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WFCEXP
This program takes as input an ASTERIX binned dataset (created by the
WFCSORT program) and converts the counts in the data_array component
into flux normalised to the on axis response of the WFC. (ie it
produces a flux which would have obtained had each element of
data_array been located on the optical axis of the instrument. The flux
calculation takes into account the following instrument dependencies:
- Instrument dead time effects (the event rates needed for the
calculation are stored in the .HKR file which is part
of the standard observation dataset).
- Instrument vignetting effects. The Instrument pointing is derived
from the .ATT file. The vignetting at points within the
field is derived from the filter and detector information stored
in the WFC Calibration File (with the logical name CAL_WFC_MASTER).
- Optionally the program may correct the fluxes in a dataset for the
degradation of the detector efficiency. The time history of the
efficiency is stored in the calibration file and is used to
determine an interpolated value at the epoch appropriate to the
dataset. The user is warned if the dataset epoch is beyond the
end of the current time history in the calibration file. In this
event the latest value for detector efficiency is used.
- Optionally the program may correct the fluxes in a one dimensional
dataset for the fraction of the point response function which fell
outside the source centred circle from which events were
originally accepted by the WFCSORT program.
Subtopics:
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