... Read in stellar spectra from FITS files read in BRUCE model spectra from FITS files extract a lightcurve lc(t) from the 2d spectrum f(w,t) convert 2d flux spectra f(w,t) to 2d normalized spectra remove spikes from data and replace with continuum cross-correlate individual spectra in datablock against mean spectrum construct templates for ccf computes centroids of ccfs from 2d array clean the data by removing outliers, fit and subtract low frequency background. write out results to ascii files . ...