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Auto-alignment and image tracking system for the SUNRISE telescope

Auto-alignment and image tracking system for the SUNRISE tel...

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conference on advanced software and control for Astronomy

作者： Schmidt, W. Berkefeld, T. Feger, B. Friedlein, R. Gerber, K. Heidecke, F. Kentischer, T. von der Luehe, O. Sigwarth, M. Soltau, D. Waelde, E. Kiepenheuer Inst Sonnenphys D-79104 Freiburg Germany

ISBN: (纸本)0819463396

The 1m balloon-borne solar telescope SUNRISE will be equipped with a wave-front sensing system for automatic in-flight focusing and alignment of the telescope and for high-precision image tracking. A six-element wavefront sensor measures low order aberrations of the telescope, including defocus and coma. The correction is achieved by moving the focusing mirror and the telescope secondary, respectively, in a closed-loop circuit. The same system measures image motion. The instrument requirements for the tracking are a dynamical range of about 30 Hz and a precision of about 0.005 arcs in the sky. The image motion signal feeds a closed-loop control system that drives both the tip-tilt mirror assembly and the mirrors that are needed for focusing and alignment. The tip-tilt unit is a dual-stage system, built at the Kiepenheuer-Insitut, consisting of a slow component with a large range of about 60 arcs and a fast component with a short range and high bandwidth. A breadboard-version of the Correlating Wavefront Sensor has been successfully tested at the German Vacuum Tower telescope on Tenerife in summer of 2005. A closed-loop bandwidth of 80 Hz was measured for the tracking system. The wave-front sensor detected image aberrations pre-set by the telescope's adaptive optics system with the required accuracy. SUNRISE will be flown in long duration stratospheric balloon flights, with a first scientific flight in 2009.

关键词： Sun robotic alignment wave-front sensing active optics

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The Java based control software of the LUCIFER instrument

The Java based control software of the LUCIFER instrument

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conference on advanced software and control for Astronomy

作者： Juette, Marcus Polsterer, Kai Knierim, Volker Luks, Thomas Ruhr Univ Bochum Inst Astron D-44780 Bochum Germany

ISBN: (纸本)0819463396

The LUCIFER instrument is a near infrared spectroraph/imager with MOS for the Large Binocular telescope. Here we present the final software design, the interrelation of the software packages and the used hardware architecture. The software package is completely running under Java using intensively its Remote Method Invocation (RMI) mechanisms in a distributed system environment. The use of Java helped us to cope with a small amount of available manpower for the SW development, providing many native built-in Java methods and classes, which speed up the development process a lot. The control software will be finally installed on a Solaris OS, hosted on a Sun Fire V880 server, which results from a specific hardware constraint. For testin g purposes a standard Linux environment is used. This shows another big Java advantage, the platform independency. The "First Light" of LUCIFER 1 is estimated for summer/fall 2007, following LUCIFER 2 one year later.

关键词： near-infrared LBT object-oriented Java instrument software distributed system

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Interconnecting astronomical networks: Evolving from single networks to meta-networks - art. no. 627409

Interconnecting astronomical networks: Evolving from single ...

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conference on advanced software and control for Astronomy

作者： White, R. R. Allan, A. Evans, S. Vestrand, W. T. Wren, J. Wozniak, P. Los Alamos Natl Lab ISR Div Los Alamos NM 87545 USA

ISBN: (纸本)0819463396

Over the past four years we have seen continued advancement in network technology and how those technologies are beginning to enable astronomical science. Even though some sociological aspects are hindering full cooperation between most observatories and telescopes outside of their academic or institutional connections, an unprecedented step during the summer of 2005 was taken towards creating a world-wide interconnection of astronomical assets. The telescope Alert Operations Network System (TALONS), a centralized server/client bi-directional network developed and operated by Los Alamos National Laboratory, integrated one of its network nodes with a node from the eScience telescopes for Astronomical Research (eSTAR), a peer-to-peer agent based network developed and operated by The University of Exeter. Each network can act independently, providing support for their direct clients, and by interconnection provide local clients with access to;outside telescope systems, software tools unavailable locally, and the ability to utilize assets far more efficiently, thereby enabling science on a world-wide scale. In this paper we will look at the evolution of these independent networks into the worlds first heterogeneous telescope network and where this may take astronomy in the future. We will also examine those key elements necessary to providing universal communication between diverse astronomical networks.

关键词： robotic telescope communication interconnection network servers clients

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New control system for the 1.5m and 0.9m telescopes at Sierra Nevada Observatory

New control system for the 1.5m and 0.9m telescopes at Sierr...

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conference on advanced software and control for Astronomy

作者： Costillo, Luis P. Ramos, J. Luis Ibanez, J. Miguel Aparicio, Beatriz Herranz, Miguel Garcia, Antonio J. Inst Astrofis Andalucia Granada 18008 Spain

ISBN: (纸本)0819463396

The Sierra Nevada Observatory (Granada, Spain) has a number of telescopes. Our study will focus on two Nasmyth telescopes with apertures of 1.5m and 0.9m and an equatorial mount. The system currently installed to control these telescopes is a 1995 centralized VME module. However, given the problems which have arisen due to the number of wires and other complications, we have decided to change this control module. We will control each telescope with a distributed control philosophy, using a serial linear communication bus between independent nodes, although all system capabilities are accessible from a central unit anywhere and at any time via internet. We have divided the tasks and have one node for alpha control, another for delta control, one for the dome, one for the focus and the central unit to interface with a pc. The nodes for alpha, delta and the dome will be used by means of FPGA's in order to efficiently sample the encoders and the control algorithms, and to generate the output for the motors and the servo. The focus will have a microcontroller, and the system is easy to expand in the event of the inclusion of more nodes. After having studied several fieldbus systems, we have opted for the CAN bus, because of its reliability and broadcasting possibilities. In this way, all the important information will be on the bus, and every node will be able to access the information at any time. This document explains the new design made in the IAA for the new consoles of control whose basic characteristics are, the distributed control, the hardware simplify, the cable remove, the safety and maintenance improve and facilitating the observation improving the interface with the user, and finally to prepare the system for the remote observation.

关键词： telescope control system IAA OSN hardware design software design CAN bus embedded distributed control servo-control

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control system architecture of AMICA: a robotic instrument in an extreme environment - art. no. 62741K

Control system architecture of AMICA: a robotic instrument i...

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conference on advanced software and control for Astronomy

作者： Di Rico, Gianluca Ragni, Maurizio Corcione, Leonardo Giro, Enrico Fantinel, Daniela INAF Osservatorio Astron Collurania Teramo Terama Italy

ISBN: (纸本)0819463396

AMICA is a camera conceived to automatically acquire infrared astronomical images in the extreme environment of Dome C (T similar to -70 degrees C, p similar to 640 mbar). For this reason, hardware and software are specially designed. They must guarantee the correct execution of observing procedures, while performing a continuous monitoring of the environmental conditions, the instrument status and the observing parameters, and a real-time adjustment of them when required. All temperature-sensitive components will be placed in a thermally controlled rack. The environmental control inside it is assigned to a Programmable Logic controller (PLC). It is responsible, in particular, for the overall system start-up. Instrument status, mainly concerning vacuum level and temperatures inside the cryostat, is directly monitored by the local cPC, which sends instructions to the PLC in case of failure, in order to start appropriate restoring procedures. All hardware components are conceived to be easily and fast replaceable. Main tasks of the AMICA control software (ACS) are: telescope interaction, observation management, environment control, events handling, data storing. Because of the high frame rate, typical of infrared imaging, the acquisition system has been interfaced with an independent application (STS), to perform read-out electronics control, fast data processing (co-adding from chopping raw frames), parameters checking (such as exposure time, chopping frequency, etc.), and data output. The software design has a multithreading architecture, based on the Object Oriented approach and developed for Windows OS platforms.

关键词： Antarctica robotic telescopes infrared control software

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SNOWS:: Sierra Nevada Observatory Weather System

SNOWS:: Sierra Nevada Observatory Weather System

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conference on advanced software and control for Astronomy

作者： Costillo, Luis P. Ibanez, J. Miguel Aparicio, Beatriz Garcia, Antonio J. Inst Astrofis Andalucia Granada 18008 Spain

ISBN: (纸本)0819463396

The Observatorio de Sierra Nevada (OSN) is located at an altitude of 2800m at the Loma de Dilar in the Sierra Nevada mountain range, in the province of Granada, Spain. It is operated and maintained by the Instituto de Astrofisica de Andalucia (IAA-CSIC) and contains two Nasmyth telescopes with apertures of 1.5 and 0.9m and an Altazimuth telescope with an aperture of 0.6m. Given that the quality of the images and, indeed, the performance of the instruments are influenced by weather conditions, it would appear that the existence of a weather station capable of producing accurate descriptions is an essential component of any observatory. This is particularly true, however, in our case where, given the altitude, weather conditions at certain times of the year are especially harsh(1). For this reason, our observatory has required the installation of a robust weather station with easily replaceable sensors which can provide accurate and reliable measures of wind, temperature and humidity(2). At the same time, in order to avoid a complex topology of unmanageably long wires due to the distribution of a large number of sensors around the buildings, domes telescope mirrors and instruments, it has been necessary to implement a distributed system with several independent nodes connected to a CAN bus. This system is now in operation and running automatically at the OSN and provides all the data from sensors to the observatory control systems and to internet users. This paper gives a detailed description of the SNOWS project, including the development of the weather station, the software and hardware architecture, and the use of distributed nodes with a linear serial bus. The paper also provides some results regarding the wind, temperature and humidity sensors employed at the OSN.

关键词： Sensors telescopes Observatories Humidity Space telescopes Data acquisition Domes control systems Databases LabVIEW

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MOPEX - A software package for astronomical image processing and visualization - art. no. 62740C

MOPEX - A software package for astronomical image processing...

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conference on advanced software and control for Astronomy

作者： Makovoz, David Roby, Trey Khan, Iffat Booth, Hartley CALTECH IPAC Spitzer Sci Ctr Pasadena CA 91125 USA

ISBN: (纸本)0819463396

We present MOPEX - a software package for astronomical image processing and display. The package is a combination of command-line driven image processing software written in C/C++ with a Java-based GUI. The main image processing capabilities include creating mosaic images, image registration, background matching, point source extraction, as well as a number of minor image processing tasks. The combination of the image processing and display capabilities allows for much more intuitive and efficient way of performing image processing. The GUI allows for the control over the image processing and display to be closely intertwined. Parameter setting, validation, and specific processing options are entered by the user through a set of intuitive dialog boxes. Visualization feeds back into further processing by providing a prompt feedback of the processing results. The GUI also allows for further analysis by accessing and displaying data from existing image and catalog servers using a virtual observatory approach. Even though originally designed for the Spitzer Space telescope mission, a lot of finictionalities are of general usefulness and can be used for working with existing astronomical data and for new missions. The software used in the package has undergone intensive testing and benefited greatly from effective software reuse. The visualization part has been used for observation planning for both the Spitzer and Herschel Space telescopes as part the tool Spot. The visualization capabilities of Spot have been enhanced and integrated with the image processing functionality of the command-line driven MOPEX. The image processing software is used in the Spitzer automated pipeline processing, which has been in operation for nearly 3 years. The image processing capabilities have also been tested in off-line processing by numerous astronomers at various institutions around the world. The package is multi-platform and includes automatic update capabilities. The software packag

关键词： image processing image visualization software reuse software integration

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telescope performance near local midnight for the Japanese advanced Meteorological Imager (JAMI)

Telescope performance near local midnight for the Japanese A...

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conference on Applications with Weather Satellites ii

作者： Pavlov, M Bell, JL Hurt, T Jacoby, M Shreckengost, B Ravela, R Schwarz, MA Raytheon Santa Barbara Remote Sensing Goleta CA 93117 USA

ISBN: (纸本)0819456195

Raytheon's Santa Barbara Remote Sensing (SBRS) division designed and built the MTSAT-1R Japanese advanced Meteorological Imager for the Japanese Ministry of Transport between March, 1999 and July, 2002. In order to meet the stressing requirements of a geosynchronous orbit, a combination of structural, thermal, and optical (STOP) analyses were used to design and optimize the beryllium three-mirror anastigmat (TMA) telescope. This modeling approach was used to characterize and minimize the thermal distortion around local midnight. On-orbit temperatures and structural deformations were predicted using thermal Desktop/SINDA and PATRAN/NASTRAN software, respectively. The resulting optical performance was evaluated using Raytheon developed HEXAGON software. The telescope design was successfully optimized to attain specified visible channel performance for most of the 24 hour orbit.

关键词： telescopes Mirrors Modulation transfer functions Sun Thermography Space telescopes Stray light Performance modeling Distortion Imaging systems

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Design and analysis of a beryllium three-mirror anastigmat telescope for the Japanese advanced meteorological imager (JAMI)

Design and analysis of a beryllium three-mirror anastigmat t...

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conference on Applications with Weather Satellites ii

作者： Bell, JL Pavlov, M Raytheon Santa Barbara Remote Sensing Goleta CA 93117 USA

ISBN: (纸本)0819456195

Raytheon's Santa Barbara Remote Sensing facility in Goleta, California designed and built an advanced meteorological imager for the Japanese Ministry of Transport between March, 2000 and July, 2002 for MTSAT-1R. One of the most stressing requirements is visible band image quality near local midnight. The 30 month program schedule forced the design team to make key decisions about the telescope design based on very preliminary analyses. Subsequent detailed analyses revealed that thermal distortions in the beryllium three-mirror anastigmat telescope would cause unacceptable performance degradation during much of the orbit. Through careful thermal, structural, and optical (STOP) analysis, the design team was able to optimize the designs of the telescope and thermal control system while meeting the challenging procurement schedule for the telescope.

关键词： telescopes Mirrors Optical instrument design Thermal modeling Wavefronts Beryllium Device simulation Imaging systems Sun Modulation transfer functions

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A correlator-based video sensor for docking with the Hubble Space telescope

A correlator-based video sensor for docking with the Hubble ...

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conference on Spaceborne Sensors ii

作者： Burcham, JD Balch, MK Granade, SR Adv Opt Syst Inc Huntsville AL 35806 USA

ISBN: (纸本)0819457833

The tragic loss of Space Shuttle Columbia threw the future of Hubble Space telescope (HST) in doubt. The Columbia Accident Investigation Board report led NASA to the realization that astronauts must have someplace to go on orbit if the Shuttle is damaged, a requirement that cannot be met for a manned HST mission. Yet missions to HST are required, since HST was designed to be serviced periodically. To address this problem, NASA is developing a robotic servicing mission to Hubble. On-orbit rendezvous and docking under tele-robotic or fully autonomous control involves a number of challenges that have not been fully resolved. One key challenge is how to bring two craft together in precise alignment to each other without an experienced astronaut on board. For this to be possible, sensors are needed to report relative distance, bearing, and orientation. At advanced Optical Systems (AOS), we have applied our ULTOR (TM) digital correlation system to the Hubble repair mission. The ULTOR (TM) system operates at approximately 10 Hertz and can accurately determine the relative distance, bearing, and orientation needed for semi- or fully-autonomous docking to HST. The system can operate using the HST berthing target or other features, including the HST itself. It is small and light enough to be placed on the servicing craft, thus avoiding orbit-to-ground communication latency issues. We will discuss the results of our testing with computer-generated imagery of the HST and with any hardware-in-the-loop simulations.

关键词： hubble space telescope advanced optical correlator optical correlation on-orbit sensors video sensors

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