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The Simons Observatory: Overview of data acquisition, control, monitoring, and computer infrastructure 6

The Simons Observatory: Overview of data acquisition, contro...

conference on software and Cyberinfrastructure for Astronomy VI held as Part of SPIE Astronomical telescopes and instrumentation conference

作者： Koopman, Brian J. Lashner, Jack Saunders, Lauren J. Hasselfield, Matthew Bhandarkar, Tanay Bhimani, Sanah Choi, Steve K. Duell, Cody J. Galitzki, Nicholas Harrington, Kathleen Hincks, Adam D. Ho, Shuay-Pwu Patty Newburgh, Laura Reichardt, Christian L. Seibert, Joseph Spisak, Jacob Westbrook, Benjamin Xu, Zhilei Zhu, Ningfeng Yale Univ Dept Phys New Haven CT 06520 USA Univ Southern Calif Los Angeles CA 90007 USA Flatiron Inst Ctr Computat Astrophys New York NY 10010 USA Univ Penn Dept Phys & Astron Philadelphia PA 19104 USA Cornell Univ Dept Astron Ithaca NY 14853 USA Cornell Univ Dept Phys Ithaca NY 14853 USA Univ Calif San Diego Dept Phys La Jolla CA 92093 USA Univ Chicago Dept Astron & Astrophys 5640 South Ellis Ave Chicago IL 60637 USA Univ Toronto Dept Astron & Astrophys 50 St George St Toronto ON M5S 3H4 Canada Stanford Univ Dept Phys Stanford CA 94305 USA Univ Melbourne Sch Phys Parkville Vic 3010 Australia Univ Calif Berkeley Dept Phys Berkeley CA 94720 USA MIT MIT Kavli Inst Cambridge MA 02139 USA

ISBN: (纸本)9781510636927

The Simons Observatory (SO) is an upcoming polarized cosmic microwave background (CMB) survey experiment with three small-aperture telescopes and one large-aperture telescope that will observe from the Atacama Desert in Chile. In total, SO will field over 60,000 transition-edge sensor (TES) bolometers in six spectral bands centered between 27 and 280 GHz to achieve the sensitivity necessary to measure or constrain numerous cosmological parameters, including the tensor-to-scalar ratio, effective number of relativistic species, and sum of the neutrino masses. The SO scientific goals require coordination and control of the hardware distributed among the four telescopes on site. To meet this need, we have designed and built an open-sourced platform for distributed system management, called the Observatory control System (ocs). This control system interfaces with all subsystems including the telescope control units, the microwave multiplexing readout electronics, and the cryogenic thermometry. We have also developed a system for live monitoring of housekeeping data and alerting, both of which are critical for remote observation. We take advantage of existing open source projects, such as crossbar. io for RPC and PubSub, twisted for asynchronous events, Graf ana for online remote monitoring, and docker for containerization. We provide an overview of the SO software and computer infrastructure, including the integration of SO-developed code with open source resources and lessons learned while testing at SO labs developing hardware systems as we prepare for deployment.

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

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Optomechanical design of PAWS, the Potsdam Arrayed Waveguide Spectrograph 4

Optomechanical design of PAWS, the Potsdam Arrayed Waveguide...

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

作者： Hernandez, Eloy Stoll, Andreas Bauer, Svend-Marian Berdja, Amokrane Bernardi, Rafael Guzman, Dani Gunther, Alan Madhav, Kalaga Roth, Martin M. Sandin, Christer Villanueva, Constanza Leibniz Inst Astrophys Potsdam AIP Sternwarte 16 Potsdam Germany Sky Walkers SpA Andes Sci Instruments Santiago Chile Sandin Adv Visualizat Stockholm Sweden Pontificia Univ Catolica Chile Vicuna Mackenna 4860 Macul Chile

ISBN: (纸本)9781510636903

We present the optomechanical design of the Potsdam Arrayed Waveguide Spectrograph (PAWS), which is the first on-sky demonstrator of an integrated photonic spectrograph specifically designed and optimized for astronomy. The instrument is based on an arrayed waveguide grating (AWG) that was designed by and custom-fabricated for the innovation center innoFSPEC Potsdam. The commissioning of the instrument is planned at the Calar Alto 2.2m telescope in southern Spain. The core of the instrument is the AWG-chip as the primary dispersive element. The AWG device is coupled to the telescope module via a single-mode fibre (SMF). The spectral image on the output facet of the AWG is a superposition of multiple spectral orders due to the cyclic dispersive behavior of the waveguide array. The output of the AWG is fed into a free-space optical system housed inside a cryostat via an infinity-corrected microscope objective. The overlapping spectral orders are separated by a second dispersion stage using a ruled grating as a cross-dispersive element, and the resulting echellogram is projected onto a Teledyne 2k x 2k H2RG near-infrared array. The requirement of sub-micron accuracy of the fibre-chip alignment has led to an advanced photonic packaging method. In order to avoid on-site alignment procedures during the on-sky testing, the AWG mount, fibre-support, and microscope objective were integrated into a single monolithic module. Optical and thermal simulations and the design of the cryostat were realized by Andes Scientific. The read-out electronics and the compatible operating software for the detector was provided by the Max Planck Institute for Astronomy (MPIA). Data analysis is performed using the open-source data reduction software P3D, which provides functionality for the removal of the instrument signature, extraction of the spectra, correction for the blaze function, wavelength calibration, and processed data file export.

关键词： Arrayed waveguide gratings integrated photonics spectrograph cryostat design photonic packaging near-infrared detectors data reduction software

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Enabling Artificial Intelligence Studies in Off-Road Mobility Through Physics-Based Simulation of Multi-Agent Scenarios 17

Enabling Artificial Intelligence Studies in Off-Road Mobilit...

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ASME International Design Engineering Technical conferences / 42nd Annual Computers and Information in Engineering conference (IDETC-CIE) / 17th International conference on Multibody Systems, Nonlinear Dynamics, and control (MSNDC)

作者： Young, Aaron Taves, Jay Elmquist, Asher Serban, Radu Negrut, Dan Benatti, Simone Tasora, Alessandro Univ Wisconsin Dept Mech Engn Madison WI 53706 USA Univ Parma Dept Engn & Architecture Parma Italy

ISBN: (纸本)9780791885468

We describe a simulation environment that enables the development and testing of control policies for off-road mobility of autonomous agents. The environment is demonstrated in conjunction with the design and assessment of a reinforcement learning policy that uses sensor fusion and inter-agent communication to enable the movement of mixed convoys of human-driven and autonomous vehicles. Policies are learned on rigid terrain and are subsequently shown to transfer successfully to hard (silt-like) and soft (snow-like) deformable terrains. The enabling simulation environment is developed from the high fidelity, physics-based simulation engine Chrono. Five Chrono modules are employed herein: Chrono::Engine, Chrono::Vehicle, PyChrono, SynChrono and Chrono::Sensor. Vehicle's are modeled using Chrono::Engine and Chrono::Vehicle and deployed on deformable terrain within the training/testing environment. Utilizing the Python interface to the C++ Chrono API called PyChrono and OpenAI Gym's supporting infrastructure, training is conducted in a GymChrono learning environment. The GymChrono-generated policy is subsequently deployed for testing in SynChrono, a scalable, cluster-deployable multi-agent testing infrastructure built on MPI. SynChrono facilitates inter-agent communication and maintains time and space coherence between agents. A sensor modeling tool, Chrono::Sensor, supplies sensing data that is used to inform agents during the learning and inference processes. The software stack and the Chrono simulator are both open source. Relevant movies: [1].

关键词： Simulation Artificial intelligence Physics Roads Mechanical admittance Sensors Testing Engines Vehicles Computer software Design Modeling Autonomous vehicles Reinforcement learning American Petroleum Institute

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CUBES, THE CASSEGRAIN U-BAND EFFICIENT SPECTROGRAPH: TOWARDS FINAL DESIGN REVIEW

arXiv

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arXiv 2024年

作者： Genoni, Matteo Dekker, Hans Covino, Stefano Cirami, Roberto Scalera, Marcello A. Bissel, Lawrence Seifert, Walter Calcines, Ariadna Avila, Gerardo Landoni, Marco Stϋrmer, Julian Ritz, Christopher Lunney, David Miller, Chris Watson, Stephen Waring, Chris Castilho, Bruno V. De Arruda, Marcio V. Verducci, Orlando Coretti, Igor Oggioni, Luca Pariani, Giorgio Redaelli, Edoardo A.M. D’ Ambrogio, Matteo Calderone, Giorgio Porru, Matteo Stilz, Ingo Smiljanic, Rodolfo Cupani, Guido Franchini, Mariagrazia Scaudo, Andrea Geers, Vincent De Caprio, Vincenzo D’ Auria, Domenico Sibalic, Mina Opitom, Cyrielle Cescutti, Gabriele D’ Odorico, Valentina Sanchez-Janssen, Ruben Quirrenbach, Andreas Barbuy, Beatriz Cristiani, Stefano Di Marcantonio, Paolo INAF-Osservatorio Astronomico di Brera via E. Bianchi 46 Merate23807 Italy INAF-Osservatorio Astronomico di Trieste via G. B. Tiepolo 11 Trieste34131 Italy Edinburgh United Kingdom Landessternwarte - Zentrum fϋr Astronomie der Universitat Heidelberg Heidelberg Germany Durham University Centre for Advanced Instrumentation Department of Physics United Kingdom Optical Lab Baader Planetarium GmbH Zur Sternwarte Mammendorf4D-82291 Germany LNA/MCTI Rua Estados Unidos Itajubá154 - 37504-364 Brazil Universidade de São Paulo - IAG Rua do Matão 1226 São Paulo Brazil Nicolaus Copernicus Astronomical Center Polish Academy of Sciences Warsaw Poland INAF-Osservatorio Astronomico di Capodimonte via Moiariello 16 Napoli80131 Italy Institute for Astronomy University of Edinburgh Royal Observatory Edinburgh United Kingdom Dipartimento di Fisica-Sezione di Astronomia Università di Trieste Trieste Italy

In the era of Extremely Large telescopes, the current generation of 8-10m facilities are likely to remain competitive at ground-UV wavelengths for the foreseeable future. The Cassegrain U-Band Efficient Spectrograph (CUBES) has been designed to provide high instrumental efficiency (> 37%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral resolving power of R > 20, 000 (with a lower-resolution, sky-limited mode of R ∼ 7, 000). With the design focusing on maximizing the instrument throughput (ensuring a Signal to Noise Ratio – SNR– ∼ 20 per spectral resolution element at 313 nm for U ∼ 17.5 mag objects in 1h of observations), it will offer new possibilities in many fields of astrophysics: i) access to key lines of stellar spectra (e.g. lighter elements, in particular Beryllium), extragalactic studies (e.g. circumgalactic medium of distant galaxies, cosmic UV background) and follow-up of explosive transients. We present the CUBES instrument design, currently in Phase-C and approaching the final design review, summarizing the hardware architecture and interfaces between the different subsystems as well as the relevant technical requirements. We describe the optical, mechanical, electrical design of the different subsystems (from the telescope adapter and support structure, through the main opto-mechanical path, including calibration unit, detector devices and cryostat control, main control electronics), detailing peculiar instrument functions like the Active Flexure Compensation (AFC). Furthermore, we outline the AIT/V concept and the main instrument operations giving an overview of its software ecosystem. Installation at the VLT is planned for 2028/2029 and first science operations in late 2029. © 2024, CC BY.

关键词： Spectral resolution

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The research of intelligentization of control systems for large astronomical optical telescopes 8

The research of intelligentization of control systems for la...

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conference on Ground-Based and Airborne telescopes VIII Part of SPIE Astronomical telescopes + instrumentation conference

作者： Xu, Lingzhe Chao, Lin Li, XiaoYan Zhang, EnPeng Wang, Tao Cui, Xiangqun Yang, Shihai Cao, Zihuang Chinese Acad Sci Nanjing Inst Astron Opt & Technol Natl Astron Observ Nanjing 210042 Peoples R China Point Smart Technol Co Ltd Guangzhou Peoples R China Chinese Acad Sci Natl Astron Observ Beijing 100012 Peoples R China Chinese Acad Sci Natl Astron Observ Key Lab Opt Astron Beijing 100012 Peoples R China

ISBN: (纸本)9781510636781

Due to the high complexity of the system and the variety of influencing factors of large astronomical telescopes, the current control system could be improved largely. It' s difficult for traditional automatic control technologies to ensure reliable and highly efficient operation. The key problem is such a system which needs to consider not only the various internal factors but also the various external factors. In addition, some factors are difficult to be digitized. Thus, it' s hard to make mathematical models to represent such complex and dynamic systems. The first goal of this project is to construct a software experimental platfoun for the intelligentization. The second goal is to develop an intelligent reliability management system, and an optimization system for observation quality. These application systems will be running using the historical data of LAMOST operation. The evaluation of such systems will be based on the simulation of these data.

关键词： telescope control System Reliability management Optimization of observation quality Artificial Intelligence Applications Intelligent decision support

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A 3D scanner based on virtual instrumentation implemented by a 1D laser triangulation method 5th

A 3D scanner based on virtual instrumentation implemented by...

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5th International conference on advanced Engineering Theory and Applications, AETA 2018

作者： Brablik, Jindrich Martinek, Radek Haluska, Marek Bilík, Petr Department of Cybernetics and Biomedical Engineering Faculty of Electrical Engineering and Computer Science VSB–Technical University of Ostrava Ostrava Czech Republic

ISBN: (纸本)9783030149062

This paper deals with the design and implementation of a 3D scanner based on 1D laser triangulation method. Virtual instrumentation principles and tools were used in the design. NI myRIO embedded device was utilized to control the scanner hardware and graphical development environment LabVIEW was used to develop a control application for the scanner and to develop GUI for aÂ PC platform. Purpose of implemented scanner is to demonstrate the principle of 3D scanners and 1D laser triangulation method to students of virtual instrumentation class. First part of this paper provides concise theoretical information about 3D scanners, 1D laser triangulation method and virtual instrumentation principles. Second part focuses on mechanical, hardware and software design and implementation of realized scanner. © Springer Nature Switzerland AG 2020.

关键词： Triangulation

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control and systems software for the Cosmology Large Angular Scale Surveyor (CLASS) 6

Control and systems software for the Cosmology Large Angular...

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conference on software and Cyberinfrastructure for Astronomy VI held as Part of SPIE Astronomical telescopes and instrumentation conference

作者： A Petroff, Matthew Appel, John W. Bennett, Charles L. Brewer, Michael K. Chan, Manwei Chuss, David T. Cleary, Joseph Couto, Jullianna Denes Dahal, Sumit Eimer, Joseph R. Essinger-Hileman, Thomas Rojas, Pedro Fluxa Harrington, Kathleen Iuliano, Jeffrey Marriage, Tobias A. Miller, Nathan J. Valle, Deniz Augusto Nunes Watts, Duncan J. Xu, Zhilei Johns Hopkins Univ Dept Phys & Astron Baltimore MD 21218 USA Villanova Univ Dept Phys Villanova PA 19085 USA NASA Goddard Space Flight Ctr Greenbelt MD 20771 USA Pontificia Univ Catolica Chile Fac Fis Santiago 7820436 Chile Univ Chicago Dept Astron & Astrophys Chicago IL 60637 USA Univ Penn Dept Phys & Astron Philadelphia PA 19104 USA Univ Oslo Inst Theoret Astrophys N-0315 Oslo Norway MIT MIT Kavli Inst 77 Massachusetts Ave Cambridge MA 02139 USA

ISBN: (纸本)9781510636927

The Cosmology Large Angular Scale Surveyor (CLASS) is an array of polarization-sensitive millimeter wave telescopes that observes similar to 70% of the sky at frequency bands centered near 40 GHz, 90 GHz, 150 GHz, and 220 GHz from the Atacama desert of northern Chile. Here, we describe the architecture of the software used to control the telescopes, acquire data from the various instruments, schedule observations, monitor the status of the instruments and observations, create archival data packages, and transfer data packages to North America for analysis. The computer and network architecture of the CLASS observing site is also briefly discussed. This software and architecture has been in use since 2016, operating the telescopes day and night throughout the year, and has proven successful in fulfilling its design goals.

关键词： telescope control software cosmic microwave background telescopes

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Mathematical Modelling and control of Cruise control System on the Inclined Plane

Mathematical Modelling and control of Cruise Control System ...

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2020 International conference on Electrical and Electronics Engineering, ICE3 2020

作者： Prakash, Y.Saty Kumar, S. Amit Dr B R Ambedkar National Institute of Technology Department of Instrumentation and Control Engineering Jalandhar India

ISBN: (纸本)9781728158464

In this paper, the performance of PID controller is evaluated at the different conditions of road to achieve the desired speed of vehicle. In order to accommodate the vast and innovative developments in technology, a suitable design of controller is essential for speed control. This speed control system proves to be a prominent laboratory prototype of advanced control system. This CCS finds wide usage due to the ease in understanding and coverage of various predominant ancient and new design approaches. This paper presents the mathematical modeling for the development of the dynamic model of speed or CCS considering the road grade and the friction coefficient occurring between road and wheel. Modeling of the controller has been done by using MATLAB/Simulink software. Finally, PID controller is designed for different conditions. © 2020 IEEE.

关键词： controllers

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Adaptive optics real-time control with the compute and control for adaptive optics (Cacao) software framework 7

Adaptive optics real-time control with the compute and contr...

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conference on Adaptive Optics Systems VII

作者： Guyon, Olivier Sevin, Arnaud Ferreira, Florian Ltaief, Hatem Males, Jared R. Deo, Vincent Gratadour, Damien Cetre, Sylvain Martinache, Frantz Lozi, Julien Vievard, Sebastien Fruitwala, Neelay Bos, Steven P. Skaf, Nour Natl Inst Nat Sci NINS Subaru Telescope Natl Astron Observ Japan 650 North Aohoku Pl Hilo HI 96720 USA Univ Arizona Steward Observ Tucson AZ 85721 USA Univ Arizona Coll Opt Sci Tucson AZ 85721 USA NINS Astrobiol Ctr 2-21-1 Osawa Mitaka Tokyo Japan Sorbonne Univ LESIA Observ Paris Univ PSLCNRS 5 Pl Jules F-92195 Meudon France King Abdullah Univ Sci & Technol Extreme Comp Res Ctr Thuwal Saudi Arabia Australian Natl Univ Res Sch Astron & Astrophys Canberra ACT 2611 Australia W M Keck Observ 65-1120 Mamalahoa Hwy Kamuela HI USA Univ Cote dAzur Observ Cote dAzur Lab Lagrange CNRS Nice France Univ Calif Santa Barbara Dept Phys Santa Barbara CA 93106 USA Leiden Univ Leiden Observ Pob 9513 NL-2300 RA Leiden Netherlands UCL Dept Phys & Astron London England

ISBN: (纸本)9781510636842

The Compute and control for adaptive optics (Cacao) is an open source software package providing a flexible framework for deploying real-time adaptive optics control. Cacao leverages CPU and GPU computational resources to meet the demands of modern AO systems with thousands of degrees of freedom running at kHz speed or faster. Cacao adopts a modular approach, where individual processes operate over a standardized data stream stucture. advanced control loops integrating multiple sensors and DMs are built by assembling multiple such processes. High-level constructs are provided for sensor fusion, where multiple sensors can drive a single physical DM. The common data stream format is at the heart of Cacao, holding data content in shared memory and timing information as semaphores. Cacao is currently in operation on the general-purpose Subaru A0188 system, the SCExAO and MagAO-X extreme-AO instruments. Its data stream format has been adopted at Keck, within the COMPASS AO simulation tool, and in the COSMIC modular RTC platform. We describe Cacao's software architecture and toolset, and provide simple examples for users to build a real-time control loop. advanced features are discussed, including on-sky results and experience with predictive control and sensor fusion. Future development plans will include leveraging machine learning algorithms for real-time PSF calibration and more optimal AO control, for which early on-sky demonstration will be presented

关键词： Adaptive Optics Real-time systems Wavefront control High-performance computing

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Rubin Observatory Active Optics System Status 8

Rubin Observatory Active Optics System Status

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conference on Ground-Based and Airborne telescopes VIII Part of SPIE Astronomical telescopes + instrumentation conference

作者： Thomas, Sandrine J. Xin, Bo Claver, Charles F. Connolly, Andrew J. Kalmbach, J. Bryce Neill, Douglas R. Ribeiro, Tiago Suberlak, Chris Tsai, Tei-Wei Vera C Rubin Observ 950 N Cherry Av Tucson AZ 85719 USA Univ Washington Dept Astron Seattle WA 98195 USA

ISBN: (纸本)9781510636781

The Vera C. Rubin Observatory is now under construction on Cerro Pachon in Chile. This ground-based facility is designed to conduct the Legacy Survey of Space and Time (LSST), which is a decade-long time-domain optical survey of the night sky. The system aberrations introduced by temperature gradients, hysteresis and other non-predictable errors can prevent the telescope from delivering a consistently high-quality image over its 3.5 degrees field of view, necessary to the LSST scientific goals. Therefore, the active optics system (AOS) uses a combination of an open-loop and a closed-loop correction. The AOS open-loop is planned to correct for typical gravity variations while the AOS closed-loop will correct the real-time (within 30s) system aberrations. The components used for this task consist mainly of: two mirrors with active support systems (M1M3 and M2), two hexapods and curvature wavefront sensors integrated to the focal plane of the science detector. By the beginning of 2019, both M1 and M3 mirrors had been extensively tested using interferometry techniques, providing necessary measurements to refine our Finite Element models. This will help to achieve higher image quality when integrating all mirrors on the telescope. Progress has also been made on the active optics pipeline, which allows for conversion of the wavefront sensor images into corrective data for the mirrors and hexapods. In this paper, we will present the main results from the mirror testing as well as predicted performance of the AOS using these results. Finally, we will discuss the test plan for commissioning the AOS on the telescope.

关键词： Rubin Observatory Active Optics control software Curvature Sensing

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