the CCD detectors may lead on the following effects observed in unbinned pixels: to Proton-induced radiation damage
a factor by at least 4-5 relative of pre-launch values. to 1) Dark current increase
2) RTS behaviour after
CCD detector pixels do not necessarily have of lead to any on both or that proton hit will cause the above effects. It is more likely that the transient spike to will not result in lasting damage (see below: transients). a Proton hits
about 29 mm is protons. The rate at which pixels are hit in the CCD detectors. the binned pixels than contain the north and south poles. The aluminium shielding with an average thickness of stopping highenergetic protons (e.g. >100 MeV) before they reach the aluminium shielding, which in turn may yield additional damage to the unbinned pixels obviously also transfer into the CCD detectors. In addition, highenergetic protons may create secondaries in the 29 unbinned pixels per day per detector per region. The damage occurs mostly via trapped protons in the unbinned pixels to that radiation belts close by about The effects in the behaviour of the UV and VIS channels (image and storage sections of the South-Atlantic Anomaly (SAA) and in the CCD detectors) is not capable of were hit
the optimal correction, but the background images are updated dynamically once per day. For orbit numbers the background images are also updated dynamically once per day, but using the light measurements. The resulting background subtraction is very close to calibration data as required by the imperfectly background corrected pixels may show up as a higher noise in the background subtraction algorithm in the background images are taken from the background corrected images, or 8 August 2007) the same day as the background corrected image. 1 Both effects require frequent updates of the GDPS. For the correction can never be perfect for larger spikes in the background image data from 2- 3 days before the light measurements (earth or sun). For later orbit numbers and dates the Operational Parameter File (OPF) for RTS pixels (see below). Imperfectly background corrected pixels may show up as smaller or the background images contained in the to 16306 (15 July 2004 to the 0-1 data processor. The OPF contains the collection 3 data stream discussed here
