Instrumentos del VLT

  • 4LGSF (4 Laser Guide Star Facility, Instalación de 4 estrellas de guiado láser) envía cuatro rayos láser al cielo para producir cuatro estrellas artificiales al excitar átomos de sodio de la atmósfera.
  • CRIRES (CRyogenic high-resolution InfraRed Echelle Spectrograph, Espectrógrafo criogénico Echelle de alta resolución en el infrarrojo) proporciona un poder de resolución de hasta 100.000 en el rango espectral de 1 a 5 micrones.
  • ESPRESSO (Echelle SPectrograph for Rocky Exoplanet and Stable Spectroscopic Observations, espectrógrafo Echelle para exoplanetas rocosos y observaciones espectroscópicas estables) es un espectrógrafo óptico de alta resolución súper estable para el foco coudé combinado del VLT.
  • FLAMES (Fibre Large Array Multi-Element Spectrograph, Espectrógrafo con Matriz de Fibras Multi Elemento) permite, gracias a su capacidad única, estudiar de manera simultánea y en alta resolución espectral cientos de estrellas individuales ubicadas en galaxias cercanas. También está equipado para espectroscopía de campo integral.
  • FORS2 (FOcal Reducer and Spectrograph, Reductor Focal y Espectrógrafo de baja dispersión)  es un instrumento con funciones múltiples que puede emplearse para la obtención de imágenes en luz visible y para la espectroscopía de baja resolución.
  • HAWK-I (High Acuity Wide field K-band Imager, Cámara de Gran Campo y Alta Agudeza en  banda-K)  es una cámara que opera en el infrarrojo cercano con un campo visual relativamente amplio.
  • KMOS (K-band Multi Object Spectrograph, Espectrógrafo Multiobjeto en banda K) es un espectrógrafo de infrarrojo cercano equipado con 24 unidades de campo integral, las que pueden posicionarse de distintas maneras.
  • MUSE (Multi-Unit Spectroscopic Explorer, explorador espectroscópico multi unidad) es un espectrógrafo de campo integral gigante que puede tomar espectros usando todo su campo de visión, de cerca de un arcominuto cuadrado.
  • NACO es un sistema de Óptica Adaptativa capaz de producir imágenes tan nítidas como las captadas en el espacio. Además está equipado con un espectrómetro, un polarímetro,  un coronógrafo, entre otros.
  • SINFONI (Spectrograph for INtegral Field Observations in the Near Infrared, Espectrógrafo para  observaciones de campo integral en el Infrarrojo Cercano) es un espectrógrafo de campo integral para observaciones en el infrarrojo cercano (1 - 2,5 micrones) alimentado por un módulo de óptica adaptativa.
  • SPHERE (Spectro-Polarimetric High-contrast Exoplanet REsearch, Búsqueda de exoplanetas por espectropolarimetría de alto contraste) es un sistema de óptica adaptativa extrema con avanzados coronógrafos, diseñado para observar exoplanetas.
  • UVES (Ultra-violet and Visible Echelle Spectrograph, Espectrógrafo Echelle para observaciones en luz visible y ultravioleta) es el espectrógrafo de alta dispersión del VLT, capaz de observar desde 300 a 1.100 nanómetros, con una resolución espectral máxima de 110.000.
  • VIMOS (VIsible Multi-Object Spectrograph, Espectrógrafo Multiobjeto en Luz Visible), un generador de imágenes y espectrógrafo multiobjeto de cuatro canales, permite obtener   espectros de baja resolución de hasta 1.000 galaxias al mismo tiempo.
  • VISIR (VLT Imager and Spectrometer for mid-Infrared, Espectrometría e imagen en el infrarrojo medio para el VLT) estudia la luz infrarroja de objetos celestes.
  • X-shooter es un espectrógrafo capaz de abarcar una gama muy amplia de longitudes de onda [UV a infrarrojo cercano] de manera simultánea.

Instrumentos fuera de servicio

  • ISAAC (Infrared Spectrometer And Array Camera, Conjunto de Cámaras y Espectrómetro Infrarrojo)  es un generador de imágenes y espectrómetro criogénico infrarrojo capaz de realizar observaciones en el rango de 1 a 5 micrones.
  • FORS1 (FOcal Reducer and Spectrograph, reductor focal y espectrógrafo) es un instrumento multimodal, similar a FORS2.
  • MAD (Multi-conjugate Adaptive optics Demonstrator) es el instrumento multiconjugado para demostrar el funcionamiento de la óptica adaptativa de ESO.
  • MIDI (MID-infrared Interferometric) es un instrumento interferométrico del infrarrojo medio para fotometría y espectroscopía.

Telescopios e instrumentos en funcionamiento y en proyecto de Paranal

Instrumentos del VLTI

  • AMBER (Astronomical Multi-Beam combineR) es un instrumento que trabaja en el infrarrojo cercano, capaz de integrar los haces de luz de tres telescopios, destinado a estudios fotométricos y espectroscópicos.
  • GRAVITY es un instrumento de segunda generación instalado en el VLTI (Very Large Telescope Interferometer y representará un gran paso adelante tanto para la interferometría como para el VLT (Very Large Telescope).
  • MATISSE es un nuevo espectro-interferómetro, parte de la segunda generación de instrumentos del VLTI (Interferómetro del VLT).
  • NAOMI (New Adaptive Optics Module for Interferometry, nuevo módulo de óptica adaptativa para interferometría), está a punto de dar un importante impulso al VLTI.
  • PIONIER (Precision Integrated-Optics Near-infrared Imaging ExpeRiment, experimento de imagen del infrarrojo cercano con óptica integrada de precisión) combina la luz de los 4 telescopios en el infrarrojo cercano.

Puede encontrar una descripción detallada de estos instrumentos en la tabla resumen de instrumentos de ESO.

Muchos de estos instrumentos han sido construidos, en colaboración con ESO, por  consorcios de laboratorios europeos.

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