The CES quick-look tool has evolved beyond a mere quick-look tool, towards pipeline functionality, although
its main objective still is to provide a quick way to check the quality of
the data. It is a background task running on the offline data reduction terminal so the
data are automatically reduced and displayed in real time. The pipeline will perform
bias subtraction and wavelength calibration before
displaying the resulting spectrum in units of S/N, providing
an immediate measure of the data quality. Dark correction is done with the latest
(master-)dark from the calibration database. Extracted spectra are written as fits-files for easy examination.
For each pixel in the dispersion direction more than 300 pixels are summed across the dispersion, hence cosmic
rays are a real problem. The pipeline removes cosmics with a simple MIDAS routine before
extracting the spectrum. The spectra are not flat-fielded by default, which is a concious choice: several spectral orders
are contaminated by grating ghosts, which even a simple
flatfielding often can remove quite well. But for checking
the data quality, it is important to be able to see that the ghost is not on top of an important spectral
feature, hence we choose as default to turn off the flat fielding. However, a master-flatfield is automatically produced, and the
user can choose to turn on flat-fielding at any time.
The pipeline offers the possibilty to re-reduce data. This way, observers may choose to rereduce
their science frames using ThAr calibrations obtained throughout the night, and turning flatfielding on or
off as desired.
Observers should be fully aware that the pipeline does not guarantee science quality reductions, and is primarily
offered as a means of checking the data quality on-the-fly. For more information, please consult the
CES Pipeline Manual.
Although it is foreseen that the pipeline can run on other computers for off-line reduction, this is currently not
possible.
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