Diseño electrónico y algoritmos de control para micro-posicionadores de fibra óptica en instrumentación astrofísica

Tras los óptimos resultados obtenidos en 2013 con el desarrollo del posicionador y la electrónica de control para el proyecto BigBOSS, la dirección del proyecto decidió re-plantear el sistema diseñado, con el objetivo de aumentar sus prestaciones en cuanto a resolución, precisión y velocidad de posicionado se refiere. Así , el Laurence Berkeley National Laboratory (Berkeley Lab.), optó por aumentar la densidad de robots posicionadores de fibra instalados en el plano focal del telescopio NOAO 4m Mayall (Arizona), renombrando el proyecto como DESI (Dark Energy Spectroscopic Investigations). Para ello, todos los grupos de investigación implicados en el diseño de los posicionadores de fibra del telescopio, se vieron obligados a reducir las dimensiones de sus prototipos, con el objetivo de seguir formando parte protagonista del proyecto. De este modo, tras la experiencia recogida con el desarrollo y prueba del posicionador y el sistema de control electrónico para el proyecto BigBOSS, el grupo español formado principalmente por el Instituto de Astrofísica de Andalucí a (IAA-CSIC), el Instituto de Física Teórica (UAM-CSIC), el grupo de investigación HCTLab (EPS-UAM) y la empresa AVS (Added Value Solutions) decidieron redimensionar el diseño planteado. Para ello, y debido a las duras restricciones físicas del nuevo diseño, se replantearon de forma radical todas las propiedades básicas del actuador, y fundamentalmente el tamaño y tipo de motores. Esto forzó un replanteamiento completo de la filosofía de control utilizada en la manipulación del robot. De este modo, este Trabajo Fin de Máster por un lado, recoge los detalles del diseño para la electrónica de control del nuevo posicionador, por otro expone y detalla la nueva filosofía de control, desarrollando los principales algoritmos que la componen y finalmente recoge los frutos de la caracterización completa del único prototipo fabricado hasta la fecha por el grupo español en el proyecto DESI.After the good results achieved in 2013 with the developed ber positioner and the control electronics for BigBOSS, the project sta decided to re-de ne de designed philosophy, with the main purpose of increase its principal characteristics, in terms of resolution, precision and placement velocity. Thus, the Laurence Berkeley National Laboratory (Berkeley Lab.) decided to increase the density of ber positioner robots in the NOAO 4m Mayall Telescope focal plate (Arizona), re-naming the project as DESI (Dark Energy Spectroscopic Investigations). To accomplish this purpose, all the research groups included in the project were forced to reduce the design of their prototypes, with the main goal of keep themselves inside the project. In this way, with the experience reached in the BigBOSS project with the last ber positioner and its electronics, the Spanish research group in which it could be highlighted the Istituto de Astrof sica de Andaluc a (IAA-CSIC), the Instituto de F sica Te orica (UAM-CSIC), the research group HCT Lab (EPS-UAM) and the company AVS (Added Value Solutions), decided to re-de ne the main design. To do that and considering the hard structural restrictions of the new design, all the main properties of the actuator and principally the length and kind of the motors were re-de ned, forcing an overall concept modi cation. Thus, this Final Master Work, on the one hand picks up all the design details of the new control electronics, explaining also the new control philosophy and the complete set of control algorithms, nally this work gathers all the results obtained with the characterization of the manufactured robot prototype by the Spanish research group of the DESI project

The Robotic Multi-Object Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI)

A system of 5,020 robotic fiber positioners was installed in 2019 on the Mayall Telescope, at Kitt Peak National Observatory. The robots automatically re-target their optical fibers every 10 - 20 minutes, each to a precision of several microns, with a reconfiguration time less than 2 minutes. Over the next five years, they will enable the newly-constructed Dark Energy Spectroscopic Instrument (DESI) to measure the spectra of 35 million galaxies and quasars. DESI will produce the largest 3D map of the universe to date and measure the expansion history of the cosmos. In addition to the 5,020 robotic positioners and optical fibers, DESI's Focal Plane System includes 6 guide cameras, 4 wavefront cameras, 123 fiducial point sources, and a metrology camera mounted at the primary mirror. The system also includes associated structural, thermal, and electrical systems. In all, it contains over 675,000 individual parts. We discuss the design, construction, quality control, and integration of all these components. We include a summary of the key requirements, the review and acceptance process, on-sky validations of requirements, and lessons learned for future multi-object, fiber-fed spectrographs

The Robotic Multi-Object Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI)

International audienceA system of 5,020 robotic fiber positioners was installed in 2019 on the Mayall Telescope, at Kitt Peak National Observatory. The robots automatically re-target their optical fibers every 10 - 20 minutes, each to a precision of several microns, with a reconfiguration time less than 2 minutes. Over the next five years, they will enable the newly-constructed Dark Energy Spectroscopic Instrument (DESI) to measure the spectra of 35 million galaxies and quasars. DESI will produce the largest 3D map of the universe to date and measure the expansion history of the cosmos. In addition to the 5,020 robotic positioners and optical fibers, DESI's Focal Plane System includes 6 guide cameras, 4 wavefront cameras, 123 fiducial point sources, and a metrology camera mounted at the primary mirror. The system also includes associated structural, thermal, and electrical systems. In all, it contains over 675,000 individual parts. We discuss the design, construction, quality control, and integration of all these components. We include a summary of the key requirements, the review and acceptance process, on-sky validations of requirements, and lessons learned for future multi-object, fiber-fed spectrographs

The Robotic Multi-Object Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI)

A system of 5,020 robotic fiber positioners was installed in 2019 on the Mayall Telescope, at Kitt Peak National Observatory. The robots automatically re-target their optical fibers every 10 - 20 minutes, each to a precision of several microns, with a reconfiguration time less than 2 minutes. Over the next five years, they will enable the newly-constructed Dark Energy Spectroscopic Instrument (DESI) to measure the spectra of 35 million galaxies and quasars. DESI will produce the largest 3D map of the universe to date and measure the expansion history of the cosmos. In addition to the 5,020 robotic positioners and optical fibers, DESI's Focal Plane System includes 6 guide cameras, 4 wavefront cameras, 123 fiducial point sources, and a metrology camera mounted at the primary mirror. The system also includes associated structural, thermal, and electrical systems. In all, it contains over 675,000 individual parts. We discuss the design, construction, quality control, and integration of all these components. We include a summary of the key requirements, the review and acceptance process, on-sky validations of requirements, and lessons learned for future multi-object, fiber-fed spectrographs

The Robotic Multiobject Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI)

A system of 5,020 robotic fiber positioners was installed in 2019 on the Mayall Telescope, at Kitt Peak National Observatory. The robots automatically re-target their optical fibers every 10 - 20 minutes, each to a precision of several microns, with a reconfiguration time less than 2 minutes. Over the next five years, they will enable the newly-constructed Dark Energy Spectroscopic Instrument (DESI) to measure the spectra of 35 million galaxies and quasars. DESI will produce the largest 3D map of the universe to date and measure the expansion history of the cosmos. In addition to the 5,020 robotic positioners and optical fibers, DESI's Focal Plane System includes 6 guide cameras, 4 wavefront cameras, 123 fiducial point sources, and a metrology camera mounted at the primary mirror. The system also includes associated structural, thermal, and electrical systems. In all, it contains over 675,000 individual parts. We discuss the design, construction, quality control, and integration of all these components. We include a summary of the key requirements, the review and acceptance process, on-sky validations of requirements, and lessons learned for future multi-object, fiber-fed spectrographs