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

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Design and Automated control of Pasteurization Process in Dairy Industry Using S7-300 PLC and HMI 19th

Design and Automated Control of Pasteurization Process in Da...

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19th control instrumentation System conference, CISCON 2022

作者： Kumaresan, K. Deepa, R. Dhanasekar, R. Monisha, C. Carolin Dasaprakash, C. Priyavarshini, G.U. Department of Electronics and Instrumentation Engineering Bannari Amman Institute of Technology Sathyamangalam Tamil Nadu Sathyamangalam638401 India

ISBN: (纸本)9789819995530

This paper presents the design and automation control of milk pasteurization process in the dairy industry using a Siemens S7-300 PLC and online monitoring with a Siemens TP 700 comport HMI panel. Pasteurization is the process of heating milk and food to a constant temperature for a certain period of time and then quickly cooling them after they have been removed from the heating process. This process decreases the growth of microorganisms in milk and prevents milk contamination. Pasteurization is the most important stage in quality milk production. In this study, the S7-300 PLC is used for accurate monitoring and control of the analog parameters like temperature, flow, and pressure in the pasteurization process tank along with sensors and actuators. The Model Predicative control (MPC) algorithm is used for nonlinear process and human machine interface screens for pasteurization processes are developed using Step7 and WinCC software. The advanced most standard Profinet communication protocol is used to configure programming devices between the PLC controller and HMI. Step7 trend results show that the temperature control in the pasteurization process takes less settling time while eliminating overshoot and increasing the product quality and lifetime. The most widely used PLC-based automation control approach in the industry, owing to its undeniable simplicity, quick response, high production in less time, low implementation, and maintenance cost. © The Author(s), under exclusive license to Springer Nature Singapore Pte Ltd. 2024.

关键词： Microorganisms

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The Pointing Monitoring Camera hardware and software systems for the ASTRI Mini-Array Project 5

The Pointing Monitoring Camera hardware and software systems...

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

作者： Germani, S. Iovenitti, S. Bruno, P. Tosti, G. Nucciarelli, G. Fugazza, D. Univ Perugia Dipartimento Fis & Geol Via A Pascoli I-06123 Perugia Italy INAF Osservatorio Astron Brera Via Brera 28 I-20121 Milan Italy INAF Osservatorio Astrofis Catania Via Santa Sofia 78 I-95123 Catania Italy

ISBN: (纸本)9781510653580;9781510653573

The ASTRI Mini-Array is an international project led by the Italian National Institute for Astrophysics (INAF) that foresees the construction and operation of an array of nine Imaging Atmospheric Cherenkov telescopes at the Observatorio del Teide in Tenerife (Spain). The main purpose of the project is to study gamma-ray astrophysical sources in the very high-energy range, particularly at the multi-TeV energy scale. The camera and electronics used for the detection of the Cherenkov light are designed to trigger on the very fast flashes from atmospheric particle showers. Although the variance method is implemented in ASTRI Mini-Array cameras, it is difficult to obtain an adequate pointing model using only Cherenkov cameras. In order to build the pointing model and to monitor and control the pointing accuracy during observations a Pointing Monitoring Camera will be installed on each telescope. The PMC systems will acquire images of the sky with a machine vision camera in the direction pointed by the telescopes and perform an astrometry check on a dedicated computer hosted in the telescope electronics cabinet. The astrometry results will be fed back to the main telescope control System. The PMC system will be controlled and it will exchange data through the OPC-UA protocol. During the Assembly Integration and Verification phase and for maintenance activities, a specifically developed Graphical User Interface will be used. The PMC hardware and software systems are described.

关键词： ASTRI Cherenkov pointing machine vision astrometry

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Laboratory Acceptance and telescope Integration Readiness of the Gran Telescopio Canarias Adaptive Optics System 8

Laboratory Acceptance and Telescope Integration Readiness of...

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conference on Adaptive Optics Systems VIII Part of SPIE Astronomical telescopes and instrumentation conference

作者： Montiila, I. Marco De la Rosa, J. Araujo, Tubio Rosicha, J. Garcia-Talavera, M. Reyes Aznar, M. Luis Gonzalez, E. Lopez, R. Simoes, R. Luis Recio, J. Patron Antolin, M. Puga Bejar, V. Sanchez Inst Astrofis Canarias IAC Calle Via Lactea S-N San Cristobal la Laguna 38205 Spain

ISBN: (纸本)9781510653528;9781510653511

The Adaptive Optics system of the 10-m class Gran Telescopio Canarias (GTCAO) is completing the acceptance tests in the laboratory at the Instituto de Astrofisica de Canarias, to be ready for its integration in the telescope at Roque de Los Muchachos Observatory (ORM) in 2023. The AO system has been designed with robustness and operability as its key characteristics, and will be a facility of GTC. It features a single deformable mirror (DM) with 373 actuators, conjugated to the telescope pupil, and a Shack-Hartmann wavefront sensor (WFS) with 312 subapertures, using an OCAM2 camera. The expected performance of the GTCAO system working on average atmospheric conditions and bright NGS is 65% Strehl Ratio in K-band. In this paper we present the characterization of the system and the tests that have been performed for its acceptance at the laboratory. A series of calibrations are required and methodically run to achieve its ultimate performance: flatten the DM, acquire the Interaction Matrix and the reference slopes, correct the non-common path aberrations etc. The WFS requires additional calibrations, to compensate the pupil displacement in all the 2 arcminutes patrol field of view, and to correct the atmospheric dispersion in the visible. Close loop gains and sampling frequency are adapted to the changing conditions, and lookup tables are created for that purpose. The compliance with the system specifications has been verified. After verification of the final software functionalities for telescope operation, the system will be shipped to the ORM, to be installed and aligned on the Nasmyth platform of the GTC, and to be integrated with the telescope control system.

关键词： Adaptive Optics Laboratory Acceptance Characterization Real time control

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Revamping of VLT-FORS control electronics with PLC systems: the final design 9

Revamping of VLT-FORS control electronics with PLC systems: ...

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conference on Ground-Based and Airborne instrumentation for Astronomy IX

作者： Baldini, V. Sulich, A. Coretti, I. Calderone, G. Cirami, R. Di Marcantonio, P. Bertocco, S. Nonino, M. Derie, F. Manescau, A. Del Valle, D. Gutierrez, P. INAF Osserv Astron Trieste Via GB Tiepolo 11 I-34131 Trieste Italy ESO Karl Schwarzschild Str 2 D-85748 Garching Germany

ISBN: (纸本)9781510653504;9781510653498

FORS2 is a multi-mode (imaging, polarimetry, long slit and multi-object spectroscopy) optical instrument mounted on the Very Large telescope (VLT) UT1 Cassegrain focus. It operates in the wavelength range of 330-1100 nm and, with the dismissed FORS1, is one of the most demanded instruments of the VLT in the astronomical community. After many years of operations (FORS1 was one of the first instruments installed at the VLT), an upgrade of the control system is absolutely required. Carried out by ESO and the Astronomical Observatory of Trieste, the upgrade will be applied to the decommissioned FORS1 instrument, that, when fully integrated, will replace FORS2 on the telescope. The upgrade will comprise the replacement of all the motors, the development of a new calibration unit, the adoption of a new ESO detector controller, and the design of a new control electronics based on Beckhoff PLC. Care will be given to the management of the motorized stages, about 50, avoiding MOS (Multi-Object Spectroscopy) slits and focal plane collision problems. The upgraded FORS will also be the first instrument to test the brand new ESO ELT instrument control framework, even if within the VLT environment. This paper will resume the design of FORS control electronics presented at the instrument Final Design Review. The new electronics layout, based on PLCs, and the motor's control software management will be also described.

关键词： FORS VLT control electronics PLC upgrade ELT SW MOS

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Time distribution on the Athena WFI

Time distribution on the Athena WFI

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conference on Space telescopes and instrumentation - Ultraviolet to Gamma Ray Part of SPIE Astronomical telescopes and instrumentation conference

作者： Veredas, Francisco Javier Albrecht, Sebastian Coutinho, Diogo Lederhuber, Andreas Reiffers, Jonas Max Planck Inst Extraterr Phys MPE Giessenbachstr D-85748 Garching Germany

ISBN: (纸本)9781510653443;9781510653436

The Wide Field Imager (WFI) is one of two instruments of the X-ray advanced telescope for High-ENergy Astrophysics (Athena) mission selected by ESA. The WFI instrument uses a camera with a DEPFET sensor, Detector Electronics (DE) to control the camera, and additional electronics units to communicate with the spacecraft on-boardcomputer (OBC). The Spacecraft Event Time (SCET) is generated on the OBC and synchronized with ground. The SCET timing synchronization between the OBC and the sensor photon detection presents particular challenges. The science user requirement of the absolute knowledge error of the WFI time stamp relative to the OBC clock is 5 mu s with a confidence level of 99.73%. In this paper, we present the WFI timing distribution implementation. The three main contributors of the timing distribution are: (1) Time delays and jitter between OBC and DE, (2) Internal delays of the DE, and (3) Delay between a photon capture and the time stamping in the DE. The first contributor is the most critical and two solving methods are identified. The first method uses only the timecode of the SpaceWire (SpW) communication network, and the second method uses a combination of pulse-per-second (PPS) signal and SpW network. SpW network standard was published in 2003 and few missions such as ESA Solar Orbiter use it exclusively for time distribution. In our analysis, we found that using the second method with a PPS signal, delays contribution is in order of nanoseconds.

关键词： Athena WFI X-ray telescope astrophysics satellite time synchronization absolute knowledge error time stamping pulse-per-second SpaceWire

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Portable In-vacuum Computerized Beam-relay Subsystem for the Magdalena Ridge Observatory Interferometer 9

Portable In-vacuum Computerized Beam-relay Subsystem for the...

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conference on Optical and Infrared Interferometry and Imaging IX

作者： Schofield, Ian S. Altamirano, Juan Buscher, David F. Creech-Eakman, Michelle J. Haniff, Christopher A. Mason, Jeffrey C. Momeni, Hamed New Mexico Inst Min & Technol MRO Interferometer Socorro NM 87801 USA Univ Cambridge Cambridge England

ISBN: (纸本)9781510675131;9781510675148

The Magdalena Ridge Observatory Interferometer (MROI) Beam Relay System (BRS) comprises a network of air-evacuated pipes and relay stations, consisting of a pier and vacuum can containing a relay mirror, shear alignment sensors, and control electronics. Located at precise points along the arms of the interferometer array, the BRS piers contain remotely controllable mirrors which can be precisely adjusted to direct light from the adjacent unit telescope down the beamline and into the Beam Combining Facility (BCF), where interference fringes are made. Changing the array configuration is a planned function of interferometer operation, but is time consuming and complicated, as it will involve moving mirror assemblies between the vacuum cans (VC). The Vacuum Can Hub (VCH) is a network Modbus message processor and instrumentation hub that connects the Vacuum Can (VC) instrumentation to the MROI power and communication infrastructure via a single Power over Ethernet (PoE) access point. This greatly simplifies and speeds up array reconfiguration. In this paper we shall discuss the MROI Automated Alignment System (AAS), which is tasked with ensuring precise alignment of beamlines connecting the UTs with the BCF, and its role as supervisor of the VCH. We also discuss the BRS components interfaced by the VCH: first, the VC 1-wire temperature sensor network, whose data is used by the AAS for driving fine adjustments of the BRS relay mirrors via the AAS's feed-forward open-loop thermal mechanical model. Second, twin shear sensors used for coarse beam alignment, each consisting of custom designed 10 x 10 pixel photodiode arrays, whose electronics and software allow direct access by the AAS by using the VCH's message routing capabilities. The VCH's ability to translate and relay Modbus messages between the network and serial domain allow high flexibility in defining the quantity and types of BRS hardware that can be installed in VCs.

关键词： Interferometer baseline beam relay system beamline alignment remote control network Modbus Arduino

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Rubin Observatory Hexapods: Issues and Upgrades 5

Rubin Observatory Hexapods: Issues and Upgrades

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

作者： Neill, Douglas R. Johnson, Brian Cho, Myung Daruich, Felipe Drass, Holger Lutfi, Mostafa Sirano, Kevin Tighe, Roberto Tsai, Te-Wei Wiecha, Oliver Rubin Observ Project Off 950 N Cherry Ave Tucson AZ 85719 USA AURA Rubin Observ Colina El Pino S-N La Serena Chile

ISBN: (纸本)9781510653580;9781510653573

The Vera Rubin Observatory hosts a large (8.4 meter) wide-field (3.5 degree) survey telescope(4). The Secondary Mirror (M2) Assembly(6) and Camera(5) utilize large hexapods(3) to facilitate optical positioning relative to the Primary/Tertiary Mirror. These hexapods were designed, fabricated, assembled, tested and met all their requirements(1). Unfortunately, both hexapods were damaged prior to integration. The camera hexapod was damaged from overheating induced separation of the low temperature grease into constituents. The M2 hexapod was damaged from water intrusion during shipping. In both cases the critical linear encoders/tapes interior to the hexapod actuators were affected. These encoders are used by the control system to determine the length of the actuator during hexapod operations. If these encoders require servicing while deployed on the telescope, the hexapod needs to be unloaded by removing its optical payload (camera or M2), and the hexapod disassembled. The hexapod actuator then needs to be disassembled and repaired. This procedure produces an unacceptable risk to equipment, and an excessive disruption of observing. To rectify this, the actuators were redesigned to allow on-telescope servicing of these encoders. The encoder to tape orientation was inverted, and an access cover was added. This facilitates servicing the encoder/tape while on the telescope, reducing the servicing time from days to minutes. To improve reliability, alterations were also applied to the electrical system. The limit switch wiring was rearranged, and the cabling to the hexapod legs was upgraded. Also, multiple software upgrades were incorporated to improve function, performance, and compatibility with the other observatory systems.

关键词： Hexapod Rubin LSST Simonyi Survey telescope LSST

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The real time computing and instrument control software for CaNaPy 8

The real time computing and instrument control software for ...

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conference on Adaptive Optics Systems VIII Part of SPIE Astronomical telescopes and instrumentation conference

作者： Jenkins, David R. Centrone, Mauro Puglisi, Alfio Haguenauer, Pierre Calia, Domenico Bonaccini Townson, Matthew Osborn, James Reyes, Marcos ESO Garching Garching Bei Muchen Germany INAF OA Roma Rome Italy INAF OA Arcetri Florence Italy CfAI Durham Durham England IAC Tenerife Tenerife Spain

ISBN: (纸本)9781510653528;9781510653511

CaNaPy is an LGS-AO experimental facility of new generation, currently being assembled by the research institutes participating to the project (INAF, IAC and Durham) and the European Southern Observatory. CaNaPy operation is at visible wavelengths, with a 63 W 589 nm laser used in pulsed mode. The project is lead by the ESO Technology Development Program, also in the frame of the ESO-ESA R&D collaboration, becoming available for ESO-ESA joint operation at OGS only after its commissioning in 2023. ESO and the participating institutes will use it for R&D field tests on LGS-AO technologies, with granted access. The CaNaPy AO system will use a Pyramid-WFS on the LGS reference;the uplink and downlink of the 589nm laser will share a common optical path using the same telescope for launch and for observations (monostatic configuration). A Shack-Hartmann WFS guiding on a nearby NGS will provide tip-tilt and focus measurements along the line of sight of the laser launch. Here, we present the current design and status of the Real-Time control software of CaNaPy, with the use of DARC for the hard real-time core control loops and the modifications to implement Pyramid control algorithms using Python based software for the auxiliary loops, control interface and diagnostic displays. We also include in our design provisions for including predictive control algorithms and operating the AO loops at high frame rates. We will then focus on the design and development of the CaNaPy Instrument control software, with particular attention to the requirements, the architecture setting, the graphic interface, the interfaces between the ICS and the other modules that manage the operations of the instrument.

关键词： adaptive optics satellite communication real time control

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Astronomical-driven based TSC project for conceptual design and demonstration of a star tracker by using 0.7-meter optical telescope system 5

Astronomical-driven based TSC project for conceptual design ...

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

作者： Anuchit, Kanatip Palee, Kritsada Torteeka, Peerapong Manuthasna, Shariff Prasit, Pakawat Kuntanapreeda, Suwat King Mongkuts Univ Technol North Bangkok Bangkok Thailand Natl Astron Res Inst Thailand Publ Org Thai Space Consortium Program Ctr Observ Operat & Engn Bangkok Thailand

ISBN: (纸本)9781510653580;9781510653573

Thai Space Consortium (TSC) was originally a cooperation program by 13 leading Thailand research organizations that proposed to develop a microsatellite for a scientific mission;moreover, the aim of the TSC program includes sharing and enhancing an advanced engineering capacity in Thailand. Due to the National Astronomical Research Institute of Thailand (NARIT) being a part of the TSC contributor;therefore, the development of the star tracker is first promoted to be an astronomical-driven project through the eye of astronomical engineers. In practice, the knowledge of star trackers can apply to satellite attitude determination systems. It is the most precisely measured absolute three-axis orientation of a spacecraft when integrated with relative sensors. Therefore, in this work, the potential of using an 0.7-meter optical telescope-based for software experimentation as a function of stars pattern recognition and attitude determination algorithms according to the detected stars on astronomical images. The image is mapped to the guide star catalog to correct the magnification, shear, and rotation of the image sensor respective to the Cartesian coordinates as a function of astrometry engineering. The result of the method is a plate-constant that then corrects the positions of a target celestial body. An inertial measurement unit (IMU) was equipped with the telescope mounting to collect the local orientation of the telescope itself to demonstrate the results of attitude determination in both deterministic-TRIAD method and solving loss function based on Wahba's problem. The proposed system integration method can be performed with negligible attitude determination error compared to the IMU-baseline attitude sensor. This contribution will present some of the experimental results and plans for further measurement campaigns.

关键词： Star tracker Astrometry Star catalog Star pattern recognition Attitude determination

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The Transients Handler System for the Cherenkov telescope Array Observatory 9

The Transients Handler System for the Cherenkov Telescope Ar...

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conference on Observatory Operations - Strategies, Processes, and Systems IX Part of SPIE Astronomical telescopes and instrumentation conference

作者： Egberts, Kathrin Hoischen, Clemens Steppa, Constantin Fuessling, Matthias Neise, Dominik Wilhelmi, Emma de Ona Oya, Igor Univ Potsdam Inst Phys & Astron Campus GolmHaus 28Karl Liebknecht Str 24-25 D-14476 Potsdam Germany CTAO gGmbH Saupfercheckweg 1 D-69117 Heidelberg Germany DESY Platanenallee 6 D-15738 Zeuthen Germany

ISBN: (纸本)9781510653542;9781510653535

The Cherenkov telescope Array Observatory (CTAO) will be the largest and most advanced ground-based facility for gamma-ray astronomy. Several dozens of telescopes will be operated at both the Northern and Southern Hemisphere. With the advent of multi-messenger astronomy, many new large science infrastructures will start science operations and target-of-opportunity observations will play an important role in the operation of the CTAO. The Array control and Data Acquisition (ACADA) system deployed on each CTAO site will feature a dedicated sub-system to manage external and internal scientific alerts: the Transients Handler. It will receive, validate, and process science alerts in order to determine if target-of-opportunity observations can be triggered or need to be updated. Various tasks defined by proposal-based configurations are processed by the Transients Handler. These tasks include, among others, the evaluation of observability of targets and their correlation with known sources or objects. This contribution will discuss the concepts and design of the Transients Handler and its integration in the ACADA system.

关键词： multi-messenger astronomy Cherenkov telescope Array Observatory gamma-ray astronomy transients target-of-opportunity observations

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