All Tables

Table 1: Relevant parameters of the HD 159176 binary system adopted throughout this paper unless otherwise stated. The numbers are taken from Pachoulakis (1996, P96) and Diplas & Savage (1994, DS).
Table 2: Performed and useful exposure times for all XMM-Newton instruments. The useful RGS exposure time is considerably reduced due to a strong flare of soft protons. The fourth column yields the background-corrected count rate for the source, between 0.4 and 10 keV for EPIC, and between 0.3 and 2.5 keV for RGS. In the case of the RGS instruments, only exposure 0001730201 is considered. The error bars on the count rate represent the $\pm$ 1 $\sigma$ standard deviation.
Table 3: Fitted model parameters for EPIC spectra of HD 159176. The upper part of the table concerns the wabs $_{\rm ISM}$ *wabs $_{\rm WIND}$ *(mekal + mekal) model, whilst the bottom part summarizes the results for the wabs $_{\rm ISM}$ *wabs $_{\rm WIND}$ *(mekal + power) model. The $N_{\rm H}$ given in the table refers to the circumstellar (i.e. wind) column assumed to be neutral. The interstellar column density is frozen at $0.17\times 10^{22}$ cm^-2 for all models. The Norm parameter 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 densities (in cm^-3), whereas for the power law this parameter corresponds to the photon flux at 1 keV. The error bars represent the 1 $\sigma$ confidence interval.
Table 4: Fitted model parameters for the EPIC-pn spectrum of HD 159176 for two different background estimation techniques. The adopted model is wabs $_{\rm ISM}$ *wabs $_{\rm WIND}$ *(mekal + mekal + power). The column densities given in the table refer to the circumstellar material. The interstellar column density is frozen at $0.17\times 10^{22}$ cm^-2. The error bars represent the 1 $\sigma$ confidence interval.
Table 5: X-ray luminosities and luminosity ratios from EINSTEIN, ROSAT and XMM observations of HD 159176. Luminosities are calculated for a 1.5 kpc distance. The Obs. CR column gives the count rates from Chlebowski et al. (1989) and Berghöfer et al. (1996) respectively for EINSTEIN and ROSAT, as well as our value for EPIC-pn. The Th. CR column provides the theoretical count rates calculated on the basis of the individual instrument response matrices for the 3 component model of Table 4 (see text).
Table 6: Model parameters for a two-temperature mekal model fitted to the RGS1 and RGS2 spectra of HD 159176, to the three EPIC spectra considered simultaneously and finally to all the XMM data taken together. The adopted model is wabs $_{\rm ISM}$ *wabs $_{\rm WIND}$ *(mekal + mekal). The column density given in the Table refers to the local (i.e. circumstellar) absorption. The interstellar column density is frozen at $0.17\times 10^{22}$ cm^-2. The error bars represent the 1 $\sigma$ confidence interval.