It should be clear from the discussions above how, in principle, the
different types of calibration data should be used in the analysis
of ISOCAM data.
The ubiquitous dark current and flat-field corrections are governed by a
simple equation for the cosmic flux in detector units:
 |
(6.1) |
. While it is often possible
to extract calibration components that match exactly the optical
configuration of an observation, even in these ideal circumstances the
so-called lens wheel jitter can compromise to some extent the accuracy
of the data by causing edge effects.
When the CAL-G files do not contain components that match exactly the configuration of an observer's data, the question arises of the best alternative that should be chosen. In the discussion above the references of type `component=ccg_ component(p1,p2,...)' show the significant parameters for each calibration component. AAC has implemented a scheme in which alternatives are assessed on the basis of their distance in selection parameter space from the exact match. An OLP FORTRAN code fragment is given in Appendix D which shows the applied selection rules.