innovations driven by more demanding requirements compared to heritage systems. These differences led to the identification of three key GMT project risks: determining if the vibration environment induced by the fan-heat exchanger units and the error in the applied influence functions required to shape the mirror are within image quality budget allocations. The third risk is incorporating damping to the force actuators to meet the seismic requirements. GMT is currently mitigating these risks by integrating a fully functional off-axis M1 Test Cell at the University of Arizona's Richard F. Canis Mirror Lab. This paper summarizes our requirements and design presented at the M1 Subsystem Preliminary Design Review in June 2019, describes our risk burn-down strategy for the M1 Subsystem, and presents our integration and test progress of the M1 Test Cell.

关键词： Test Cell Primary Mirror Active Optics Force Actuators Hardpoints Thermal control control System Damping

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SkyLab - Research and Development Facility for Ground-based Observations 8

SkyLab - Research and Development Facility for Ground-based ...

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conference on Ground-Based and Airborne telescopes VIII Part of SPIE Astronomical telescopes + instrumentation conference

作者： Kozlowski, Stanislaw Pazderski, Dariusz Krysiak, Bartlomiej Patelski, Radoslaw Jedwabny, Tomasz Kozlowski, Krzysztof Sybis, Michal Poznan Univ Tech Inst Automat Control & Robot Poznan Poland Poznan Univ Tech Inst Radiocommun Poznan Poland

ISBN: (纸本)9781510636781

The paper is focused on presentation of the fully autonomous observation SkyLab laboratory which was established recently to support research in the field of astronomical instrumentation and surveillance-related surveys. This facility is operated by the Poznan University of Technology. The main purpose of this laboratory is to provide new hardware and software technologies for precise tracking of sidereal and non-sidereal targets using 0.5 to 1.0 meter class telescopes. In particular, in this paper we take into account the robotized high-speed altazimuth mount equipped with direct-drive motors which was built specifically for the project. The mechanical design of the mount and the application of robust control algorithms make it possible to achieve high speed of operation and high tracking accuracy. We present experimental evaluation of the mount characteristics. In order to quantify precision of the instrument we present results of real observation scenarios concerning tracking of Low Earth Orbit satellites.

关键词： Robotized telescope mount observatory infrastructure laboratory space surveillance and NEO applications autonomous observatories

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The segmented pupil experiment for exoplanet detection. 4. A versatile image-based wavefront sensor for active optics 8

The segmented pupil experiment for exoplanet detection. 4. A...

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conference on Ground-based and Airborne instrumentation for Astronomy VIII

作者： Martinez, P. Gouvret, C. Marcotto, A. Dejonghe, J. Spang, A. Beaulieu, M. Preis Doyen, G. Le Duigou, J. M. Univ Cote dAzur Observ Cote dAzur CNRS Lab Lagrange Nice France Ctr Natl Etud Spatiales 18 Ave Edouard Belin F-31401 Toulouse 9 France

ISBN: (纸本)9781510636828

SPEED - the segmented pupil experiment for exoplanet detection - currently in final integration phase, is designed to test strategies and technologies for high-contrast instrumentation with segmented telescopes by offering an ideal cocoon to progress in these domains with complex telescope apertures. SPEED combines precision segment phasing architectures, optimised small inner-working angle (IWA) coronagraphy, and wavefront shaping to create a small IWA and small field of view (FoV) dark hole in the science detector. Over the years SPEED has made significant hardware and software progress to start the exploitation of the bench. We have completed several key hardware including the common-path wavefront sensor for cophasing optics based on the self-coherent camera (SCC) concept. In this paper, we report on the wavefront sensing strategy designed for SPEED, from the adaptation of the SCC concept to cophasing optics towards an alternative implementation of the conventional SCC, called the fast-modulated SCC, for both wavefront control and shaping applications. We present a progress overview on this wavefront sensor for (i) cophasing control and monitoring from the scientific image, as well as (ii) its interest for the wavefront shaping unit of the bench.

关键词： Exoplanets wavefront control active optics extremely large telescopes instrumentation

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ProExtor: Mining API Protocols for Program Vulnerability Detection 21

ProExtor: Mining API Protocols for Program Vulnerability Det...

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Proceedings of the 3rd International conference on advanced Information Science and System

作者： Huijia Ye Juwei Rao Yang Shi Zhihua Li Electric Power Dispatching Control Center Meizhou Power Supply Bureau China

ISBN: (纸本)9781450385862

API protocols play an important role in program verification, testing, evolution and other phases of the software development process. Many approaches have been proposed to mine API protocols automatically from programs. However, few tools are available, especially dynamical API protocol mining tools. In this paper, we present a dynamical API protocol mining tool for Java programs: ProExtor. Our tool mines API protocols in an online mode based on the instrumentation technique of Java agent. For each class, it produces two models: a probabilistic model and a deterministic model. The probabilistic model will be evolved persistently when more application programs are fed for mining. The deterministic model is transformed from the latest probabilistic model, which can be used for program verification, testing, evolution, etc. Both models can be visualized with the software Graphviz. We elaborate design and implementation details of our tool and an application to a real-world program. We believe our work is a good reference for the development of similar tools.

关键词： Program Dynamic Analysis

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