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The steps in the basic pipeline are as follows:
- Input reset-corrected single frames 1 MEF per pointing
- Non-linearity correction if needed
- Update master dark, flatfield frames and bad pixel masks
- Dark-correct, flatfield and gain-correct on-sky data
- Update current running sky estimate if appropriate
- Sky subtract all target frames
- Remove further instrumental artefacts if present
- Derive internal astrometric transformation if necessary
- Form interlaced superframe and pixel variance map
- Generate object catalogues
- Astrometric and photometric calibration
- Morphological classification
- Data quality control measures
- Check by matching with 2MASS catalogue
Nigel Hambly
2002-10-02