The most direct way to deal with data where the published values represent fitted continuum values is to fit a continuum to your observed data, interpolate the tabulated data, and divide the two resulting spectra to get a calibration spectrum.
Fitting a continuum is a task that is not easily automated. The simplest way in Figaro is to display the spectrum and then use `cfit'. For example:
ICL> splot standobs reset accept ICL> cfit output=standfit
will enable you to use the graphics cursor to indicate continuum points on the displayed spectrum and thus generate the continuum spectrum by spline interpolation. A messy job, but not one you have to do often. Remember that the messy parts of the flux calibration are connected with generating the calibration spectrum, and you only have to do that once; applying it is simple.
The published points represent a smooth curve, so just interpolating directly between them should be quite satisfactory. That is, there should be no need to edit the spiketrum generated by `gspike' prior to using `interp', although `spied' is always available if necessary. This time, since HD 84937 is an Oke & Gunn standard, let's use G158-100 instead. So the first two steps will be
ICL> gspike spectrum=standobs table=g158m100 spiketrum=gmspike ICL> interp spiketrum=gmspike spectrum=gmfit
generates `gmfit' as the interpolated spectrum from the published points.
Dividing `gmfit' by `standfit' will now generate the required calibration spectrum. Note that `idiv' will not do, since the division has to allow for the wavelength range of each element, and for the exposure time. The command `caldiv' must be used instead.
ICL> caldiv standard=gmfit spectrum=standfit output=calib
will generate `calib' as the required calibration spectrum.
FIGARO A general data reduction system