All Figures

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{5618f1.eps}\end{figure}$ Figure 1: Two typical line profiles corresponding to high S/N FEROS spectra of WR 25. The emission line is N IV $\lambda$ 4058 and is shown in the heliocentric rest frame. One (plain line) was observed on HJD 2 452 383.507 (corresponding to $\phi =0.78$ , see Table 3) and is exhibiting a RV of -48 km s^-1; the other was observed on HJD 2 453 133.605 ( $\phi =0.39$ ) corresponding to a velocity of -10 km s^-1. The main change between the two spectra is a shift in RV.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{5618f2.eps}\end{figure}$ Figure 2: Amplitude spectrum (square root of the power spectrum) as a function of the frequency expressed in d^-1 and corresponding to the analysis of the HRS data set. From 0.04 d^-1 to 0.5 d^-1, no peak exceeds 13 km s^-1. The adopted main frequency is marked by a filled circle and the expected positions of the main aliases of this frequency are marked with open circles.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{5618f3.eps}\end{figure}$ Figure 3: Run of the Marraco & Muzzio (1980) statistic as a function of the frequency expressed in d^-1 and corresponding to the analysis of the HRS data set. The main dips are seen at $\nu = 0.0012$ d^-1, $\nu = 0.0016$ d^-1, $\nu = 0.0024$ d^-1 and $\nu = 0.0048$ d^-1; the first three are subharmonics of $\nu = 0.0048$ d^-1 and are a well-known artifact of this kind of method. Other dips are visible at $\nu = 0.0082$ d^-1, $\nu = 0.0100$ d^-1, $\nu = 0.0302$ d^-1 and $\nu = 0.0329$ d^-1. The last two are also aliases of the $\nu = 0.0048$ d^-1 dip. The cited frequencies are marked as in Fig. 2.
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In the text

$\begin{figure}\par\includegraphics[width=8.6cm,clip]{5618f4.eps}\end{figure}$ Figure 4: Observed radial velocities (along with the fitted models) corresponding to the N IV $\lambda$ 4058 emission line in the spectra of WR 25. The data are phased according to the ephemeris as given in Table 3; phase 0.0 corresponds to periastron. The different panels illustrate different analyzed data sets. Top: our HRS data only (filled circles). Middle top: HRS+MRS+LRS data; open triangles represent the RVs in the MRS set, and squares the LRS ones. Middle bottom: all + published data; crosses are the RVs from Conti et al. (1979), Moffat (1978), and Hamann et al. (1995). In each plot, the solid curve represents the relevant orbital solution as given in Table 3. Bottom: radial velocities of the interstellar Ca II K absorption feature measured on our spectra.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{5618f2.eps}\end{figure}$	Figure 2: Amplitude spectrum (square root of the power spectrum) as a function of the frequency expressed in d^-1 and corresponding to the analysis of the HRS data set. From 0.04 d^-1 to 0.5 d^-1, no peak exceeds 13 km s^-1. The adopted main frequency is marked by a filled circle and the expected positions of the main aliases of this frequency are marked with open circles.
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