All Tables

Table 1: Log of VLA observations. The date, programme and configuration are listed, as well as the wavelength observed and the integration time on HD 168112 (in min). Fluxes are given in Table 10.
Table 2: Fluxes of the flux calibrator 3C48, based on the 1995.2 VLA coefficients (Perley & Taylor 1999). The two values for each entry correspond to the two 50 MHz sidebands (IF1 and IF2).
Table 3: Performed duration and effective exposure time of both observations (April and September 2002). The difference between the performed and effective duration of the exposures is only due to overheads.
Table 4: Stellar parameters of HD 168112 taken from Leitherer (1988).
Table 5: Best-fit parameters for EPIC spectra of HD 168112 in the case of a wabs $_{{\rm ISM}}$ *wind*(2-T mekal) model. Results are given for combined MOS, pn, and combined EPIC spectra. The upper and bottom parts of the table concern the first and second observation respectively. The ISM absorption component ( wabs $_{{\rm ISM}}$ ) is frozen at 0.58 $\times$ 10²² cm^-2. The quoted circumstellar absorption column is ionized, with $N_{\rm W}$ expressed in cm^-2. The last column gives the observed flux between 0.4 and 10.0 keV for each fitting result. The normalization parameter (Norm) of the mekal component is defined as $(10^{-14}/(4~\pi~D^2))\int{n_{\rm e}~n_{\rm H}~{\rm d}V}$ , where D, $n_{\rm e}$ and $n_{\rm H}$ are respectively the distance to the source (in cm), and the electron and hydrogen number densities (in cm^-3). The error bars represent the 1- $\sigma$ confidence interval.
Table 6: Best-fit parameter values for a wabs $_{{\rm ISM}}$ *wind*(mekal+power) model for the combined EPIC-MOS data, EPIC-pn, and the three EPIC spectra together. The ISM absorption component is frozen at 0.58 $\times$ 10²² cm^-2. The local absorption column accounts for the ionization of the wind, with $N_{\rm W}$ expressed in cm^-2. The upper and lower parts of the table refer to the first and second observation respectively. For the power law component, the normalization parameter (Norm₂) corresponds to the photon flux at 1 keV. The error bars represent the 1- $\sigma$ confidence interval.
Table 7: X-ray fluxes and luminosities of HD 168112. The third column gives the absorbed flux, and the fourth one yields the flux corrected for interstellar absorption. Luminosities corrected for interstellar absorption were determined for the two exposures between 0.4 and 10.0 keV and are given in the fifth column. These luminosities were calculated adopting a 2 kpc distance (see Table 4).
Table 8: EPIC-MOS and EPIC-pn count rates obtained for HD 168112 during the two XMM-Newton observations between 0.4 and 10.0 keV. The error bars represent the 1- $\sigma$ confidence interval.
Table 9: Observed fluxes estimated in the case of the model resulting from combined EPIC-MOS data fitted with the two-temperature model, in the case of the warm local absorption model.
Table 10: VLA fluxes and spectral index.
Table 11: Average radial velocities of nine absorption lines in the spectrum of HD 168112 as measured on our SPM and FEROS data. The third column yields the instrumentation used for the observation: echelle spectrograph at San Pedro (SPM), FEROS at the 1.5 m telescope (F1.5) or FEROS at the 2.2 m telescope (F2.2).
Table 12: Differential LTPV photometry of HD 168112. The quoted magnitudes and 1- $\sigma$ dispersions correspond to the difference A 5020 - B 5020 (where A 5020 is the magnitude of HD 168112 and B 5020 that of HD 168135). The first column yields the code of the telescope + instrument configuration (see Manfroid et al. 1991) and the second column indicates the number of data points for each set-up.