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

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A first generation software product line for data acquisition systems in astronomy

A first generation software product line for data acquisitio...

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2nd conference on advanced software and control for Astronomy

作者： Lopez-Ruiz, J. C. Heradio, Rube Cerrada Somolinos, Jose Antonio Coz Fernandez, Jose Ramon Ramos, Pablo Lopez Instituto de Astrofísica de Canarias (Spain) Univ. Nacional a Distancia (Spain) Univ. de La Laguna (Spain)

ISBN: (纸本)9780819472298

This article presents a case study on developing a software product line for data acquisition systems in astronomy based on the Exemplar Driven Development methodology and the Exemplar Flexibilization Language tool. The main strategies to build the software product line are based on the domain commonality and variability, the incremental scope and the use of existing artifacts. It consists on a lean methodology with little impact on the organization, suitable for small projects, which reduces product line start-up time. software Product Lines focuses on creating a family of products instead of individual products. This approach has spectacular benefits on reducing the time to market, maintaining the know-how, reducing the development costs and increasing the quality of new products. The maintenance of the products is also enhanced since all the data acquisition systems share the same product line architecture.

关键词： software Product Lines methodologies reuse software architecture

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Cornell Caltech Atacama telescope Primary Mirror Surface Sensing and controllability

Cornell Caltech Atacama Telescope Primary Mirror Surface Sen...

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conference on Ground-Based and Airborne instrumentation for Astronomy II

作者： MacDonald, Daniel Woody, David Bradford, C. Matt Chamberlin, Richard Dragovan, Mark Goldsmith, Paul Radford, Simon Sebring, Thomas Zmuidzinas, Jonas CALTECH Jet Prop Lab 4800 Oak Grove Dr Pasadena CA 91109 USA CALTECH Pasadena CA 91125 USA Cornell Univ Ithaca NY 14853 USA

ISBN: (纸本)9780819472229

To meet the 10 mu m RMS half wavefront error requirement for the 25 m diameter Cornell Caltech Atacama telescope (CCAT), active control of the approximately 200 primary mirror panels is required. The CCAT baseline design includes carbon fiber aluminum honeycomb sandwich mirror panels. Distortions of the panels due to thermal gradients, gravity and the mounting scheme need to be taken into consideration in the control system design. We have modeled the primary mirror surface as both flat and curved surfaces and have investigated mirror controllability with a variety of sensor types and positions. To study different mirror segmentation schemes and find acceptable sensor configurations, we have created a software package that supports multiple segment shapes and reconfigurable panel sizing and orientation. It includes extensible sensor types and flexible positioning. Inclusion of panel and truss deformations allows modeling the effects of thermal and gravity distortions on mirror controllability. Flat mirrors and curved mirrors with the correct prescription give similar results for controlled modes, but show significant differences in the unsensed flat mirror modes. Both flat and curved mirror models show that sensing schemes that work well with rigid, thermally stable panels will not control a mirror with deformable panels. Sensors external to the mirror surface such as absolute distance measurement systems or Shack-Hartmann type sensors are required to deal with panel deformations. Using a combination of segment based sensors and external sensors we have created a promising prototype control system for the CCAT telescope.

关键词： CCAT large telescopes segmented mirrors mirror alignment telescope control

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Beating the cost curve and redefining the scientific telescope utility using 0.4-Meter Robotic Cluster Network

Beating the cost curve and redefining the scientific telesco...

引用

conference on Ground-Based and Airborne instrumentation for Astronomy II

作者： Dubberley, Matthew A. Walker, Zachary A. Haldeman, Benjamin J. Las Cumbres Observ Global Telescope Goleta CA 93117 USA

ISBN: (纸本)9780819472229

Las Cumbres Observatory Global telescope (LCOGT) is redefining the function of robotic telescopes by deploying 0.4 meter telescopes that act as a highly networked intelligent instrument. The 0.4 meter telescopes, (P4) are optimized for quick and accurate object acquisition and tracking. This minimizes response time and enables the leveraging of the instrument. A single P4 can independently execute multiple science programs concurrently or team up with other P4s for deeper or multi-color observations of a single target. The intelligent control software will optimize the observation schedule for each individual telescope and the entire network. LCOGT is deploying 6 networked clusters consisting of four P4s around the world, providing capacity and versatility beyond the classical observatory. Each P4 has zero slippage, no backlash friction systems, and is currently achieving 20 deg/s slewing. Blind pointing is currently 8 arcsec RMS. Using the AG acquisition routine, the drive will have repeatable pointing to within 0.6 arcsec within 12 seconds from anywhere on the sky. Other features include wind buffet correction, rapid thermalization, dual autoguiders, novel scanning flat fielding device, large 20 kg instrument capacity, high speed instrument changer, and a stiff split ring mount.

关键词： Robotic telescope Network Cost Friction Drive Direct Drive

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Design and Realization of the control System for the Three-channels Birefringent Filter

Design and Realization of the Control System for the Three-c...

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2nd conference on advanced software and control for Astronomy

作者： Zhu, Dan Nanjing Univ Posts & Telecommun Nanjing 210036 Peoples R China

ISBN: (纸本)9780819472298

Space Solar telescope is one of the large-scale scientific programs under development in China. In it, an important part is the filter, a birefringent filter with three-channels. It consists of 17 rotatable wave plates. In coordination with other mechanical and optical components, complicated and precise adjustments of their attitudes are necessary, which requests a high-accuracy control system to ensure their concertedness. The paper describes the design and realization of the control system. It mainly has a hardware plate and a software one. The former uses an industrial controller, a control card and step motors, while the latter uses the technique construction of the object oriented. That is modularization design with lengthwise dividing as per functions and breadthwise dividing as per element layers. Shift arithmetic for whole spectrum in programs is for intelligent spectral scanning. At the same time, the control information is roundly recorded in the data base of the system. Tests show that the system is characterized by high precision, good stabilization, high data safety and user-friendly interface, totally meeting the design requirements. Also discussed in this paper is some new conceivability to realize the handiness and miniaturization of the filter to fit the use in space flight in the future.

关键词： Three-channels Birefringent Filter control system software control card stepping motors object oriented modularization design

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The ALMA Computing Project - Initial Commissioning

The ALMA Computing Project - Initial Commissioning

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2nd conference on advanced software and control for Astronomy

作者： Glendenning, B. E. Raffi, G. Natl Radio Astron Observ Socorro NM 87801 USA European Southern Observ Garching Germany

ISBN: (纸本)9780819472298

The Atacama Large Millimeter/Submillimeter Array (ALMA) is a large radio interferometric telescope consisting of 66 antennas with variable positions, to be located at the Chajnantor 5000mat a high site (5000m) in Chile. ALMA commissioning has now started with the arrival of several antennas in Chile and will continue for the next 4 years. The ALMA software was from the beginning has been developed as an end-to-end system including: proposal preparation, dynamic scheduling, instrument control, data handling and formatting, data archiving and retrieval, automatic and manual data processing systems, and support for observatory operations. This presentation will expand mostly on ALMA software aspects issues on which we are concentrating in this phase: management, procedures, testing and validation. While software development was based on a common software infrastructure (ALMA Common software - ACS) from the beginning, end-to-end testing was limited by the hardware available, and was possible for years until recently only on computer models. Although the control software was available early in prototype stand-alone form to support testing of prototypes antennas, it was only recently that dynamic interferometry was reached and software could be tested end to end with a somewhat stable hardware platform. The lessons learned so far will be explained, in particular the need for a realistic validation environment, the balance to be achieved between incremental development and the needed for stability and usability, and the way to achieve all the above with a development team distributed over three four continents. Some general lessons can be drown drawn on the potential conflicts between software and system (hardware) testing, or in other words on the danger in taking short-cuts in software testing and validation.

关键词： ALMA Common software control software Commissioning Management Distributed Development

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High performance astronomical data communications in the LSST Data Management System

High performance astronomical data communications in the LSS...

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2nd conference on advanced software and control for Astronomy

作者： Kantor, Jeff Lambert, Ron Cox, Chip Levine, Deborah Smith, Chris Jagatheeson, Arun Cribbs, Chris LSST Corp. (United States) WHREN-LILA (United States) California Institute of Technology (United States)

ISBN: (纸本)9780819472298

The Large Synoptic Survey telescope (LSST) is an 8.4m (6.5m effective), wide-field (9.6 degree2), ground-based telescope with a 3.2 GPixel camera. It will survey over 20,000 degree2 with 1,000 re-visits over 10 years in six visible bands, and is scheduled to begin full scientific operations in 2016. The Data Management System will acquire and process the images, issue transient alerts, and catalog the world's largest database of optical astronomical data. Every 24 hours, 15 terabytes of raw data will be transferred via redundant 10 Gbps fiber optics down from the mountain summit at Cerro Pachon, Chile to the Base Facility in La Serena for transient alert processing. Simultaneously, the data will be transferred at 2.5Gbps over fiber optics to the Archive Center in Champaign, Illinois for archiving and further scientific processing and creation of scientific data catalogs. Finally, the Archive Center will distribute the processed data and catalogs at 10Gbps to a number Data Access Centers for scientific educational, and public access. Redundant storage and network bandwidth is built into the design of the system. The current networking acquistiion strategy involves leveraging existing dark fiber to handle within Chile, Chile - U.S. and within U.S. links. There are a significant number of carriers and networks involved and coordinating the acquisition, deployment, and operations of this capability. advanced protocols are being investigated during our Research and Development phase to address anticipated challenges in effective utilization. We describe the data communications requirements, architecture, and acquisition strategy in this paper.

关键词： Large Synoptic Survey telescope Data centers Data archive systems Astronomy Cameras Data communications Lanthanum telescopes Imaging systems control systems

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The software development process at the Chandra X-ray Center

The software development process at the Chandra X-ray Center

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2nd conference on advanced software and control for Astronomy

作者： Evans, Janet D. Evans, Ian N. Fabbiano, Giuseppina Smithsonian Astrophys Observ Cambridge MA 02138 USA

ISBN: (纸本)9780819472298

software development for the Chandra X-ray Center Data System began in the mid 1990's, and the waterfall model of development was mandated by our documents. Although we initially tried this approach, we found that a process with elements of the spiral model worked better in our science-based environment. High-level science requirements are usually established by scientists, and provided to the software development group. We follow with review and refinement of those requirements prior to the design phase. Design reviews are conducted for substantial projects within the development team, and include scientists whenever appropriate. Development follows agreed upon schedules that include several internal releases of the task before completion. Feedback from science testing early in the process helps to identify and resolve misunderstandings present in the detailed requirements, and allows review of intangible requirements. The development process includes specific testing of requirements, developer and user documentation, and support after deployment to operations or to users. We discuss the process we follow at the Chandra X-ray Center (CXC) to develop software and support operations. We review the role of the science and development staff from conception to release of software, and some lessons learned from managing CXC software development for over a decade.

关键词： data processing development processes software development system architecture

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Launching GUPPI: the Green Bank Ultimate Pulsar Processing Instrument

Launching GUPPI: the Green Bank Ultimate Pulsar Processing I...

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2nd conference on advanced software and control for Astronomy

作者： DuPlain, Ron Ransom, Scott Demorest, Paul Brandt, Patrick Ford, John Shelton, Amy L. Natl Radio Astron Observ 520 Edgemont Rd Charlottesville VA 22903 USA Natl Radio Astron Observ Green Bank WV 24944 USA

ISBN: (纸本)9780819472298

The National Radio Astronomy Observatory (NRAO) is launching the Green Bank Ultimate Pulsar Processing Instrument (GUPPI), a prototype flexible digital signal processor designed for pulsar observations with the Robert C. Byrd Green Bank telescope (GBT). GUPPI uses field programmable gate array (FPGA) hardware and design tools developed by the Center for Astronomy Signal Processing and Electronics Research (CASPER) at the University of California, Berkeley. The NRAO has been concurrently developing GUPPI software and hardware using minimal software resources. The software handles instrument monitor and control, data acquisition, and hardware interfacing. GUPPI is currently an expert-only spectrometer, but supports future integration with the full GBT production system. The NRAO was able to take advantage of the unique flexibility of the CASPER FPGA hardware platform, develop hardware and software in parallel, and build a suite of software tools for monitoring, controlling, and acquiring data with a new instrument over a short timeline of just a few months. The NRAO interacts regularly with CASPER and its users, and GUPPI stands as an example of what reconfigurable computing and open-source development can do for radio astronomy. GUPPI is modular for portability, and the NRAO provides the results of development as an open-source resource.

关键词： pulsar FPGA agile development rapid application development instrument control data acquisition hardware interface Berkeley Emulation Engine (BEE)

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The GTC primary mirror control system

The GTC primary mirror control system

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2nd conference on advanced software and control for Astronomy

作者： Lefort, B. Castro, J. Inst Astrofis Canarias GTC Project Tenerife 38200 Spain

ISBN: (纸本)9780819472298

The Gran Telescopio Canarias (GTC) primary mirror control system is responsible for making the 36 segments behave like a monolithic mirror. It deals with 108 positioners giving 3 degrees of freedom to each segment, 168 position sensors installed between adjacent segments measuring nanometrical displacements, 216 actuators controling the figure of each segment creating torques, 216 load cells quantifying the applied deforming forces and 216 PT100 monitoring the primary mirror temperature gradient to predict structural dilatations. It provides simple engineering access to all functionalities of each device as well as real time capabilities required to work in closed-loop. All the critical parameters can be monitored from any observatory's workstation thanks to the fully embedded distributed environment included in the control system framework. Hardware interfaces as VME, CAN field buses are fully transparent for the user thanks to the Java front-end (inspector) that allows to start, control and turn-off each part of the system with a simple mouse click.

关键词： GTC active optics control CAN

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KISIP: A software Package for Speckle Interferometry of Adaptive Optics Corrected Solar Data

KISIP: A Software Package for Speckle Interferometry of Adap...

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2nd conference on advanced software and control for Astronomy

作者： Woeger, Friedrich von der Luehe, Oskar Natl Solar Observ POB 62 Sunspot NM 88349 USA Kiepenheuer Inst Sonnenphysik D-79104 Freiberg Germany

ISBN: (纸本)9780819472298

We present a speckle interferometry code for solar data taken with the help of an adaptive optics (AO) system. As any AO correction is only partial there is a need to use post-facto reconstruction algorithms to achieve the diffraction limit of the telescope over a large field of view most of the observational time. However, data rates of current and future solar telescopes are ever increasing with camera, chip sizes. In order to overcome the tedious and expensive data handling, we investigate the possibility to use the presented speckle reconstruction program in a real-time application at telescope sites themselves. The program features Fourier phase reconstruction algorithms using either an extended Knox-Thompson or a triple correlation scheme. The Fourier amplitude reconstruction has been adjusted for use with models that take the correction of an AO system into account. The code has been written in the C programming language and optimized for parallel processing in a multi-processor environment. We analyze the scalability of the code to find possible bottlenecks. Finally, the phase reconstruction accuracy is validated by comparison of reconstructed data with satellite data. We conclude that the presented code is capable to run in future real-time reconstruction applications at solar telescopes if care is taken that the multi-processor environments have low latencies between the processing nodes.

关键词： adaptive optics image reconstruction speckle interferometry

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