La Silla - Science Operation Department History of changes at the 2.2-m telescope
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Detailed schedule of changes

The schedule of changes below details the dates at which modifications were carried out at WFI which can affect the flat fields and other properties of the instrument. Data in one configuration should not be reduced with calibrations from other. This is particularly true for flat fields and for zero point maps.

• Configuration 12: (26 Dec 2005) WFI was warmed-up and cooled down. Decontaminated CCDs.
• Configuration 11: (14 September 2005) WFI CCDs were contaminated. New configuration after detox in this date.
• Configuration 10: (23 June 2005) realuminization of M1
• Configuration 9: (16 March 2005 to present date) baffle 5 plus FEROS ADC in FEROS adapter
• Configuration 8: (5 March 2005 -- 15 March 2005) baffle 3 without FEROS adapter.
• Configuration 7: (18 April 2004-5 March 2005) baffle4 plus added velvet to eliminate unwanted reflection spots: baffle5. Covered selected annular segments of the walls surrounding the light path with velvet.
• Configuration 6: (XXX date) baffle3 plus FEROS, plus extra baffle ring in FEROS adapter: baffle4
• Configuration 5: (XXX date) baffle3 plus FEROS adapter
• Configuration 4: (Beginning of 2003) Improved baffle: baffle3, no vignetting.
• Configuration 3: (12 December 2002) Rings taken out (but spacer in), return to original baffle1.
• Configuration 2: (18 September 2002) Before FEROS, rings added to baffle: baffle2. The rings were found to cause a slight vignette but were on the telescope for a couple of months. At the same time a spacer was added between WFI and the telescope (20 mm). Now the distance of M1 and M2 is not the same as before. This should add negligible aberrations but might affect precision astrometry.
• Configuration 1: Beginning of WFI until 18 September 2002) Original baffle: baffle1

Send comments to <ls-sciops@eso.org> Last update: Jan 05, 2006