All Tables

Table 1: HD 102065 ``fact sheet''. A_v is the visible extinction, E(B-V) is the color index (Boulanger et al. 1994). ${\rm {H}_{2}}$ column densities from (Gry et al. 2002). The total column density ( $N_{\rm H} = N({\rm H}) + 2 N({\rm H}_2$ )) has been derived from E(B-V).
Table 2: Wavelength and f-values for the observed absorption lines. Most of those values are from Morton (2000 and 2001) & Verner et al. (1994). Oscillator strengths values for S I are taken from Beideck et al. (1994). Values for O I $1355.5977~\textrm{\AA}$ and Ni II $1317.2170~\textrm{\AA}$ are from Welty et al. (1999). CO oscillator strengths have been kindly provided by Dr. Eidelsberg.
Table 3: Molecular absorption lines detected in the optical spectra. Listed parameters are from Gredel et al. (1993).
Table 4: Results from emission line measurements. H I measurements are performed on the difference spectrum (see text and Fig. 5). The H I component at $14.5~{\rm ~ km ~ {s}^{-1}}$ is not detected in absorption and is probably due to background gas situated behind the star HD 102065.
Table 5: Interstellar component characteristics derived from the absorption lines in the UV and optical spectrum. The ions absorption in component 1 may be distributed over the velocities of components A and B however the fits have been performed with one component. Velocities: the listed uncertainties on $V_{\rm LSR}$ apply to relative velocities. The absolute uncertainty from the precision of the STIS wavelength calibration is about $1.2~{\rm {km~s}}^{-1}$ , absolute velocities have however been confirmed to about $0.3~{\rm {km~ s}}^{-1}$ by the good agreement between component C and the CO emission in the heterodyne data, which have an absolute precision of $0.1~{\rm {km~ s}}^{-1}$ . Temperature: when possible, temperatures are derived from the combination of b-values from species of different masses. The precise temperatures for components A and B have been derived under the assumption that they can be identified to the two components seen in emission in the Blue Cloud H I spectrum. Column densities (in cm^-2): numbers in parentheses are powers of 10. All error bars are 3 $\sigma$ uncertainties, except for the intervals given by the arrows, indicating and upper limit derived from a faint line and a lower limit derived from a strong saturated line. Si II, C II and C II* profiles are saturated for all components, implying that only a lower limit could be derived for the whole absorption.