All Figures

	Figure 1: Histogram showing the number of stars N showing LPV as a function of the projected rotation velocity. It can be noticed that LPV are easier to detect for stars having low values.
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In the text

	Figure 2: Lower part: bi-dimensional plot of the temporal evolution (on an arbitrary scale) of the residual spectra for the star HD 277. Upper part: from bottom to top are successively represented the mean spectrum, the individual residual spectra and the dispersion around the mean residual (see text).
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In the text

	Figure 3: Fit of the orbit of HD 62454. Empty symbols represent the companion velocities. The values of Kaye et al. (1999) are represented as stars. The dot-dash line represents the heliocentric velocity of the system.
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In the text

	Figure 4: Fit of the orbit of HD 70645. The dot-dash line represents the heliocentric velocity of the system.
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In the text

	Figure 5: Fit of the orbit of HD 80731. The dot-dash line represents the heliocentric velocity of the system.
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In the text

	Figure 6: Fit of the orbit of HD 100215 with a fixed null eccentricity (see text). The dot-dash line represents the heliocentric velocity of the system.
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In the text

	Figure 7: Upper panel: a region of the composite spectrum of HD 108100 showing both broad and narrow components. Lower panel: zoom on the narrow component showing LPV as a function of the observation date written on the right side of the graph. The dashed line represents the average spectrum.
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In the text

	Figure 8: Fit of the orbit of HD 221866. Empty symbols represent the companion velocities. The dot-dash line represents the heliocentric velocity of the system.
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In the text