FlexureFlexure at the CCD is measured at about +/-3 pixels over the whole sky with the locking screws for the CCD stage in place, or about +/-5 pixels (for 15 micron pixels) without the locking screws. This is a real problem for spectroscopy with a chip which produces pronounced interference fringes, since the fringes in the flat field will not match the fringes in the data unless the flat is done at the same position as each observed object. You may choose to ignore this source of error, or make a low frequency map of the flats and shift it to match the flexure, or not use flat fields at all, or take flats to match every object, or some other method of your own devising, but it will in any case require some consideration. Similarly, the flexure will affect your wavelength calibration, but this may be corrected for by using skylines to re-determine the zero point for each observation. If you want maximum accuracy you may wish to do a line lamp calibration before and after each object observation. It's a nuisance, but they are fairly fast to do.
Support Astronomers (firstname.lastname@example.org) Last modified: Tue Jul 17 18:44:07 PDT 2012