All Tables

• Table 1: Main astrophysical parameters. References: ^a van den Ancker et al. (1998), ^b Donati et al. (1997), ^c Gerbaldi et al. (2001), ^d Abt et al. (2002), ^e Royer et al. (2002).
• Table 2: Observing log. The fourth column gives the number of sub-exposures. The S/N ratios are given per resolution element.
• Table 3: Derived parameters for the CS species identified in absorption in HD 100546 spectrum. The velocities are given in the star's rest frame. "sat'' is for saturated lines, "var'' for variability. For the saturated absorption lines, we measured the velocity of the centroid. For the species which present no temporal spectral variation, we give the velocity and the column density calculated from the average of the two spectra.
• Table 4: Long-term variable CS spectral features in HD 100546 spectrum. is the ratio of the radiation pressure to the stellar gravity. For Fe II, the  value listed is taken from Beust et al. (2001).
• Table 5: Short-timescale variable CS gas in the HD 100546 spectrum of 2002. The velocity of the centroid is given in the stellar rest frame.
• Table 6: Emission line measurements. The second column gives the total integrated flux of the observed profile (not corrected for reddening). The third column gives the number of components used to model the line profile with simple Gaussians. The last three columns give the parameters for each component: the central velocity in the stellar rest frame, the Full Width Half Maximum ( FWHM) and the corresponding integrated flux.
• Table 7: CS absorption lines identified in the HD 100546 FUSE spectrum. Below 1100 Å, the low flux level does not allow clear identification of weak CS atomic lines, and the main CS features in the spectrum are due to H₂ transitions.