A copy of this work was available on the public web and has been preserved in the Wayback Machine. The capture dates from 2007; you can also visit the original URL.
The file type is
Radial Velocities Heliocentric radial velocities of the principal components have been determined by using the cross-correlation technique. The spectra of the program stars were cross-correlated order by order, using the routine FXCOR in IRAF, against spectra of radial velocity standards of similar spectral types. The radial velocity of the components is derived from the position of the cross-correlation peak. In the case of BD+39 2587 we observe the chromospheric emission lines of bothfatcat:ozhpjhimavhkrlwoevn3unag3u