There are two ways in which the standard-star data are tabulated, both are tables of fluxes versus wavelengths: in one, each point has a corresponding pass-band width; in the other, each point is a fit to a continuum curve. In the first case, the published standard and your observed standard should look the same once the flux in the appropriate pass bands has been summed - even when absorption features are present in the spectrum. In the second case you must either fit a continuum to your data or, if there are no absorption features present in the wavelength range covered, you might just interpolate between the points in the published standard.
Simple Spectroscopy Reductions