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Primera luz para el más grande sistema de óptica adaptativa
La Unidad de Telescopio 4 da un paso decisivo para lograr plenamente el sistema de óptica adaptativa
28 de Octubre de 2016
Se ha alcanzado un importante hito en el proyecto para transformar la Unidad de Telescopio 4 (Yepun) del Very Large Telescope de ESO (VLT), en un telescopio totalmente adaptativo, con la instalación de un espejo secundario deformable en el telescopio.
Los sistemas de óptica adaptativa compensan el efecto borroso causado por la atmósfera terrestre que degrada la nitidez de las imágenes obtenidas con los telescopios, inclusive con un telescopio de la magnitud y sofisticación del VLT. La instalación del nuevo sistema de Óptica Adaptativa (AOF) como una parte integral de UT4 permitirá al telescopio obtener imágenes aún más nítidas.
El espejo secundario deformable consiste en un espejo flexible de 2.2mm de espesor, montado sobre un sistema que contiene 1170 actuadores que permiten cambiar la forma del espejo para corregir los efectos causados por la turbulencia de la atmósfera. Con poco más de un metro de diámetro, es el mayor espejo para óptica adaptativa que jamás se haya producido. El espejo deformable ha requerido tecnología de vanguardia y la trayectoria de su desarrollo comenzó hace varios años. La construcción de la “óptica de referencia”, esencialmente el soporte del espejo, se terminó en el año 2010, y la primera versión del delgado espejo se entregó a la Sede Central de ESO en Garching, a fines del 2011, prosiguiendo con una versión perfeccionada en el 2014. Luego de extensos controles de rendimiento realizados en Garching, el montaje del espejo secundario deformable se envió a Chile y ha sido montado en el telescopio Yepun de 8,2 metros de diámetro.
Recientemente se ha realizado la alineación óptica y se ha sometido al espejo deformable a diversas pruebas, en modo rígido y montado en el telescopio, las cuales ha superado con éxito.
Además de reemplazar el espejo secundario convencional del telescopio con este nuevo espejo secundario, el Sistema de Óptica Adaptativa también incluye el Four Laser Guide Star Facility (4LGSF), cuya primera luz se realizó en abril del 2016, como también la instalación de módulos de óptica adaptativa en diversos focos del espejo secundario. Los módulos de óptica adaptativa son GRAAL (GRound laser Adaptive optics Assisted by Lasers), que alimentan imágenes corregidas a los instrumentos HAWK-I y GALACSI (Ground Atmospheric Layer Adaptive Corrector for Spectroscopic Imaging), que filtran imágenes para el espectrógrafo MUSE.
Se han desarrollado, asimismo, otras herramientas adicionales para optimizar la operación del Sistema AOF que ya están en funcionamiento. Ellas incluyen el software denominado Astronomical Site Monitor, que monitorea la atmósfera para determinar la altitud en que ocurren las turbulencias, y el sistema de Control de Tráfico Láser, que impide que los rayos del sistema 4LGSF interfieran con aeronaves o telescopios espaciales.
Con el advenimiento del Sistema AOF, el VLT continuará expandiendo su listado de resultados científicos de categoría mundial, y la experiencia con el sistema de Paranal servirá para superar los desafíos técnicos que plantea el próximo gran proyecto de ESO: la construcción del European Extremely Large Telescope.
Enlaces
Contactos
Robin Arsenault
ESOGarching bei München, Alemania
Tel: +49 89 3200 6524
Correo electrónico: rarsenau@eso.org
Peter Grimley
ESO, Assistant Public Information Officer
Garching bei München, Alemania
Tel: +49 89 3200 6383
Email: pgrimley@eso.org
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