The ESO 3.6m Telescope


ESO 3.6m Telescope

The ESO 3.6m Telescope was commissioned in 1977, and completely upgraded in 1999. In 2004 a new secondary mirror cell was manufactured, improving considerably the image quality of the telescope. In 2007 the control system of the lateral pads was upgraded. The image quality of the telescope is better than 0.2 arcsec at Zenith. The telescope has a horseshoe/fork mounting, and an interchangeable top unit allowing the secondary mirror to be changed from a F/8 to a F/35 Cassegrain focus. The pointing error is about 5 arcsec RMS. The pointing is limited to 70 deg. zenithal distance, and 5.5h HA, but a small region under the pole is reachable. Operation and maintenance of the telescope is the responsibility of ESO.
Since April 2008 HARPS, using the F/8 Cassegrain focus, is the only instrument available at the 3.6m.

The telescope is at a geographical location of 70.7345W, 29.2584S, and an altitude of 2400 metres above sea level.

News and Updates

  • Main mirror aluminized on August 12th 2008
  • Nov. 2006: Maintenance of the 3.6m dome is completed. The dome is working smoothly.
  • Main mirror aluminized on September 13th 2005.
  • Aug. 2004: The telescope reaches an image quality better than 0.2 arcsec at Zenith.

Current Instruments

The ESO 3.6m telescope host the following instrument:

  • HARPS: The High Accuracy Radial velocity Planet Searcher at the ESO La Silla 3.6m telescope is dedicated to the discovery of extrasolar planets. It is a fibre-fed high resolution echelle spectrograph.

Decommissionned Instruments

  • CES: A spectrograph providing a resolving power of up to 235,000 in the 346 - 1028 nm region.
  • EFOSC2: The ESO Faint Object Spectrograph and Camera (v.2) to give its full name, is a very versatile instrument for low resolution spectroscopy and imaging.
  • TIMMI-2 Thermal Infrared MultiMode Instrument dedicated to the 3 micron to 25 micron

Content of these Pages

The following items are available on the 3.6m Telescope pages, using the bar on the left.

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