Outline of Basic Pipeline

The steps in the basic pipeline are as follows:

1. Input reset-corrected single frames 1 MEF per pointing

2. Non-linearity correction if needed

3. Update master dark, flatfield frames and bad pixel masks

4. Dark-correct, flatfield and gain-correct on-sky data

5. Update current running sky estimate if appropriate

6. Sky subtract all target frames

7. Remove further instrumental artefacts if present

8. Derive internal astrometric transformation if necessary

9. Form interlaced superframe and pixel variance map

10. Generate object catalogues
    • Astrometric and photometric calibration

    • Morphological classification

    • Data quality control measures

    • Check by matching with 2MASS catalogue