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

共 1190 条记录，以下是11-20 订阅

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The Simons Observatory: Antenna control software integration and implementation 11

The Simons Observatory: Antenna control software integration...

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conference on : Millimeter, Submillimeter, and Far-Infrared Detectors and instrumentation for Astronomy XI

作者： Saunders, Lauren J. Hasselfield, Matthew Koopman, Brian J. Newburgh, Laura Yale Univ Dept Phys New Haven CT 06511 USA Flatiron Inst Ctr Computat Astrophys New York NY 10010 USA

ISBN: (纸本)9781510653627;9781510653610

The Simons Observatory (SO) is a ground-based cosmic microwave background survey experiment that consists of three 0.5 m small-aperture telescopes and one 6 m large-aperture telescope, sited at an elevation of 5200 m in the Atacama Desert in Chile. SO will study the polarization and temperature anisotropies of the Cosmic Microwave Background (CMB). The observatory will require well-understood telescope pointing and scanning. Good antenna control will allow us to execute the scan strategy devised to optimize sensitivity to our scientific goals, calibrate the system with celestial targets, and make maps. To achieve this, we integrate the data acquisition and control of the telescopes' Antenna control Units (ACUs) within the software framework of the SO Observatory control System (OCS). We present here the current status of the software integration for the ACUs, as well as measurements of the Small Aperture telescope platforms' responsiveness to software commanding in the factory, plans for in situ measurements, and prospects for implementation on the Large Aperture telescope.

关键词： Cosmic Microwave Background Antenna control Unit Observatory control System Simons Observatory control software monitoring data acquisition

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MAVIS: designing the interface between instrument control software and SRTC 8

MAVIS: designing the interface between instrument control so...

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conference on software and Cyberinfrastructure for Astronomy VIII

作者： Costa, E. Doucet, N. Savarese, S. Salasnich, B. Bernard, J. Gratadour, D. Rigaut, F. INAF Astron Observ Padova Vicolo Osservatorio 5 Padua Italy INAF Astron Observ Capodimonte Salita Moiariello 16 Naples Italy Australian Natl Univ Adv Instrumentat Technol Ctr Res Sch Astron & Astrophys Canberra ACT Australia

ISBN: (纸本)9781510675261;9781510675254

MAVIS is the new MCAO Assisted Visible Imager and Spectrograph for ESO's Very Large telescope. It is intended to be installed at the Nasmyth focus of UT4 "Yepun" telescope and it is composed of two main parts: a multi conjugate adaptive optics module and its post focal instrumentation, an imager and an IFU spectrograph, both operating in the visible spectrum. The project is now in the final design phase and it is expected to be commissioned in 2030. In this paper we focus on the interface between the instrument control system software (ICSS) and the soft Real-Time Computer (SRTC). ICSS is in charge of controlling all the motorized functions, managing the scientific exposures, monitoring the status of the system and coordinating the sequence of operations;on the other hand RTC receives data from from the wavefront sensors (8 LGS and 3 NGS) to compute the corrections to be applied by the two post focal deformable mirrors and 8 LGS jitter mirrors. ICSS will be based on the new ESO ELT software framework, which is still under development;SRTC will be based on the new ESO RTC Toolkit, also under development. We present the first design of the common interface between ICSS and SRTC, focusing mainly on the communication processes (commands and data) and which are the most critical points we had to face.

关键词： MAVIS VLT Instrument control software Real Time Computer Interface Adaptive Optics

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The CRS: a scalable full-stack control system for Microwave Kinetic Inductance Detectors 12

The CRS: a scalable full-stack control system for Microwave ...

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conference on Millimeter, Submillimeter, and Far-Infrared Detectors and instrumentation for Astronomy XII

作者： Montgomery, J. Avelino, W. Dobbs, M. Letang, J. Rouble, M. Savchyn, S. Smecher, G. TO Technol Inc Montreal PQ Canada McGill Univ Montreal PQ Canada

ISBN: (纸本)9781510675278;9781510675285

The *** control and Readout System (CRS) is a modular microwave control and readout system for mm-wave and radio astronomy, THz imaging, noise radar, and superconducting qubit control. The configuration discussed in this work implements firmware for readout of microwave Kinetic Inductance Detector (KID) arrays. The CRS can operate 4,096 KIDs over 2.5 GHz of complex bandwidth between 0-10 GHz, typically allocated across four independent RF chains at 1,024x multiplexing and 625MHz of complex bandwidth each. Every CRS can operate as a standalone unit or collectively within one or more backplane-enabled subracks that distribute power, clocking, and synchronization, scaling to an arbitrary number of channels. Each fully populated subrack supports arrays of more than 65,000 KIDs. The signal processing and control software supports recent innovations in multi-probe measurements and dynamic feedback modes, which are described in Rouble et al. (2024, these proceedings). The CRS has recently been selected as the new baseline readout system for the proposed South Pole telescope instrument, SPT-3G+.1 We present the hardware design, firmware capabilities, open-source control and data acquisition software, and the first laboratory characterization measurements.

关键词： multiplexing readout kinetic inductance detectors CRS digital signal processing quantum sensors

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Thermal design and control of Athena Wide Field Imager (WFI) Camera Head

Thermal design and control of Athena Wide Field Imager (WFI)...

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conference on Space telescopes and instrumentation - Ultraviolet to Gamma Ray

作者： Saraf, Anirudh Mukund Antonelli, Valeria Pietschner, Daniel Mayr, Astrid Mueller-Seidlitz, Johannes Haelker, Olaf Schnetler, Hermine Nandra, Kirpal Max Planck Inst Extraterr Phys Giessenbachstr 1 D-85748 Garching Germany

ISBN: (纸本)9781510675094;9781510675100

The Wide Field Imager (WFI) is one of two instruments on the ATHENA (advanced telescope for High-ENergy Astrophysics) X-ray space telescope. The WFI features a camera head comprising a large detector array with a readout time of less than 5 ms and a fast detector with a readout time of 80 mu s. The large detector array consists of four quadrants and each quadrant houses a sensor with a matrix of 512 x 512 pixels of Depleted P-channel Field Effect Transistors (DEPFET) with a pixel size of 130 mu m. The fast detector comprises a sensor with 64x64 pixels, using the same technology and pixel size as the large detector. Both sensors are controlled and read out by the frontend electronics (FEE), which consists of two types of application specific integrated circuits (ASIC) mounted close to the DEPFET sensors. The DEPFET sensors operate at temperatures between 193 K and 213 K, dissipating less than 1 W per LD. In contrast, the frontend electronics operate at a higher temperature, requiring approximately 10 W per large detector. The proximity of the ASICs and the DEPFET sensor for electrical performance necessitates a complex thermal design, decoupling the cooling chains for the DEPFET and the FEE.

关键词： WFI NewAthena Thermal Design Thermal control X-Ray instruments

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Programming Methodologies of NSF's DKIST Facility Management System 8

Programming Methodologies of NSF's DKIST Facility Management...

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conference on software and Cyberinfrastructure for Astronomy VIII

作者： Foster, Christopher White, Charles R. Natl Solar Observ 22 Ohia Ku St Makawao HI 96768 USA

ISBN: (纸本)9781510675261;9781510675254

The National Science Foundation's Daniel K. Inouye Solar telescope (DKIST) is the largest solar telescope in the world, utilizing a 4-m offset primary mirror that accumulates a 13 kW solar load. Safely offsetting and extracting that heat load is the Facility Management System (FMS), that controls all aspects of the Facility Thermal System (FTS). Using 3 PAC/PLC controllers, FMS provides coolant across 11 individual loops, each at different temperatures, to meet the requirements of the telescope, coude, enclosure, optics, and instruments, as well as controlling the Domestic Water System, the Energy Management System, Active and Passive ventilation, and the HVAC system including the Coude Instrument Lab cleanroom. control of all of these systems needs to be coordinated to provide the best thermal system performance based on the environmental conditions and operational requirements. Due to the unique and innovative nature of the observatory and the decision to self-perform a variety of construction work packages, all of the system programming and thermal instrumentation design was performed in-house. During DKIST's construction phase, each subsystem was commissioned at the most basic acceptable level, then immediately put into a production environment due to pre-existing cooling demands of the facility. This led to a tight time budget to program and deliver the FMS, making sequential prototyping, commissioning, and acceptance nearly impossible. These parameters drove the need for a flexible programming approach, more similar to a retrofit than a new system-wide design, when performing system adjustments and integrating new subsystems. By using state machine programming, it is possible to design the system using diagrams that makes it easier to review potential system operations with all interested parties, including those that are not programmers. This also reduces the time to receive feedback from users, debugging time, and identifying edge cases all while making the

关键词： PLC Solar telescope Facility Heat Load Allen-Bradley

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Post-wide-field-upgrade imaging performance evaluation of the Hobby-Eberly telescope 10

Post-wide-field-upgrade imaging performance evaluation of th...

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conference on Ground-Based and Airborne telescopes X

作者： Lee, Hanshin Kriel, Herman Janowiecki, Steven Fowler, Jim Pautzke, Justen McReynolds, Nathan D. Robison, Chris Univ Texas Austin McDonald Observ 2515 Speedway Mail Stop C1400 Austin TX 78712 USA Univ Texas Austin Hobby Eberly Telescope 32 Mt Fowlkes Rd Ft Davis TX 79734 USA

ISBN: (纸本)9781510675117;9781510675124

The Hobby-Eberly telescope (HET) is an innovative 10m-class telescope that operates with a fixed-altitude segmented spherical primary mirror (M1) while a tracker, located at the top of the telescope, moves the prime-focus spherical aberration corrector (SAC) and instrument package in order to track the sidereal and non-sidereal motions of celestial objects. In 2016, we completed the wide-field upgrade of the telescope, which includes the Wide-Field Corrector (WFC), the tracker, the prime focus instrument package, and all electromechanical hardware and telescope control software. Post the upgrade, we have been monitoring the imaging performance of the telescope through the in-situ metrology systems. These systems highlight weak spots of the telescope facility in imaging performance and provide quantitative guidance to specific facility repair and/or upgrades to further improve the HET's overall performance. This paper discusses our long-range (7yrs) datasets, specific analysis techniques used, and current outcomes of this investigativeeffort in the context of specific facility improvement and upgrade plans.

关键词： HET Imaging performance Metrology

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20 Years of Experience Maintaining the Encoders in the Very Large telescope at Paranal Observatory. 10

20 Years of Experience Maintaining the Encoders in the Very ...

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conference on Ground-Based and Airborne telescopes X

作者： Salgado, Fernando Huerta, Rodrigo Carlos Pineda, Juan Garces, Eduardo Alvarez, Nicolas Carlos Palacios, Juan Figueroa, Jose Rojas, Pascual Baez, Jose Cea, Victor Boccas, Maxime European Southern Observ Paranal Chile

ISBN: (纸本)9781510675117;9781510675124

More than 20 years have already passed since the first light of Antu, the Very Large telescope (VLT) Unit 1 at Paranal Observatory on 25th of May 1998. Encoders are key parts of the control of axes like Altitude, Azimuth, Adapters and Rotators in all the telescopes, where absolute encoders are used to get an accurate measurement of the position, at the level of micrometer. The intention of this document is to summarize and show some problems we had in these years, some modifications and suggestion to improve the design in order to avoid those problems. We also present some new applications of encoders to measure speed instead of position. A typical problem in the Adapters is analyzed, given that the encoder tape is located too close to the bearing it easily gets dirty, forcing our Maintenance Support and Engineering Department (MSE) to dismount the attached instrument and the whole Adapter Rotator getting access to clean its encoder system, with the consequent risk of losing operation time. Same issue is shown in Auxiliary telescopes, GRAAL Co-rotator and the European antenna in ALMA. All the encoder heads in the Adapters and Rotators were modified to avoid damage in the encoder tape, a change of a damaged tape was needed in 2005 and was done for the first time at ESO. A new design of the encoder head support is shown for both Altitude and Azimuth, which provides a fine and accurate way to adjust them. They have been installed in UT4 Azimuth and UT3 Altitude axes. A new design for Azimuth encoder tape is suggested to improve its robustness against variations of height in the hydraulic bearing system. Preventive, Condition-based, Corrective, and "Predictive" Maintenance applied to encoder systems are commented. The Obsolescence is analyzed. And a special case related with Calibration of encoders is also discussed. The integration of encoder signals to the axes plays a pivotal role in the deployment of a cutting-edge control system for the primary axes, Altitude and A

关键词： Encoders Position measurement Engineering experience telescope design Preventive and Corrective maintenance telescope axis control Very Large telescope (VLT) Extremely Large telescope (ELT)

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Advancements in Astronomical instrumentation: A New control software Framework for ELT and VLT instruments at ESO 8

Advancements in Astronomical Instrumentation: A New Control ...

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conference on software and Cyberinfrastructure for Astronomy VIII

作者： Kiekebusch, M. Andolfato, L. Del Valle, D. Feyrin, S. Hoffstadt, A. Knudstrup, J. Moins, C. Munoz, I Popovic, D. Reinero, C. Rosenquist, C. Sivera, P. Schmutzer, R. Szubiakowski, P. European Southern Observ Karl Schwarzschild Str 2 D-85748 Garching Germany European Southern Observ Cerro Paranal S-N Antofagasta Chile

ISBN: (纸本)9781510675261;9781510675254

The European Southern Observatory (ESO) has made a considerable progress in the implementation of a new software framework, the Instrument control System Framework (IFW) tailored to facilitate the development of upcoming astronomical instruments at the Extremely Large telescope (ELT). This framework offers a complete, scalable, and adaptable infrastructure to support the diverse needs of instrument control. The framework's architecture is strongly based on ESO's extensive experience in operating and maintaining VLT instruments while integrating the technological innovations specified by the ELT project. It presents a unified approach to instrument control, fostering the coordination of various heterogenous instruments subsystems and tasks, ranging from the control of instrument hardware functions and data visualization to the execution of science observations and instrument calibrations. The framework is primarily targeted to instrument developers from ESO partner institutes who are currently working on the first-generation ELT instruments. ESO extended the framework's application in 2019 to all new instruments within its optical telescopes. This strategy aims to reduce maintenance costs and promote ELT-VLT integrated operations, embracing future VLT instruments. The framework is being elaborated following the ELT Development Process, a sort of scrum like process supported by the tools Jenkins, Gitlab and Jira. This paper provides an overview of the design principles, key features, as well as details of the development process and main technologies employed in its construction.

关键词： ELT VLT framework instrument control software architecture design hardware control camera control

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The Simons Observatory: Deployment and current configuration of the Observatory control System for SAT-MF1 and data access software systems 12

The Simons Observatory: Deployment and current configuration...

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conference on Millimeter, Submillimeter, and Far-Infrared Detectors and instrumentation for Astronomy XII

作者： Bhimani, Sanah Lashner, Jack Aiola, Simone Crowley, Kevin T. Galitzki, Nicholas Harrington, Kathleen Hasselfield, Matthew Johnson, Alyssa Koopman, Brian J. Nakata, Hironobu Newburgh, Laura Nguyen, David Randall, Michael Silva-Feaver, Max Yale Univ Dept Phys Wright Lab New Haven CT 06511 USA Flatiron Inst Ctr Computat Astrophys New York NY 10010 USA Univ Texas Austin Dept Phys Austin TX 78712 USA Texas Ctr Cosmol & Astroparticle Phys Weinberg Inst Theoret Phys Austin TX 78712 USA Princeton Univ Joseph Henry Labs Phys Jadwin Hall Princeton NJ 08544 USA Univ Tokyo Dept Phys Tokyo 1130033 Japan Argonne Natl Lab High Energy Phys Div Lemont IL 60439 USA Univ Chicago Dept Astron & Astrophys Chicago IL 60637 USA Univ Calif San Diego Dept Astron & Astrophys La Jolla CA 92093 USA Univ Calif San Diego Dept Phys La Jolla CA 92093 USA Kyoto Univ Fac Sci Dept Phys Kyoto 6068502 Japan Univ Southern Calif 825 Bloomwalk Los Angeles CA 90089 USA

ISBN: (纸本)9781510675278;9781510675285

The Simons Observatory (SO) is a Cosmic Microwave Background experiment located in the Atacama Desert in Chile. SO consists of three small aperture telescopes (SATs) and one large aperture telescope (LAT) with a total of 60,000 detectors in six frequency bands.(1) As an observatory, SO encompasses hundreds of hardware components simultaneously running at different readout rates-all separate from its 60,000 detectors on-sky and their metadata. We provide an overview of commissioning SO's data acquisition software system for SAT-MF1, the first SAT deployed to the Atacama site. Additionally, we share insights from deploying data access software for all four telescopes, detailing how performance limitations affected data loading and quality investigations, which led to site-compatible software improvements.

关键词： Cosmic Microwave Background Observatory control System control software data acquisition monitoring data access software

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Design and feasibility study of a scalable liquid mirror 6

Design and feasibility study of a scalable liquid mirror

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conference on Advances in Optical and Mechanical Technologies for telescopes and instrumentation VI

作者： Kadala, Kristyn Andersen, Torben Choi, Heejoo Gregoriev, Ross Kim, Daewook Li, Yifan Tarkenton, Grey Lockheed Martin Space 3251 Hanover St Palo Alto CA 94304 USA Univ Arizona Wyant Coll Opt Sci 1630 E Univ Blvd Tucson AZ 85721 USA

ISBN: (纸本)9781510675230;9781510675247

Enabling tilt and imaging-while-slewing for ground-based liquid mirror telescopes would allow for very large-scale, low-cost mirror solutions. To explore how to accomplish this, our team has taken a systems approach leveraging optical, manufacturing, material, and modeling expertise to address the key technical challenges of creating a stable liquid surface. These technical challenges include maintaining optical quality surface figures while slewing and tilting, creating high optical reflectance concomitantly with controllable liquids, characterizing large-scale deformable optics, and manufacturing and scalability of proposed designs to greater than 50 m configurations. In this paper, we present both a solution framework as well as preliminary modeling results to demonstrate mirror feasibility for a ferrofluid, magnetically-actuated approach. In parallel with the overall telescope liquid mirror design effort, we discuss nanomaterial synthesis techniques for reflective ferrofluid as well as manufacturing development of a magnetically permeable metallic paraboloid shell with surface wicking structure and electromagnetic control coil arrays. The forces from the coils and capillarity from the wick establish the requisite control and stability to deliver required wavefront performance and maintain fluid stability. We share our initial model and small-scale coupon test results for baseline ferrofluid, wicking structure, and actuation inputs to demonstrate feasibility. We also outline next steps for our optical and ferrofluid modeling and material synthesis for a prototype 50 cm mirror we anticipate building in the near future.

关键词： Largescale Optics Liquid Mirror telescope

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