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LINC-NIRVANA: Achieving 10 mas Imagery on the Large Binocular telescope

LINC-NIRVANA: Achieving 10 mas Imagery on the Large Binocula...

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conference on Ground-Based and Airborne instrumentation for Astronomy ii

作者： Herbst, T. M. Ragazzoni, R. Eckart, A. Weigelt, G. Max Planck Inst Astron Konigstuhl 17 D-69117 Heidelberg Germany Univ Cologne Inst Phys 1 D-50937 Cologne Germany Max Planck Inst Radioastron D-53121 Bonn Germany

ISBN: (纸本)9780819472243

LINC-NIRVANA is an innovative imaging interferometer fed by dedicated multi-conjugated adaptive optics systems. The instrument combines the light of the two, 8.4-meter primary mirrors of the Large Binocular telescope (LBT) on a single focal plane, providing panoramic imagery with 23-meter spatial resolution. The instrument employs a number of innovative technologies, including multi-conjugated adaptive optics, state-of-the-art materials, low vibration mechanical coolers, active and passive control, and sophisticated software for data analysis. LINC-NIRVANA is entering its final integration phase, with the large adaptive-optics and imaging subsystems coming together in the clean room in Heidelberg. Here, we report on progress, including insights gained on integration of large instruments.

关键词： near-infrared imaging interferometry Fizeau LBT

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Improved Guiding Accuracy Through Slit Viewer of Subaru telescope

Improved Guiding Accuracy Through Slit Viewer of Subaru Tele...

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2nd conference on advanced software and control for Astronomy

作者： Iseki, Akihiro Tomono, Daigo Tajitsu, Akito Itoh, Noboru Miki, Sachiko Natl Inst Nat Sci Natl Astron Observ Japan Subaru Telescope 650 N Aohoku Pl Hilo HI 96720 USA Mitsubishi Electr Corp Commun Syst Ctr Amagasaki Hyogo 6618661 Japan

ISBN: (纸本)9780819472298

The Subaru telescope provides a feature of auto guiding the telescope using the slit viewer (SV). The SV guide uses the target star as a guide star. There are advantages to guide the target star directly. However, the guide accuracy was not good. The guide star is located on the slit and some lights is vignetted by the slit. But the SV guide simply took the centroid of the light to measure the position of the star without taking the vignetting of the slit into account. In 2006, we improved the SV to detect center of gravity with the vignetting of the slit taken into account. It assumes a Gaussian distribution of light except for the slit. By this improvement, the guiding accuracy of the telescope improved from 0.37 arcsec to less than 0.2 arcsec. The effect of the improvement was also confirmed with actual observations.

关键词： Ground based telescope Subaru telescope auto guiding slit viewer guiding accuracy

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A polynomial-based trajectory generator for improved telescope control

A polynomial-based trajectory generator for improved telesco...

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2nd conference on advanced software and control for Astronomy

作者： Smith, David R. Souccar, Kainal MERLAB PC 357 S Candler St Decatur GA 30030 USA Univ Massachusetts Amherst Amherst MA 01003 USA

ISBN: (纸本)9780819472298

For any telescope, a fundamental performance requirement is the acquisition and tracking of the source. While this depends on many factors, the system accuracy is fundamentally limited by the servo tracking performance on the encoders. This tracking performance must be balanced with the need for large slewing motions to new sources. While the classical rate loop and position loop model permits basic operation, there has been increasing use through the years of gain scheduling or command pre-processors to improve telescope path planning and enable better performance. This is particularly important for telescopes that employ scanning or fast switching motions. As telescope control systems have moved to fully digital systems running at high update rates, more sophisticated approaches have become possible for telescope path planning. Taking advantage of the speed of available computation, we have developed a new real time trajectory generator that provides improved performance over previous implementations. Given a position command, the system generates a path to the desired end point. The resulting path is guaranteed to be continuous in position, velocity, and acceleration, as well as to respect specified limits in velocity, acceleration, and jerk. Significantly, the calculation provides not only the desired position over the interval, but also the velocity and acceleration, permitting their use in feedforward control to improve the tracking accuracy at all points on the path. The algorithm is presented, as well as some results with the system implemented on a real telescope.

关键词： telescope control command preprocessor trajectory generator path planning

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controlling the Hamburg Robotic telescope: a description of the software

Controlling the Hamburg Robotic Telescope: a description of ...

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2nd conference on advanced software and control for Astronomy

作者： Gonzalez-Perez, Jose N. Hempelmann, Alexander Mittag, Marco Hagen, Hans-Juergen Hamburger Sternwarte D-21029 Hamburg Germany

ISBN: (纸本)9780819472298

The Hamburg Robotic telescope (HRT) is a fully automatic 1.2m telescope designed for high resolution spectroscopy of active stars. It uses the Heidelberg Extended Range Optical Spectrograph (HEROS) which is fed by a 50 mu m fiber connected to the Nasmyth focus of the telescope through ail adapter. Here we present the software that controls the whole system of the HRT. This software works both in fully automatic and interactive mode. It organizes the interaction between the Central control System (CCS: the core of the system) and the subsystems: building, telescope, spectrograph, adapter, environmental sensors (weather station and sky monitor) and scheduler. The CCS performs its operation by sending commands (ASCii messages through TCP/IP sockets to the different. subsystems. The robotic operation is divided into discrete procedures, such as "Initialization", "Observation" or "Calibration". Each procedure consists of a set of commands which will be carried out, (sequentially or even in parallel) if a, set of conditions is met.: e.g. only when one command is successfully accomplished., the next will be sent. Furthermore, the Error Handler takes the necessary actions when a problem inhibits the normal progress of the observation (e.g. bad weather, non-detection of the target or technical problems). The scheduler selects the target from a. primary list in a manner which combines the scientific priority with observational feasibility and the history of observations. Finally, we present the Automatic Reduction Pipeline developed on the basis of REDUCE, ail IDL reduction package, to obtain the final spectrum from the raw data.

关键词： Robotic telescope robotic software high resolution spectroscopy

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The GTC main axes servos and control system

The GTC main axes servos and control system

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2nd conference on advanced software and control for Astronomy

作者： Suarez, M. Rosich, J. Ortega, J. Pazos, A. Inst Astrofis Canarias GTC Project Tenerife 38200 Spain

ISBN: (纸本)9780819472298

The GTC azimuth and elevation axes control systems employ large custom direct-drive motors operated by means of embedded fully-digital current loops. A high-performance position loop has been developed based on sinusoidal encoder feedback with interpolation error compensation. Real-time servo feedback and trajectory tracking is implemented by object-oriented software components at CPU-level which trigger encoder sampling, interpolate the remote CORBA demands and perform high-frequency setpoint streaming for the servo controller.

关键词： Servo control real-time software

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A Non-linear Disturbance-decoupled Elevation Axis controller for the Multiple Mirror telescope

A Non-linear Disturbance-decoupled Elevation Axis Controller...

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2nd conference on advanced software and control for Astronomy

作者： Clark, D. Trebisky, T. Powell, K. Univ Arizona Multiple Mirror Telescope Observ 933 N Cherry Ave Tucson AZ 85721 USA Univ Arizona Steward Observ Ctr Astron Adapt Opt Tucson AZ 85721 USA

ISBN: (纸本)9780819472298

The Multiple Mirror telescope (MMT), upgraded in 2000 to a monolithic 6.5m primary mirror from its original array of six 1.8m primary mirrors, was commissioned with axis controllers designed early in the upgrade process without regard to structural resonances or the possibility of the need for digital filtering of the control axis signal path. Post-commissioning performance issues led us to investigate replacement of the original control system with a more modem digital controller with full control over the system filters and gain paths. This work, from system identification through controller design iteration by simulation, and pre-deployment hardware-in-the-loop testing, was performed using latest-generation tools with Matlab (R) and Simulink (R). Using Simulink's Real Time Workshop toolbox to automatically generate C source code for the controller from the Simulink diagram and a custom target build script, we were able to deploy the new controller into our existing software infrastructure running Wind River's VxWorks (TM) real-time operating system. This paper describes the process of the controller design, including system identification data collection, with discussion of implementation of non-linear control modes and disturbance decoupling, which became necessary to obtain acceptable wind buffeting rejection.

关键词： telescope control system non-linear Matlab digital filter system identification generated code

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Design and implementation of a service-oriented driver architecture for LINC-NIRVANA

Design and implementation of a service-oriented driver archi...

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2nd conference on advanced software and control for Astronomy

作者： Kittmann, Frank Briegel, Florian Mohr, Lars Egner, Sebastian Gaessler, Wolfgang Berwein, Juergen Pavlov, Alexey Storz, Clemens Max Planck Inst Koenigstuhl 17 D-69117 Heidelberg Germany Natl Astron Observ Japan Subaru Telescope Hilo HI 96720 USA

ISBN: (纸本)9780819472298

LINC-NIRVANA (LN) is a German-Italian Fizeau (imaging) interferometer for the Large Binocular telescope (LBT). The Instrument control software (ICS) of this instrument is a hierarchical, distributed software package, which runs on several computers. In this paper we present the bottom layer of the hierarchy - the Basic Device Application (BASDA) layer. This layer simplifies the development of the ICS through a general driver architecture, which supports different types of hardware. This generic device architecture provides a high level interface to encapsulate the hardware dependent driver. The benefit of such a device architecture is to keep the basic device-driver layer flexible and independent from the hardware, and to keep the hardware transparent to the ICS. Additionally, the basic device-driver layer supports interfaces to IDL based applications for calibration and laboratory testing of astronomical instruments, and interfaces to engineering GUIs that allow to maintain the software components easily.

关键词： LBT LINC NIRVANA MPIA ICS Instrument control software Basic Device Application

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OEil 1.0 visual control system for the pointing and tracking of ground-based telescopes

OEil 1.0 visual control system for the pointing and tracking...

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2nd conference on advanced software and control for Astronomy

作者： Ferreira, Julian Rodriguez Espinel, Angela Gelvez Gomez, Arturo Plata Cabeza, Jorge Mejia Univ Ind Santander Grp Halley Astron Bucaramanga Colombia Inst Nacl Pesquisas Espaciais Div Astrofis Sao Jose Dos Campos SP Brazil

ISBN: (纸本)9780819472298

An inexpensive solution using an artificial vision system appears to the problem of pointing, tracking and guiding a telescope. A stellar sensor called "R2D2" has been developed. The elements of the system are a CMOS sensor with the respective optics and "Oeil 1.0", a software package that we have developed under the object oriented environment of Matlab 7.0. The software is built in a graphical user interface that allows an easy interaction between the user and the system. The stellar sensor is mounted in parallel to the telescope, captures images of the night sky and sends them to the software, which makes preprocessing and noise reduction routines, identifies the stars and their centroids, and calculates the equatorial coordinates of all the stars, the center of the image and any other point into the image. Finally the tracking of the stellar object placed in the center of the field of view is made thanks to the continuously feedback of images and the successful results obtained with the image processing techniques.

关键词： Astrometry image processing pointing tracking telescope stellar sensor

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STARS 2.0 2^nd generation open source archiving and query software

STARS 2.0 2<SUP>nd</SUP> generation open source archiving an...

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conference on Observatory Operations - Strategies, Processes, and Systems ii

作者： Winegar, Tom Subaru Telescope Mauna Kea HI USA

ISBN: (纸本)9780819472267

The Subaru telescope is in process of developing an open-source alternative to the 1st-generation software and databases (STARS 1) used for archiving and query. For STARS 2, we have chosen PHP and Python for scripting and MySQL as the database software. We have collected feedback from staff and observers, and used this feedback to significantly improve the design and functionality of our future archiving and query software. Archiving - We identified two weaknesses in 1st-generation STARS archiving software: a complex and inflexible table structure and uncoordinated system administration for our business model: taking pictures from the summit and archiving them in both Hawaii and Japan. We adopted a simplified and normalized table structure with passive keyword collection, and we are designing an archive-to-archive file transfer system that automatically reports real-time status and error conditions and permits error recovery. Query - We identified several weaknesses in 1st-generation STARS query software: inflexible query tools, poor sharing of calibration data, and no automatic file transfer mechanisms to observers. We are developing improved query tools and sharing of calibration data, and multi-protocol unassisted file transfer mechanisms for observers. In the process, we have redefined a 'query': from an invisible search result that can only transfer once in-house right now, with little status and error reporting and no error recovery - to a stored search result that can be monitored, transferred to different locations with multiple protocols, reporting status and error conditions and permitting recovery from errors.

关键词： Stars Calibration Databases telescopes Data archive systems Observatories Astronomy Data centers Prototyping control systems

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The WIYN One Degree Imager: An Update

The WIYN One Degree Imager: An Update

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conference on Ground-Based and Airborne instrumentation for Astronomy ii

作者： Harbeck, Daniel R. Jacoby, George H. Muller, Gary Sawyer, Dave Harmer, Charles Yeatts, Andrey Cavin, John Corson, Charles Univ Wisconsin 475 N Charter St Madison WI 53706 USA WIYN Observat Tucson AZ 85719 USA Natl Opt Astron Observ Tucson AZ 85719 USA

ISBN: (纸本)9780819472243

The WIYN Consortium is building the One Degree Imager (ODI) for its 3.5m telescope, located at Kitt Peak, Arizona (USA). ODI will utilize both the excellent image quality and the one degree field of view of the WIYN telescope. Image quality will be actively improved by localised tip/tilt image motion stabilisation using a novel concept of Orthogonal Transfer Array (OTA) CCDs, which are a new detector type jointly developed with the PanSTARRS project. Its anticipated median image quality of <= 0.55" in the R band will make ODI a unique and competitive instrument in the landscape of the next generation of large field imagers. A conceptual design of ODI was presented earlier at SPIE.(1) In the meantime, this concept matured, the ODI project has been fully funded, and it has entered the construction phase. A prototype camera (QUOTA) with a field of view of 16' x 16' has already seen first star light in fall 2006. In this paper we report on the evolution of ODI's definition, the design of its components, the status of the OTA detector development, and the path towards first light in early 2010. In accompanying papers we detail the design of the ODI's optical corrector, the mechanical structures, and the software & instrument system control design.

关键词： Ground based telescope instrumentation wide-field imaging One Degree Imager Orthogonal Transfer Array CCD WIYN telescope

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