The spectral characteristics described above, especially the presence of the Ca II triplet in emission and the absence of He II emission, places V589Sgr as a special member in the class of symbiotic stars. 7633 -10 Table 1 lists the equivalent width and the radial velocity for the main spectral lines. Heliocentric radial velocities were measured by fitting Gaussian functions to the profiles whereas the equivalent width was obtained by integration of the flux between the points where the profile merges with the continuum. The errors reflect the root mean square of the averages. Several lines cannot be identified.
Possible causes are line blending or existence of lines of high excitation ions.
The above average of H I velocities does not consider the low velocity H and H lines, since these lines are likely contaminated with Fe I and Fe II and might suffer of wavelength calibration biases on the CCD blue edge. A long-term study is necessary to confirm the radial velocity variability of this star.