An automatic set of procedures will be available to process the data acquired from standard OSIRIS observing modes. At least (a) standard imaging, (b) long-slit spectroscopy, (c) charge shuffling imaging and (d) fast photometry observing modes will be processed using the pipeline. The processing is done in two phases: a pre-process and a post-process. The pre-processing procedures include standard CCD operations: bias subtraction, dark current correction, flat-field correction, and cosmic-ray events removal.
Post-processing of data depends of the observing mode and will include wavelength calibration and geometric distortion correction. Required calibration frames will be taken either from existing databases or acquired frames during observations.
During observations, images will be displayed after acquisition. It will be possible to use basic tools to analyse the images and to perform statistics and profile measurements. Users may need to perform a quick reduction for fast scientific assessment of the data.
The OSIRIS Data Factory is completely included in the GCS Data Factory subsystem at the Operations Co-ordination level. The GCS hardware and software standards will be used in the design and implementation of the OSIRIS Data Factory.
Data Factory use cases are embedded into this use case. All frames, both science and calibration, are processed in the right way to finally obtain reduced scientific data. There are two types of processing:
Calibration frames processing: Calibration frames (zero, flat-fields, arc lamps, TF arcs, etc.) are processed before they could be used to process science (target) frames. These calibration data are combined to produce flat-field frames adequate for each observing mode. Other necessary parameters are also obtained after this processing such as wavelength calibration solutions and TF parameters. The processed calibration frames are then validated and are ready to be archived by the "Operation Repository".
Science (target) frames processing: Using the calibration frames and parameters already processed, target frames are pre and post processed. These processes include bias subtraction, flat-field correction, cleaning of cosmic-ray events and cosmetics (pre-processing), and geometric distortion correction and wavelength calibration. Post processing tasks are observation-type dependent.
Last update July 8, 2005, by Héctor Castañeda