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conference on Ground-Based and Airborne instrumentation for Astronomy VI

作者： Coker, Carl T. Pappalardo, Daniel Pogge, Richard Martini, Paul Derwent, Mark O'Brien, Thomas P. Honscheid, Klaus Ohio State Univ Dept Astron 140 W 18th Ave Columbus OH 43210 USA Ohio State Univ Dept Phys 191 W Woodruff Ave Columbus OH USA

ISBN: (数字)9781510601963

ISBN: (纸本)9781510601963

The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 40 million galaxies over 14,000 sq deg will be measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope will deliver light to 5,000 fiber optic positioners. The fibers in turn feed ten broad-band spectrographs. We present the design details of the instrument mechanism control systems for the spectrographs. Each spectrograph has a stand-alone mechanism control box that operates the unit's four remotely-operated mechanisms (two shutters and two Hartmannn doors), and provides a suite of temperature and humidity sensors. Each control box is highly modular, and is operated by a dedicated on-board Linux computer to provide all of the control and monitoring functions. We describe our solution for integrating a number of network-connected devices within each unit spectrograph, and describe the basic software architecture.

关键词： DESI spectrograph instrument control

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Bottom-up laboratory testing of the DKIST Visible Broadband Imager (VBI) 7

Bottom-up laboratory testing of the DKIST Visible Broadband ...

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conference on Modeling, Systems Engineering, and Project Management for Astronomy VII

作者： Ferayorni, Andrew Beard, Andrew Cole, Wes Gregory, Scott Woeger, Friedrich Natl Solar Observ 3665 Discovery Dr Boulder CO 80303 USA

ISBN: (纸本)9781510602014;9781510602021

The Daniel K. Inouye Solar telescope (DKIST) is a 4-meter solar observatory under construction at Haleakala, Hawaii [1]. The Visible Broadband Imager (VBI) is a first light instrument that will record images at the highest possible spatial and temporal resolution of the DKIST at a number of scientifically important wavelengths [2]. The VBI is a pathfinder for DKIST instrumentation and a test bed for developing processes and procedures in the areas of unit, systems integration, and user acceptance testing. These test procedures have been developed and repeatedly executed during VBI construction in the lab as part of a "test early and test often" philosophy aimed at identifying and resolving issues early thus saving cost during integration test and commissioning on summit. The VBI team recently completed a bottom up end-to-end system test of the instrument in the lab that allowed the instrument's functionality, performance, and usability to be validated against documented system requirements. The bottom up testing approach includes four levels of testing, each introducing another layer in the control hierarchy that is tested before moving to the next level. First the instrument mechanisms are tested for positioning accuracy and repeatability using a laboratory position-sensing detector (PSD). Second the real-time motion controls are used to drive the mechanisms to verify speed and timing synchronization requirements are being met. Next the high-level software is introduced and the instrument is driven through a series of end-to-end tests that exercise the mechanisms, cameras, and simulated data processing. Finally, user acceptance testing is performed on operational and engineering use cases through the use of the instrument engineering graphical user interface (GUI). In this paper we present the VBI bottom up test plan, procedures, example test cases and tools used, as well as results from test execution in the laboratory. We will also discuss the benefits realized t

关键词： Daniel K. Inouye Solar telescope instrumentation Testing Integration

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27 Level/IGBT asymmetrical multilevel inverter using PWM for locomotives 2

27 Level/IGBT asymmetrical multilevel inverter using PWM for...

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2nd International conference on Science Technology Engineering and Management, ICONSTEM 2016

作者： Suganthi Vinodhini, J. Samuel Rajesh Babu, R. Department of Electronics and Instrumentation Research Scholar SATHYABAMA UNIVERSITY Chennai India Department of Electronics and Instrumentation SATHYABAMA UNIVERSITY Chennai India

ISBN: (纸本)9781509017065

This paper presents a new twenty seven level cascaded H-bridge multi level inverter for locomotives. This proposed multi level inverter can overcome the need for a large number of electronic switches when the number of level increased. This proposed topology increases the efficiency of the inverter by reducing the switching losses using pulse width modulation technique. Recently in Japan they developed an advanced inverter drive system for bullet trains. By comparing all multilevel inverter topologies this proposed topology can achieve economic voltage control in locomotives which can reduce the total harmonic distortion in both electronic devices and traction motor in general. The proposed multilevel inverter and total harmonic distortion results with MATLAB software was described in this paper. © 2016 IEEE.

关键词： Pulse width modulation

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Thermal analysis of the WFI on the ATHENA observatory

Thermal analysis of the WFI on the ATHENA observatory

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conference on Space telescopes and instrumentation - Ultraviolet to Gamma Ray

作者： Fuermetz, Maria Pietschner, Daniel Meidinger, Norbert Max Planck Inst Extraterr Phys Giessenbachstr D-85748 Garching Germany

ISBN: (纸本)9781510601895;9781510601901

The WFI (Wide-Field Imager) instrument is one of two instruments of the ATHENA (advanced telescope for High-ENergy Astrophysics) mission. ATHENA is the second L-class mission in ESA's Cosmic Vision plan with launch in 2028 and will address the science theme "The Hot and Energetic Universe" by measuring hot gas in clusters and groups of galaxies as well as matter flow in black holes. A moveable mirror assembly focusses the X-ray light to the focal plane of the WFI. The instrument consists of two separate detectors, one with a large DEPFET array of 512x512 pixels and one small and fast detector with 64x64 DEPFET pixels and a readout time of only 80 mu s. The mirror system will achieve an angular resolution of 5" HEW. The rather large field of view of 40' x40' in combination with rather high power consumption is challenging not only for the thermal control system. DEPFET sensors as well as front-end electronics and electronics boxes have to be cooled, where a completely passive cooling system with radiators and heat pipes is highly favored. In order to reduce the necessary radiator area, three separate cooling chains with three different temperature levels have been foreseen. So only the DEPFET sensors are cooled down to the lowest temperature of about 190K, while the front-end electronics is supposed to be operated between 250K and 290K. The electronics boxes can be operated at room temperature, nevertheless the excess heat has to be removed. After first estimations of heat loads and radiator areas, a more detailed model of the camera head has been used to identify gradients between the cooling interfaces and the components to be cooled. This information is used within phase A1 of the project to further optimize the design of the instrument, e.g. material selection.

关键词： ATHENA Wide-Field Imager WFI thermal control heat pipe DEPFET cooling

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Upgraded Cameras for the HESS Imaging Atmospheric Cherenkov telescopes 6

Upgraded Cameras for the HESS Imaging Atmospheric Cherenkov ...

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conference on Ground-Based and Airborne instrumentation for Astronomy VI

作者： Giavitto, Gianluca Ashton, Terry Balzer, Arnim Berge, David Brun, Francois Chaminade, Thomas Delagnes, Eric Fontaine, Gerard Fuessling, Matthias Giebels, Berrie Glicenstein, Jean-Francois Graeber, Tobias Hinton, Jim Jahnke, Albert Klepser, Stefan Kossatz, Marko Kretzschmann, Axel Lefranc, Valentin Leich, Holger Luedecke, Hartmut Lypova, Iryna Manigot, Pascal Marandon, Vincent Moulin, Emmanuel de Naurois, Mathieu Nayman, Patrick Penno, Marek Ross, Duncan Salek, David Schade, Markus Schwab, Thomas Simoni, Rachel Stegmann, Christian Steppa, Constantin Thornhill, Julian Toussnel, Francois DESY D-15738 Zeuthen Germany Univ Leicester Dept Phys & Astron Univ Rd Leicester LE1 7RH Leics England Univ Amsterdam GRAPPA Astron Inst Anton Pannekoek Sci Pk 904 NL-1098 XH Amsterdam Netherlands CEA Saclay DSM Irfu F-91191 Gif Sur Yvette France Univ Denis Diderot Paris 7 Univ Pierre & Marie Curie Paris 6 LPNHE CNRS IN2P3 4 Pl Jussieu F-75252 Paris 5 France Ecole Polytech CNRS IN2P3 Lab Leprince Ringuet F-91128 Palaiseau France Max Planck Inst Kernphys POB 103980 D-69029 Heidelberg Germany

ISBN: (数字)9781510601963

ISBN: (纸本)9781510601963

The High Energy Stereoscopic System (H.E.S.S.) is an array of five imaging atmospheric Cherenkov telescopes, sensitive to cosmic gamma rays of energies between similar to 30 GeV and several tens of TeV. Four of them started operations in 2003 and their photomultiplier tube (PMT) cameras are currently undergoing a major upgrade, with the goals of improving the overall performance of the array and reducing the failure rate of the ageing systems. With the exception of the 960 PMTs, all components inside the camera have been replaced: these include the readout and trigger electronics, the power, ventilation and pneumatic systems and the control and data acquisition software. New designs and technical solutions have been introduced: the readout makes use of the NECTAr analog memory chip, which samples and stores the PMT signals and was developed for the Cherenkov telescope Array (CTA). The control of all hardware subsystems is carried out by an FPGA coupled to an embedded ARM computer, a modular design which has proven to be very fast and reliable. The new camera software is based on modern C++ libraries such as Apache Thrift, OMQ and Protocol buffers, offering very good performance, robustness, flexibility and ease of development. The first camera was upgraded in 2015, the other three cameras are foreseen to follow in fall 2016. We describe the design, the performance, the results of the tests and the lessons learned from the first upgraded H.E.S.S. camera.

关键词： HESS upgrade PMT signal readout Cherenkov telescope VHE gamma-ray astronomy NECTAr

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Comparison on bidirectional inverter using open loop and closed loop system 2

Comparison on bidirectional inverter using open loop and clo...

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2nd International conference on Science Technology Engineering and Management, ICONSTEM 2016

作者： Antonyalexander, J. Raj, Anand Suganthi Vinodhini, J. Dept of Electronics and Instrumentation SATHYABAMA UNIVERSITY Chennai India

ISBN: (纸本)9781509017065

关键词： Insulated gate bipolar transistors (IGBT)

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The Atmospheric Remote-sensing Infrared Exoplanets Large-survey (ARIEL) payload electronic subsystems

The Atmospheric Remote-sensing Infrared Exoplanets Large-sur...

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conference on Space telescopes and instrumentation - Optical, Infrared, and Millimeter Wave

作者： Focardi, M. Pace, E. Colome, J. Ribas, I. Rataj, M. Ottensamer, R. Farina, M. Di Giorgio, A. M. Wawer, P. Pancrazzi, M. Noce, V. Pezzuto, S. Morgante, G. Artigues, B. Sierra-Roig, C. Gesa, L. Eccleston, P. Crook, M. Micela, G. INAF OAA Arcetri Astrophys Observ Largo E Fermi 5 I-50125 Florence Italy Univ Florence Dept Phys & Astron Largo E Fermi 2 I-50125 Florence Italy IEEC CSIC Space Sci Inst Carrer Can Magrans Cerdanyola Del Valles 08193 Spain Polish Acad Sci CBK Space Res Ctr Bartycka 18a PL-00716 Warsaw Poland Univ Vienna Inst Astron Turkenschanzstr 17 A-1180 Vienna Austria INAF IAPS Inst Space Astrophys & Planetol Via Fosso Cavaliere 100 I-00133 Rome Italy INAF IASF Space Astrophys Inst Via P Gobetti 101 I-40129 Bologna Italy STFC RAL Space Rutherford Appleton Lab Harwell Oxford OX11 0QX England INAF OAPa Astron Observ Palermo Piazza Parlamento 1 I-90134 Palermo Italy

ISBN: (数字)9781510601888

ISBN: (纸本)9781510601871;9781510601888

The ARIEL mission has been proposed to ESA by an European Consortium as the first space mission to extensively perform remote sensing on the atmospheres of a well defined set of warm and hot transiting gas giant exoplanets, whose temperature range between similar to 600 K and 3000 K. ARIEL will observe a large number (similar to 500) of warm and hot transiting gas giants, Neptunes and super-Earths around a range of host star types using transit spectroscopy in the similar to 2-8 mu m spectral range and broad-band photometry in the NIR and optical. ARIEL will target planets hotter than 600 K to take advantage of their well-mixed atmospheres, which should show minimal condensation and sequestration of high-Z materials and thus reveal their bulk and elemental composition. One of the major motivations for exoplanet characterisation is to understand the probability of occurrence of habitable worlds, i.e. suitable for surface liquid water. While ARIEL will not study habitable planets, its major contribution to this topic will results from its capability to detect the presence of atmospheres on many terrestrial planets outside the habitable zone and, in many cases, characterise them. This represents a fundamental breakthrough in understanding the physical and chemical processes of a large sample of exoplanets atmospheres as well as their bulk properties and to probe in-space technology. The ARIEL infrared spectrometer (AIRS) provides data on the atmospheric composition;these data are acquired and processed by an On-Board Data Handling (OBDH) system including the Cold Front End Electronics (CFEE) and the Instrument control Unit (ICU). The telescope control Unit (TCU) is also included inside the ICU. The latter is directly connected to the control and Data Management Unit (CDMU) on board the Service Module (SVM). The general hardware architecture and the application software of the ICU are described. The Fine Guidance Sensor (FGS) electronics and the Cooler control Electroni

关键词： Exoplanets atmospheres remote sensing transit spectroscopy NIR photometer payload electronics Instrument control Unit Fine Guidance Sensor telescope control

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Tomography for astronomical adaptive optics using the CANARY on-sky demonstrator

Tomography for astronomical adaptive optics using the CANARY...

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Adaptive Optics: Analysis, Methods and Systems, AO 2016

作者： Gendron, E. Morris, T. Basden, A. Vidal, F. Buey, T. Gratadour, D. Morel, C. Gach, J.-L. Feautrier, P. Stadler, E. Chemla, F. Cohen, M. Sevina, A. Younger, E. Osborn, J. Henry, D. Dipper, N. Wilson, R. Butterley, T. Biten, U. Reevesb, A. Huet, J.-M. Perret, D. Dickson, C. Atkinson, D. Longmore, A. Todd, S. Talbot, G. Morris, S. Rousset, G. Myers, R. LESIA Obs. Paris CNRS UPMC Univ. Paris Diderot 5 p. Janssen Meudon92190 France Centre for Advanced Instrumentation Durham Univ. South Road DurhamDH1 3LE United Kingdom GEPI Obs. Paris CNRS UPMC Univ. Paris Diderot 5 p. Janssen Meudon92190 France First Light Imaging S.A.S 100 Impasse des Houillères Meyreuil13590 France UMR 7326 Marseille13388 France BP 53 Grenoble Cedex 938041 France UKATC Royal Observatory Edinburgh Blackford Hill EdinburghEH9 3HJ United Kingdom

ISBN: (纸本)9781943580156

CANARY is an on-sky demonstrator instrument for the investigation of novel forms of tomographic Adaptive Optics (AO) which are required by the prospective European Extremely Large telescope (E-ELT). CANARY is deployed on the 4.2m William Herschel telescope in the Canary Islands, Spain. In its most evolved variant (Phase C2), CANARY employs four Laser Guide Star (LGS) Wavefront Sensors (WFS) and three Natural Guide Star (NGS) WFS to perform tomography on the turbulent atmospheric volume above the telescope. The projected wavefront phase error for a particular line of sight is then corrected by two Deformable Mirrors (DMs), and the resultant residual wavefront error is monitored by a further NGS WFS and an image recording camera. We outline the CANARY design, and present the most recent results obtained with a novel open/closed loop control approach designed to mimic the E-ELT. © OSA 2016.

关键词： Tomography

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Design of instrumentation and software for precise laser machining

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AIP conference Proceedings 2017年第1期1896卷

作者： D. Wyszyński Marcin Grabowski Piotr Lipiec 1)Faculty of Mechanical Engineering Cracow University of Technology Poland

The paper concerns the design of instrumentation and software for precise laser machining. Application of advanced laser beam manipulation instrumentation enables noticeable improvement of cut quality and material loss. This factors have significant impact on process efficiency and cutting edge quality by means of machined part size and shape accuracy, wall taper, material loss reduction (e.g. diamond) and time effectiveness. The goal can be reached by integration of laser drive, observation and optical measurement system, beam manipulation system and five axis mechanical instrumentation with use of advanced tailored software enabling full laser cutting process control and monitoring.

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The GMT-Consortium Large Earth Finder (G-CLEF): An optical echelle spectrograph for the Giant Magellan telescope (GMT) 6

The GMT-Consortium Large Earth Finder (G-CLEF): An optical e...

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conference on Ground-Based and Airborne instrumentation for Astronomy VI

作者： Szentgyorgyi, Andrew Baldwin, Daniel Barnes, Stuart Bean, Jacob Ben-Ami, Sagi Brennan, Patricia Budynkiewicz, Jamie Chun, Moo-Yung Conroy, Charlie Crane, Jeffrey D. Epps, Harland Evans, Ian Evans, Janet Foster, Jeff Frebel, Anna Gauron, Thomas Guzman, Dani Hare, Tyson Jang, Bi-Ho Jang, Jeong-Gyun Jordan, Andres Kim, Jihun Kim, Kang-Min de Oliveira, Claudia Mendes Lopez-Morales, Mercedes McCracken, Kenneth McMuldroch, Stuart Miller, Joseph Mueller, Mark Oh, Jae Sok Onyuksel, Cem Ordway, Mark Park, Byeong-Gon Park, Chan Park, Sung-Joon Paxson, Charles Phillips, David Plummer, David Podgorski, William Seifahrt, Andreas Stark, Daniel Steiner, Joao Uomoto, Alan Walsworth, Ronald Yu, Young-Sam Harvard Smithsonian Ctr Astrophys 60 Garden St Cambridge MA 02140 USA Univ Arizona Steward Observ 933 North Cherry St Tucson AZ 85721 USA Carnegie Inst Sci The Observ 813 Santa Barbara St Pasadena CA 91101 USA Pontificia Univ Catolica Chile Vicuna Mackenna 4860 Santiago Chile Univ Chicago 640 S Ellis Ave Chicago IL 60637 USA Korea Astron & Space Sci Inst KASI 776 Daedeokdae Ro Daejeon South Korea MIT Kavli Inst Astrophys & Space Res 77 Massachusetts Ave Cambridge MA 02139 USA Univ Calif Santa Cruz UCO Lick Observ Santa Cruz CA 95064 USA Univ Sao Paulo Rua Matao 1226 BR-05508900 Sao Paulo Brazil

ISBN: (数字)9781510601963

ISBN: (纸本)9781510601963

The GMT-Consortium Large Earth Finder (G-CLEF) will be a cross-dispersed, optical band echelle spectrograph to be delivered as the first light scientific instrument for the Giant Magellan telescope (GMT) in 2022. G-CLEF is vacuumenclosed and fiber-fed to enable precision radial velocity (PRV) measurements, especially for the detection and characterization of low-mass exoplanets orbiting solar-type stars. The passband of G-CLEF is broad, extending from 3500 angstrom to . This passband provides good sensitivity at blue wavelengths for stellar abundance studies and deep red response for observations of high-redshift phenomena. The design of G-CLEF incorporates several novel technical innovations. We give an overview of the innovative features of the current design. G-CLEF will be the first PRV spectrograph to have a composite optical bench so as to exploit that material's extremely low coefficient of thermal expansion, high in-plane thermal conductivity and high stiffness-to-mass ratio. The spectrograph camera subsystem is divided into a red and a blue channel, split by a dichroic, so there are two independent refractive spectrograph cameras. The control system software is being developed in model-driven software context that has been adopted globally by the GMT. G-CLEF has been conceived and designed within a strict systems engineering framework. As a part of this process, we have developed a analytical toolset to assess the predicted performance of G-CLEF as it has evolved through design phases.

关键词： Echelle spectrograph precision radial velocity G-CLEF GMT high dispersion spectroscopy ELTs

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