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.

• Parameters