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software architecture for OSIRIS: an infrared integral-field spectrograph for the Keck adaptive optics system

Software architecture for OSIRIS: an infrared integral-field...

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conference on advanced telescope and instrumentation control software ii

作者： Weiss, JL Barczys, M Larkin, JE LaFreniere, D Quirrenbach, A Gasaway, TM Krabbe, A Univ. of California/Los Angeles (United States) Univ. of California/San Diego (United States) Univ. of California/Berkeley (United States)

ISBN: (纸本)0819446270

OSIRIS is an infrared integral-field spectrograph being built for the Keck AO system. OSIRIS presents novel data reduction and user-interaction challenges which are addressed by software being developed for OSIRIS. The complex raw data frames, containing up to 4096 interleaved spectra, are reduced in real-time and meaningfully displayed for quality-of-observation feedback to observers. Following an observing night, data are optimally reduced to science-quality data cubes in a semi-automated fashion. Further, the software must efficiently coordinate OSIRIS' spectroscopic observations with the SHARC off-axis imager and the AO system. To meet these demands, OSIRIS software is comprehensive and integrates the planning, execution, and reduction of observations. Facilitating this architecture is the formulation of observations into 'datasets', rather than into individual frames. Datasets are functional groups of frames organized by the needs and capabilities of the data reduction software (DRS). A typical dataset consists of dithered OSIRIS observations, coupled with associated off-axis AO PSF imagery from SHARC. A Java-based planning tool enables 'sequences' of datasets to be planned and saved both prior to and during observing sessions. An execution client interprets these XML-based files, and configures the hardware servers for OSIRIS, SHARC, and AO before executing the observations. As observations are completed, extensive information about the instrument and observatory are collated in an archival relational database. The DRS then uses information in the database, as well as archived calibration data and SHARC PSF data to produce a final science-quality data product, which may include differential refraction corrections, 3D PSF modeling/deconvolution, and OH-suppression.

关键词： control software data reduction observation planning astronomical instrumentation integral-field spectroscopy infrared adaptive optics data cube

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Update on the Subaru Cassegrain Instrument Automatic Exchanger control system

Update on the Subaru Cassegrain Instrument Automatic Exchang...

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conference on advanced telescope and instrumentation control software ii

作者： Omata, K Usuda, T Yutani, M Nishimura, T Sawada, S Natl Astron Observ Subaru Telescope Hilo HI 96720 USA

ISBN: (纸本)0819446270

We report on the status of the Cassegrain Instrument Automatic Exchanger (CIAX) control system for the Subaru telescope. Devices controlled by a shell program in the previous version are now controlled by a macro. It can now be operated safely from remote site. Features of the new system are: 1. New macro. The new macro has two features: (1) Action skip. The macro can skip actions that have been executed earlier. It judges whether to skip by checking the status of devices. Resumption of interrupted macro or reversal from halfway of a process is possible. (2) Macro flexibility: The script has every possible sequential action and chooses actions by checking device status. For instance, it can determine whether the cart is at the telescope or at one of the instrument standby flanges and select a proper hookup command. 2. GUI for macro operation and CGI for rewriting setup files. The new GUI uses a commercial instrument control language. A CGI application accesses setup files. 3. Onmi-directional Infrared (IR) LAN. Omnidirectional IR LAN is being tested for the cart because radio frequency wireless LAN is prohibited on Mauna Kea to avoid interference to radio telescopes. Conventional IR LAN failed because of its directionality. The CIAX system is now routinely used for instrument exchange. For complete automatic operation, there are still a few tasks left, such as macro-controlled instrument shutdown and restarting, standardizing interfaces and procedure for all instruments and further increasing reliability which is higher already compared to conventional manual exchange.

关键词： auto exchanger Cassegrain instruments observation efficiency automatic cart Subaru telescope PLC

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Keywords revisited

Keywords revisited

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conference on advanced Global Communications Technologies for Astronomy ii

作者： Kwok, SH Cohen, RW WM Keck Observ Calif Assoc Res Astron Kamuela HI 96743 USA

ISBN: (纸本)0819446246

Keywords, a concept that uses named parameters to access information from devices and instruments, originated in the early 1990s and is the foundation of the Keck Task Library, KTL. KTL uses different underlying communication schemes to provide a consistent API to a diversity of client applications. Increasing instrument complexity, the need to integrate multiple subsystems into a unified whole, and the demand for greater flexibility and productivity in the software development process, has prompted us to review the concept of keywords and its implementation. In this paper, we discuss the application of modern software methodology and communication protocols to enhance the Keck Task Library.

关键词： telescope control Keck observatory keywords inter-process communication

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LUCIFER control software: An OO approach using CORBA technology

LUCIFER control software: An OO approach using CORBA technol...

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advanced telescope and instrumentation control software ii

作者： Jütte, Marcus Polsterer, Kai Lehmitz, Michael Dettmar, Ralf-Jürgen Astronomisches Institut Ruhr-Universität Bochum Universitätsstr. 150 D-44780 Bochum Germany Landessternwarte Königsstuhl 12 69117 Heidelberg Germany

In this paper we present the design of the control software for the LET NIR spectroscopic Utility with Camera and Integral- Field Unit for Extragalactic Research (LUCIFER) which is one of the first-light instruments for the Large Binocular telescope (LBT) on Mt. Graham, Arizona. The LBT will be equipped with two identical LUCIFER instruments for both mirrors. Furthermore we give an overview of the intended hardware structure of the instrument. Since the project requires a detailed and exact modeling of the software we present UML diagrams starting with an overall model down to use case, activity and class diagrams including an example for one special instrument unit.

关键词： Optical telescopes

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e-STAR: a distributed telescope network

e-STAR: a distributed telescope network

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conference on advanced Global Communications Technologies for Astronomy ii

作者： Steele, IA Naylor, T Allan, A Etherton, J Mottram, CJ Liverpool JMU Astrophys Res Inst Liverpool CH41 1LD Merseyside England

ISBN: (纸本)0819446246

The e-STAR (e-Science telescopes for Astronomical Research) project uses GRID techniques to develop the software infrastructure for a global network of robotic telescopes. The basic architecture is based around Intelligent Agents which request data from Discovery Nodes that may be telescopes or databases. Communication is based on a development of the XML RTML language secured using the Globus I/O library, with status serving provided via LDAP. We describe the system architecture and protocols devised to give a distributed approach to telescope scheduling, as well as giving details of the implementation of prototype Intelligent Agent and Discovery Node systems.

关键词： telescopes networks robotic XML GRID software scheduling

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Overview of the control system for the Keck Interferometer

Overview of the control system for the Keck Interferometer

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conference on advanced telescope and instrumentation control software ii

作者： Booth, AJ Eychaner, G Hovland, E Johnson, RL Lupton, W Niessner, A Palmer, D Reder, LJ Rudeen, AC Smythe, RF Tsubota, K CALTECH Jet Propuls Lab Pasadena CA 91109 USA

ISBN: (纸本)0819446270

The Keck Interferometer links the two 10m Keck telescopes located atop Mauna Kea in Hawaii. It is the first 10m class, fully AO equipped interferometer to enter operation. Further, it is the first large interferometer designed to be handed over from a design and implementation team to a separate operations team, and be used by astronomers who are not interferometer specialists. As such it offers unique challenges in reducing an extremely complex and powerful system to an apparently simple user interface, and providing a well engineered system that can be maintained by people who did not develop it. This paper gives an overview of the control system that has been implemented for the single baseline operation of the instrument, and indicates how this will be extended to allow control of the future modes of the instrument (nulling, differential phase and astrometry). The control system has several parts. One is for control of "slow" sub-systems, which is based in the EPICS architecture, already ubiquitous at the Keck Observatory. Another, used to control hard real time sub-systems, is based on a new infrastructure developed at JPL, programmed in C++, Java, and using CORBA for communication. This infrastructure has been developed specifically with the problems of interferometric control in mind and is used in JPL's flight testbeds, as well as the Keck Interferometer. Finally, a user interface and high level control layer is in development using a variety of tools including UML based modeling in the Rhapsody tool (using C++ and CORBA), Java, and Tcl/Tk for prototyping.

关键词： interferometry control system real time control

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Utilizing Internet technologies in Observatory control Systems

Utilizing Internet technologies in Observatory Control Syste...

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conference on advanced telescope and instrumentation control software ii

作者： Cording, D Electroopt Syst Queanbeyan NSW 2620 Australia

ISBN: (纸本)0819446270

The Internet boom of the past few years has spurred the development of a number of technologies to provide services such as secure communications, reliable messaging, information publishing and application distribution for commercial applications. Over the same period a new generation of computer languages have also developed to provide object oriented design and development, improved safety and reliability, and cross platform compatibility. Whilst the business models of the '***' era proved to be largely unviable, the technologies that they were based upon have survived. In the past eighteen months these technologies have matured to the point were they can now be utilized to build secure, robust and complete observatory control control systems. This paper will describe how Electro Optic Systems has utilized these technologies in the development of its third generation Robotic Observatory control System (ROCS). ROCS provides an extremely flexible configuration capability within a control system structure to provide truly autonomous robotic observatory operation including observation scheduling. ROCS was built using Internet technologies such as Java, Java Messaging Service (JMS), Lightweight Directory Access Protocol (LDAP), Secure Sockets Layer (SSL), eXtendible Markup Language (XML), Hypertext Transport Protocol (HTTP) and Java WebStart. ROCS was designed to be capable of controlling all aspects of an observatory and be able to be reconfigured to handle changing equipment configurations or user requirements without the need for an expert computer programmer. ROCS consists of many small components, each designed to perform, a specific task, with the configuration of the system specified using a simple meta language. The use of small components facilitates testing and makes it possible to prove that the system is correct.

关键词： Internet security robotic control

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OSIRIS software: An overview

OSIRIS software: An overview

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advanced telescope and instrumentation control software ii

作者： López-Ruiz, José C. Aguiar, Marta Joven, Enrique Herrera, Alberto Gigante, José V. Cruz-López, Antonio González-Serrano, Ignacio IAC 38200 La Laguna Tenerife Spain Inst. de Fisica de Cantabria CSIC-Universidad de Cantabria 39005 Santander Spain

OSIRIS (Optical System for Imaging and low/intermediate-Resolution Integrated Spectroscopy) is an instrument designed to obtain images and low resolution spectra of astronomical objects in the optical domain (from 365 through 1000nm). It will be installed on Day One (middle of 2004) in the Nasmyth focus of the 10-meter Spanish GTC telescope. This paper shows an overview of the OSIRIS instrument software. Its architecture is distributed with real time features, having in mind to build a reusable, maintainable and inexpensive system. In this paper, we outline the main performances of the current design and some examples already implemented are given.

关键词： Computer software

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User relevant TA data architecture

User relevant TA data architecture

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conference on Airborne telescope Systems ii

作者： Levin, T Lattner, K Bittner, H Kayser Threde GmbH D-81379 Munich Germany

ISBN: (纸本)081944636X

For operation and monitoring, the SOFIA telescope assembly comprises a dedicated controls system. Basically this system appears to the user to consist of four major controller subsystems: Master control Processor (MCP), Tracker controller (TRC), telescope Assembly Servo control Unit (TASCU) and Secondary Mirror controller (SMC). They are accessible via a single command driven interface link through the MCP. With the example of the subsystems MCP and TRC, commonality aspects in communication interface architecture and software protocol selection are discussed. The special requirements associated with the installation in an aircraft are considered as well as maintenance aspects for 20 years of operation. The paper covers user relevant hard-/software design aspects of the TA flight as well as ground support systems. The usage of the TA data structure definitions, provided in XML, throughout the whole observatory for interface description and implementation are explained.

关键词： SOFIA TA MCP TRC software DESIGN INTERFACE DESIGN XML EGSE COMPOSE

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Status of VLTI control system: how to make an optical interferometer a data producing facility

Status of VLTI control system: how to make an optical interf...

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conference on advanced telescope and instrumentation control software ii

作者： Wallander, A Argomedo, J Ballester, P Bauvir, B Comin, M Donaldson, R Duhoux, P Gennai, A Gilli, B Housen, N Huxley, A Karban, R Kiekebush, M Longinotti, A Munoz, I Duc, TP European So Observ D-85748 Garching Germany

ISBN: (纸本)0819446270

After having established routine science operations for four 8 in single dish telescopes and their first set of instruments at the Paranal Observatory, the next big engineering challenge for ESO has been the VLT Interferometer. Following an intense integration period at Paranal, first fringes were obtained in the course of last year, first with two smaller test siderostats and later with two 8 in VLT telescopes. Even though optical interferometry today may be considered more experimental than single telescope astronomy, we have aimed at developing a system with the same requirements on reliability and operability as for a single VLT telescope. The VLTI control system is responsible for controlling and coordinating all devices making up VLTI, where a telescope is just one out of many subsystems. Thus the pure size of the complete system increases the complexity and likelihood of failure. Secondly, some of the new subsystems introduced, in particular the delay lines and the associated fringe-tracking loop, have more demanding requirements in terms of control loop bandwidth, computing power and communication. We have developed an innovative generic multiprocessor controller within the VLT framework to address these requirements. Finally, we have decided to use the VLT science operation model, whereby the observation is driven by observation blocks with minimum human real-time interaction, which implies that VLTI is seen as one machine and not as a set of telescopes and other subsystems by the astronomical instrument. In this paper we describe the as-built architecture of the VLTI control and data flow system, emphasising how new techniques have been incorporated, while at the same time the investments in technology and know-how obtained during the VLT years have been protected. The result has been a faster development cycle, a robustness approaching that of VLT single dish telescopes and a "look and feel" identical to all other ESO observing facilities. We present oper

关键词： VLTI control system interferometer software engineering

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