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Response Function

On a regular basis, the observatory observes a standard star that has a reasonably well characterised spectral energy distribution. The purpose of the sw_respfunc recipe is to use this data to calculate the instrument throughput. It is used for quality control purposes and observers will have little use for this routine.

The recipe takes the FITS image created by isaacp sw_spjitter, extracts the spectrum, correlates the RA and DEC in the FITS header with a star in the catalogue and calculates the efficiency and the conversion curves.

The output consists of four files:

_extr.tfits is the extracted spectrum
_back.tfits is the background spectrum
_conversion.tfits is the conversion curve
_efficiency.tfits is the efficiency curve

Christopher Lidman