Spectrograph for INtegral Field Observations in the Near Infrared

Go to Unit Telescope 4 (UT4, Yepun) of the Very Large Telescope (VLT) at the Paranal Observatory and SINFONI can be found conducting its own beautiful observational orchestra, thanks to its two component instruments working together: SPIFFI (SPectrometer for Infrared Faint Field Imaging), which is an infrared integral field spectrograph, and the SINFONI-AO (adaptive optics) module. George Hau and Bin Yang are responsible for arranging SINFONI’s harmony with the stars.

An integral field spectrograph (IFS) allows you to observe in three dimensions across the entirety of an astronomical object in one go: each pixel of the image is associated with a full spectrum, measuring the intensity of the light at each wavelength (the wavelength is a measurement of its colour — in some objects, it can be converted into a velocity towards or away from the Earth and tells us about its relative position in space as a result.

SINFONI uses an “image slicer” technique: as shown in the figure below, a two-dimensional image (a) is chopped into smaller components (via “optical slicing”) and re-positioned by special segmented mirrors so that they lie in a line end-to-end instead of on top of each other (b). This essentially forms a very long virtual slit. The light from the virtual slit is split by SPIFFI into its separate colours and therefore wavelengths (c), and the image is then reconstructed from the individual slices at each wavelength, i.e. the image is reconstructed from all the slices at the red end of the spectrum, then the green, etc. They are then combined to give us the final, 3D information we desire (d).

Traditional methods of obtaining spectra over the full extent of a large, extended object is both time consuming and inefficient — an IFS solves both of these problems. SINFONI is therefore the ideal instrument for looking at some of the most interesting galaxies and planetary nebulae in the Universe. Because SINFONI only uses mirrors, it can be cooled to extremely low temperatures (between -150 and -273 degrees C, or “cryogenic temperatures”). This, combined with the adaptive optics module SINFONI-AO, which also works better towards the red end of the spectrum, means that overall SINFONI is tailored for observing at infrared wavelengths.

Thanks to SINFONI-AO, the instrument can also correct for atmospheric turbulence. The distorted image of a guide star is used to measure the effect of the turbulence, and a small, deformable mirror adjusts itself in real time to correct for these distortions. For the cases where a reference star is not available, the Laser Guide Star (LGS) can be used to create a bright spot 80 kilometres above the telescope and this is used as an artificial reference star. As a result, the images reaching SPIFFI are almost as sharp as if there were no atmosphere above the VLT at all — music to our ears!

Science highlights with SINFONI

  • A giant gas cloud is being ripped apart by the supermassive black hole at the centre of the Milky Way; SINFONI has been studying the cloud’s fate (eso1151, eso1332). Before that, SINFONI observed the motion of stars surrounding the black hole, which were used to measure how far away it is and its mass. (eso0846).
  • SINFONI has made many observations to study the growth and evolution of galaxies in a distant past:  at the beginning, they tended to gently snack on nearby gas (eso1040, eso1330), but at a later stage in their growth, they would cannibalise other, smaller galaxies. (eso1212)
  • The most distant galaxy ever measured to date was observed by SINFONI as it was only 600 million years after the Big Bang. (eso1041)
  • List of the scientific papers produced by SINFONI, via the ESO library TelBib database.

A raw image obtained with SINFONI. The image slicer chopped the image of a small region of the sky into a series of 32 narrow slices, and aligned them at the entrance of the spectrograph. The spectrograph then spread the light into its individual colours, forming a spectrum of each slice. Here, the 32 spectra of the individual slice appear as vertical bands. Each slice is slightly vertically offset from its neighbours. Complex data-processing software is required to re-assemble the information contained here into a full 3D spectral image.


 The authoritative technical specifications as offered for astronomical observations are available from the Science Operation page.

Site: Paranal
Telescope: VLT UT4
Focus: Cassegrain
Type: Near-infrared integral field spectrograph with adaptive optics capabilities
Wavelength coverage: Infrared, 1–2.5 μm
Spatial resolution: Adaptive optics: diffraction limited resolution (down to 0.05 arcseconds). The smallest pixel size is 0.025 arcseconds
Spectral resolution: 1500–4000
First light date: August 2004 (eso0426)
Images taken with the instrument: Link
Images of the instrument: Link
Science goals:  High spatial and spectral resolution studies of compact objects (star-forming regions, nuclei of galaxies, cosmologically distant galaxies, galactic centre).


Max Planck Institute for Extraterrestrische Physik (MPE), Garching, Germany.

Nederlandse Onderzoekschool Voor Astronomie (NOVA) in Leiden, Netherland.

The Netherlands Foundation for Research in Astronomy (ASTRON), Netherland