All Figures

$\begin{figure} \par {\includegraphics[width=6.9cm,clip]{1444fig1.eps} } \end{figure}$ Figure 1: A randomly chosen set of the normalised disentangled Si III profiles of $\kappa~$ Sco (HJDs 2 449 876-50 658) in the rest frame of the primary centered at 4560 Å. For clarity we have shifted the flux level of each profile with a value 0.04 with respect to the previous one.
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In the text

$\begin{figure} \par {\includegraphics[angle=-90,width=10.8cm,clip]{1444fig2.eps} } {\includegraphics[angle=-90,width=10.8cm,clip]{1444fig3.eps} } \end{figure}$ Figure 2: Top ( bottom): line profile measurements taken on HJD 2 450 742.4691 (HJD 2 450 194.9224). The observed spectrum of the primary shifted with +53.39km s^-1 (-55.34 km s^-1) is given by the full black line and the KOREL disentangled profile in the rest frame of the primary by the dotted line. The gray profile is the observed one from which the disentangled profile of the secondary is subtracted after applying its orbital shift of -57.84 km s^-1 (62.70 km s^-1) and to which a subsequent orbital shift towards the rest frame of the primary +53.39 km s^-1 (-55.34 km s^-1) is applied. The vertical lines indicate the integration boundaries we used to calculate the velocity moments from the Si III profiles centered at 4552.654 Å and 4567.872 Å. At the bottom of each figure the residual disentangled and secondary removed spectra with respect to the observed spectrum are also shown, after an arbitrary shift towards flux level 0.88.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=7cm,clip]{1444fig4.eps... ...ce*{5mm} \includegraphics[angle=-90,width=7cm,clip]{1444fig5.eps} } \end{figure}$ Figure 3: Lomb-Scargle periodogram of the RV ( left) and EW ( right) derived from the disentangled Si III 4552.654 Å profiles of the primary. On top of each panel, the window function, shifted according to the highest peak in the periodogram, is shown.
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In the text

$\begin{figure} \par {\includegraphics[angle=-90,width=11.9cm,clip]{1444fig6.eps} } \end{figure}$ Figure 4: The first three normalised moments (without prewhitening in case of f₁; after prewhitening with f₁ in case of f₂ and f₃) of the Si III 4552.654 Å line of $\kappa~$ Sco, calculated from the disentangled spectra of the primary and folded with the frequencies f₁ ( left), f₂ ( middle) and f₃( right). The dots are the observations, while the full line is a fit for the indicated frequencies with no, one and two harmonics for respectively $\langle v\rangle$ , $\langle v^2\rangle$ and $\langle v^3\rangle$ .
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=7cm,clip]{1444fig7.eps... ...ce*{5mm} \includegraphics[angle=-90,width=7cm,clip]{1444fig8.eps} } \end{figure}$ Figure 5: Lomb-Scargle periodograms of the residuals of the EW ( left) and first velocity moment ( right) of the disentangled Si III 4552.654 Å profiles of the primary after prewhitening with f₁ = 4.99922 c d^-1. The frequencies reported in the literature are indicated by dashed lines: 4.8678 c d^-1, 5.2767 c d^-1 (Lomb & Shobbrook 1975), 0.2809 c d^-1, 2.2498 c d^-1 and 5.6950 c d^-1 (WIRE, Cuypers et al. 2004).
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In the text

$\begin{figure} \par {\includegraphics[angle=-90,width=7.53cm,clip]{1444fig9.eps}... ...\par {\includegraphics[angle=-90,width=8.23cm,clip]{1444fg12.eps} } \end{figure}$ Figure 6: IPS diagrams for f₁, f₂ and f₃ and their first harmonic, calculated from the Si III 4552.654 Å ( left) and 4567.874 Å ( right) line of the disentangled profiles. The top panel shows the average line profile. Each of the three sub-panels shows the distribution of the phase (expressed in $\pi$ radians) and of the amplitude across the line profile. Thick black line: single-sinusoid fit with indicated f; light gray line: triple-sinusoid fit with f₁, f₂ and f₃; thin black line: single-sinusoid fit with 2f. For clarity the phase distribution across the line profile for 2f is plotted with an offset.
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In the text

$\begin{figure} \par {\includegraphics[width=5.2cm,clip]{1444fg13.eps} } \end{figure}$ Figure 7: Mean profile and phase and amplitude diagrams for f₁ centered at 4552.654 Å. The solid black line represents the diagnostics derived from the disentangled spectra. The other lines are derived from theoretically calculated profiles, with different $(\ell ,m)$ values: (1,-1) (dark gray solid line); (2,-1) (light gray solid line); (2,-2) (dark gray dashed-dotted line). The phases are given in $\pi$ radians.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{1444fg14.eps}\hspace*{2mm} \includegraphics[width=6.9cm,clip]{1444fg15.eps}\end{figure}$ Figure 8: Phase distribution across the 4552.654 Å profile for sinusoidal fits with f₂ ( left) and f₃ ( right). The solid black line represents the diagnostics derived from the disentangled spectra. The other lines are derived from theoretically calculated profiles, with different $(\ell ,m)$ values as indicated. The phases are expressed in terms of $\pi$ radians.
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In the text

$\begin{figure} \par\includegraphics[width=5.04cm,clip]{1444fg16.eps}\end{figure}$ Figure 9: The first three velocity moments (dots) computed from 40 averaged spectra in the region near Si III 4552.654 Å over the pulsation cycle of f₁ = 4.99922 c d^-1. The crossed and dashed lines correspond respectively to theoretical moments computed for the first two best solutions of the upper part of Table 3. The full line corresponds to the best solution for a model with f₁ and 2f₁ (indicated in bold in Table 4).
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In the text

$\begin{figure} \par {\includegraphics[width=7.4cm,clip]{1444fg17.eps} } \end{figure}$ Figure 10: The Si distribution on the surface of $\kappa~$ Sco obtained with INVERS11 from the Si III 4552.654 Å line for $T_{\rm eff} = 25~000$ K, $\log g = 3.8$ , $v\sin~i= 100$ km s^-1 and $i=70^{\circ }$ . a) is the mercator projection of the abundance distribution and comprises contour lines around regions of equal abundance. b) shows the mapped stellar surface in four rotational phases (0.0, 0.25, 0.5, 0.75). Below each phase, values for the mean abundance averaged over the visible part can be found. Dark colour means high, bright colour means low abundance.
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In the text

$\begin{figure} \par {\includegraphics[angle=-90,width=8.3cm,clip]{1444fg18.eps} } \end{figure}$ Figure 11: A phase plot of the first two moments of the disentangled Si III 4552.654 line profiles folded with $f_{\rm super} = 0.29407$ c d^-1.
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In the text

$\begin{figure} \par {\includegraphics[width=6.9cm,clip]{1444fig1.eps} } \end{figure}$	Figure 1: A randomly chosen set of the normalised disentangled Si III profiles of $\kappa~$ Sco (HJDs 2 449 876-50 658) in the rest frame of the primary centered at 4560 Å. For clarity we have shifted the flux level of each profile with a value 0.04 with respect to the previous one.
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$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=7cm,clip]{1444fig4.eps... ...ce*{5mm} \includegraphics[angle=-90,width=7cm,clip]{1444fig5.eps} } \end{figure}$	Figure 3: Lomb-Scargle periodogram of the RV ( left) and EW ( right) derived from the disentangled Si III 4552.654 Å profiles of the primary. On top of each panel, the window function, shifted according to the highest peak in the periodogram, is shown.
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{1444fg14.eps}\hspace*{2mm} \includegraphics[width=6.9cm,clip]{1444fg15.eps}\end{figure}$	Figure 8: Phase distribution across the 4552.654 Å profile for sinusoidal fits with f₂ ( left) and f₃ ( right). The solid black line represents the diagnostics derived from the disentangled spectra. The other lines are derived from theoretically calculated profiles, with different $(\ell ,m)$ values as indicated. The phases are expressed in terms of $\pi$ radians.
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$\begin{figure} \par {\includegraphics[angle=-90,width=8.3cm,clip]{1444fg18.eps} } \end{figure}$	Figure 11: A phase plot of the first two moments of the disentangled Si III 4552.654 line profiles folded with $f_{\rm super} = 0.29407$ c d^-1.
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