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control of the TSU 2-m automatic telescope

Control of the TSU 2-m automatic telescope

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conference on advanced software, control and Communication Systems for Astronomy

作者： Eaton, JA Williamson, MH Tennessee State Univ Ctr Excellence Informat Syst Nashville TN USA

ISBN: (纸本)0819454281

Tennessee State University is operating a 2-m automatic telescope for high-dispersion spectroscopy. The altazimuth telescope is fiber-coupled to a conventional echelle spectrograph with two resolutions (R=30,000 and 70,000). We control this instrument with four computers running linux and communicating over ethernet through the UDP protocol. A computer physically located on the telescope handles the acquisition and tracking of stars. We avoid the need for real-time programming in this application by periodically latching the positions of the axes in a commercial motion controller and the time in a GPS receiver. A second (spectrograph) computer sets up the spectrograph and runs its CCD, a third (roof) computer controls the roll-off roof and front flap of the telescope enclosure, and the fourth (executive) computer makes decisions about which stars to observe and when to close the observatory for bad weather. The only human intervention in the telescope's operation involves changing the observing program, copying data back to TSU, and running quality-control checks on the data. It has been running reliably in this completely automatic, unattended mode for more than a year with all day-to-day adminsitration carried out over the Internet. To support automatic operation, we have written a number of useful tools to predict and analyze what the telescope does. These include a simulator that predicts roughly how the telescope will operate on a given night, a quality-control program to parse logfiles from the telescope and identify problems, and a rescheduling program that calculates new priorities to keep the frequency of observation for the various stars roughly as desired. We have also set up a database to keep track of the tens of thousands of spectra we expect to get each year.

关键词： telescope control automation quality control

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ESO-VLT/FLAMES: control software for a multi-object observing facility

ESO-VLT/FLAMES: Control software for a multi-object observin...

引用

conference on advanced software, control and Communication Systems for Astronomy

作者： Popovic, D Di Marcantonio, P Santin, P Farrell, T Pozna, E Schmutzer, R European So Observ D-85748 Garching Germany

ISBN: (纸本)0819454281

FLAMES is a complex observational facility for multi-object spectrography installed at ESO VLT UT2 telescope at Paranal. It consists of a Fibre Positioner that feeds GIRAFFE, a medium-high resolution spectrograph, and UVES, a high resolution stand-alone spectrograph operational in slit mode since 1999. The Positioner is the core component of FLAMES. It is a rather large and complex system comprising two spherical focal plates of approx. 90 cm in diameter, an exchanger mechanism, R-theta robot motions and a pneumatic gripper mechanism with a built-in miniature CCD camera. The main task of the Positioner is to place a fibre (button) at a given focal plate position with accuracy better than 40 microns. The fibre positioning process is performed on the plate attached to the robot while an observation is being performed on the plate attached to the telescope rotator. The whole instrument is driven by software designed in accordance with the VLT Common software standards, allowing the complete integration of the instrument in the VLT environment. The paper mainly focuses on two areas: the low-level control and the performance of the Fibre Positioner;and the high level coordinating software architecture that provides facility for parallel operations of multiple instruments.

关键词： VLT multiple instruments Fibre Positioner multi-object real-time control OzPoz gripper

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LBT double prime focus camera control software

LBT double prime focus camera control software

引用

conference on advanced software, control and Communication Systems for Astronomy

作者： Di Paola, A Baruffolo, A Gallozzi, S Pedichini, F Speziali, R INAF Rome Astron Observ Catone Italy

ISBN: (纸本)0819454281

The LBT double prime focus camera (LBC) is composed of twin CCD mosaic imagers. The instrument is designed to match the double channel structure of the LBT telescope and to exploit parallel observing mode by optimizing one camera at blue and the other at red side of the visible spectrum. Because of these facts, the LBC activity will likely consist of simultaneous multi-wavelength observation of specific targets, with both channels working at the same time to acquire and download images at different rates. The LBC control software is responsible for coordinating these activities by managing scientific sensors and all the ancillary devices such as rotators, filter wheels, optical correctors focusing, house-keeping information, tracking and Active Optics wavefront sensors. The result is obtained using four dedicated PCs to control the four CCD controllers and one dual processor PC to manage all the other aspects including instrument operator interface. The general architecture of the LBC control software is described as well as solutions and details about its implementation.

关键词： LBC LBT instrument control software user interface

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UML modeling of the LINC-NIRVANA software

UML modeling of the LINC-NIRVANA software

引用

conference on advanced software, control and Communication Systems for Astronomy

作者： Gässler, W Bertram, T Briegel, F Driebe, T Heininger, M Nussbaum, E Storz, C Wang, J Zealouk, L Herbst, TM Ragazzoni, R Eckhardt, A Weigelt, G Max Planck Inst Astron D-69117 Heidelberg Germany

ISBN: (纸本)0819454281

LINC-NIRVANA is a Fizeau interferometer for the Large Binocular telescope (LBT) doing imaging in the near infrared (J,H.,K - band). Multi-conjugated adaptive optics is used to increase sky coverage and to get diffraction limited images over a 2 arcminute field of view. The control system consists of five independent loops, which are mediated through a master control. Due to the configuration, LINC-NIRVANA has no delay line like other interferometers. To remove residual atmospheric piston, the system must control both the primary and secondary mirrors, in addition to a third, dedicated piston mirror. This leads to a complex and interlocked control scheme and software. We will present parts of the instrument software design, which was developed in an object-oriented manner using UML. Several diagram types were used to structure the overall system and to evaluate the needs and interfaces of each sub-system to each other.

关键词： instrument software UML fizeau interferometer interferometer adaptive optics MCAO

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Porting and refurbishment of the WSS TNG control software

Porting and refurbishment of the WSS TNG control software

引用

conference on advanced software, control and Communication Systems for Astronomy

作者： Caproni, A Zacchei, A Vuerli, C Pucillo, M Osserv Astron Trieste INAF I-34131 Trieste Italy

ISBN: (纸本)0819454281

The Workstation software System (WSS) is the high level control software of the Italian Galileo Galilei telescope settled in La Palma (Canary Islands), developed at the beginning of '90 for HP-UX workstations. WSS may be seen as a middle layer software system, that manages the communications between the real time systems (VME), different workstations and high level applications, providing a uniform distributed environment. The project to port the control software from the HP workstation to Linux environment started at the end of 2001. It is aimed to refurbish the control software introducinc, some of the new software technologies and languages that belong to the open source software under the Linux operating system. The project was realized by gradually substituting each HP workstation with a Linux PC with the ooal to avoid heavy changes in the original software running under HP-UX. Three main phases characterized the project: creation of a simulated control room with several Linux PCs running WSS (to check all the functionalities);insertion in the simulated control room of some HPs (to check the mixed environment);substitution of HP workstations in the real control room. From a software point of view, the project introduces some new technologies, like multi-threading, and the possibility to develop high level WSS applications with almost every programming language that implements the Berkley sockets. A library to develop java applications has been also created and tested.

关键词： WSS control software TNG CGG

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A standard control system for the Large Millimeter telescope and instruments

A standard control system for the Large Millimeter Telescope...

引用

conference on advanced software, control and Communication Systems for Astronomy

作者： Souccar, K Wallace, G Malin, D Univ Massachusetts Dept Astron Amherst MA 01003 USA

ISBN: (纸本)0819454281

The Large Millimeter telescope monitor and control system is automatically generated from a set of XML configuration files. This insures that all inter-system communications and user interfaces adhere to a common standard. The system was originally designed to control the electro-mechanical components of the telescope but it maps well to the control of instruments. Properties of the instruments are defined in XML and subsequent control and communication code and user interfaces are generated. This approach works well in theory, however, when it comes to installing the system on the actual instruments, several problems arise: the goals of instrument developers, software support for instrument developers, hardware compatibility issues, and choice of computer architecture and development environment. In this paper, we present a discussion of the above issues and suggest tried solutions.

关键词： Large Millimeter telescope telescope instruments reusable software automatically generated software monitor and control framework XML Java CORBA

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Altair interactions

Altair interactions

引用

conference on advanced software, control and Communication Systems for Astronomy

作者： Dunn, J Véran, JP Herriot, G Smith, M Natl Res Council Canada Herzberg Inst Astrophys Victoria BC V9E 2E7 Canada

ISBN: (纸本)0819454281

Altair, ALTitude-conjugated Adaptive optics for InfraRed at Gemini North, was commissioned last October and is one of Canada's major contributions to the Gemini Project, a seven-nation consortium that built identical 8m telescopes in Hawaii (Gemini North) and Chile (Gemini South). Altair coordinates and transfers data and status to both local and external subsystems at very high speeds. External Gemini subsystems include the telescope control System (TCS), Acquisition and Guiding (A&G), Observatory control System (OCS), Gemini Interlock System (GIS), Time Server, Data Handling System (DHS), and Status and Alarm Database. This paper focuses on a few select sequences such as closing the control loop and delivering a corrected image, collecting statistics, and display data to highlight the complexity of the interactions within Altair.

关键词： adaptive optics Gemini control systems real-time control altair EPICS RPC

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Pointing calibration of the SMA antennas

Pointing calibration of the SMA antennas

引用

conference on advanced software, control and Communication Systems for Astronomy

作者： Patel, NA Sridharan, TK Harvard Smithsonian Ctr Astrophys Cambridge MA 02138 USA

ISBN: (纸本)0819454281

The Submillimeter Array (SMA) is a new radio interferometer consisting of 8 antennas of 6 meters diameter each, recently deployed in operation at the summit of Mauna Kea in Hawaii. The antennas currently operate at 230, 345 and 690 GHz bands and have high enough surface accuracy to allow operations at 890 GHz. At the highest frequencies, the FWHM primary beam size of each antenna will be about 12" which imposes a stringent requirement for single-dish pointing accuracy of I". We summarize the current status of pointing of the SMA antennas and the methods we have implemented to derive the pointing model parameters. We discuss the stability of the pointing models over time scales of several weeks. The difference between the radio and optical pointing offsets is a function of elevation only, and can be calibrated by observing a common source or a pair of neighboring sources. We present results of such a calibration and its application to improve the radio pointing performance during submillimeter observations.

关键词： radio telescopes antenna measurements pointing calibration telescope control software

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James Webb Space telescope - Supporting multiple ground system transitions in one year

James Webb Space Telescope - Supporting multiple ground syst...

引用

conference on advanced software, control and Communication Systems for Astronomy

作者： Detter, R Fatig, C Steck, J NASA Goddard Space Flight Ctr Greenbelt MD 20771 USA

ISBN: (纸本)0819454281

Ideas, requirements, and concepts developed during the very early phases of the mission design often conflict with the reality of a situation once the prime contractors are awarded. This happened for the James Webb Space telescope (JWST) as well. ne high level requirement of a common real-time ground system for both the Integration and Test (I&T), as well as the Operation phase of the mission is meant to reduce the cost and time needed later in the mission development for recertification of databases, command and control systems, scripts, display pages, etc. In the case of JWST, the early Phase A flight software development needed a real-time ground system and database prior to the spacecraft prime contractor being selected. To compound the situation, the very low level requirements for the real-time ground system were not well defined. These two situations caused the initial real-time ground system to be switched out for a system that was previously used by the flight software development team. To meet the high-level requirement, a third ground system was selected based on the prime spacecraft contractor needs and JWST Project decisions. The JWST ground system team has responded to each of these changes successfully. The lessons learned from each transition have not only made each transition smoother, but have also resolved issues earlier in the mission development than what would normally occur.

关键词： operations tradeoffs ground systems requirements

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The JCMT observing queue and recipe sequencer

The JCMT observing queue and recipe sequencer

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conference on advanced software, control and Communication Systems for Astronomy

作者： Kackley, RD Rees, NP Walther, C Jenness, T Joint Astron Ctr Hilo HI 96720 USA

ISBN: (纸本)0819454281

The James Clerk Maxwell telescope (JCMT), the world's largest sub-mm telescope, will soon be switching operations from a VAX/VMS based control system to a new, Linux-based, Observatory control System(1) (OCS). A critical part of the OCS is the set of tasks that are associated with the observation queue and the observing recipe sequencer: 1) the JCMT observation queue task 2) the JCMT instrument task, 3) the JCMT Observation Sequencer (JOS), and 4) the OCS console task. The JCMT observation queue task serves as a staging area for observations that have been translated from the observer's science program into a form suitable for the various OCS subsystems. The queue task operates by sending the observation at the head of the queue to the JCMT instrument task and then waits for the astronomer to accept the data before removing the observation from the queue. The JCMT instrument task is responsible for running up the set of tasks required to observe with a particular instrument at the JCMT and passing the observation on to the JOS. The JOS is responsible for executing the observing recipe, pausing/continuing the recipe when commanded, and prematurely ending or aborting the observation when commanded. The OCS console task provides the user with a GUI window with which they can control and monitor the observation queue and the observation itself. This paper shows where the observation queue and recipe sequencer fit into the JCMT OCS, presents the design decisions that resulted in the tasks being structured as they are, describes the external interfaces of the four tasks, and details the interaction between the tasks.

关键词： instrument control observatory control user interface sequencer observing recipe XML DRAMA

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