All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{9992fg01.ps}\end{figure}$ Figure 1: Colour-magnitude ((b-y)₀ versus absolute magnitude M_v) diagram indicating the position of HD 49434 (star). The (b-y)₀ and M_v values of HD 49434 (an error bar is given in the left bottom corner) are taken from Hauck & Mermilliod (1998) and from the HIPPARCOS satellite data, respectively. Dashed and solid tracks indicate evolutionary tracks for the overshooting extension distances $d_{\rm over}$ = 0.1 and 0.2, respectively (see Claret 1995, for details). The ZAMS and the borders of the $\delta$ Sct (longer black lines) and $\gamma$ Dor (shorter gray lines) instability strips are indicated by solid lines.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=16.3cm,clip]{9992fg02.ps}\end{figure}$ Figure 2: Ground-based light curves of HD 49434. The top panel shows all relative KON Johnson V (triangles), SNO Strömgren y (open diamonds) and SPMO Strömgren y (stars) magnitudes. The bottom left panel zooms in on SNO and SPMO data obtained in November 2006. The bottom right panel shows the light curves obtained during the nights of 26 and 28 November 2006, and 1 December 2006 at SPMO. We plotted the individual nights with an offset of 2.1 mmag for clarity. On top of the figure we indicated the time span of the spectroscopic ground-based observations described in this paper (see Sect. 2.2) with a black line, while the continuous CoRoT observations are given in gray.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{9992fg03.ps}\end{figure}$ Figure 3: SCARGLE periodograms calculated from the Strömgren v data (SPMO and SNO) of HD 49434. The top panel indicates the associated spectral window, followed by the periodogram of the observed light variations, and those calculated after subsequent removal of the frequencies 1.73480 d^-1 and 0.23427 d^-1. These two frequencies are indicated by dashed gray lines. The amplitudes are expressed in mmag.
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In the text

$\begin{figure} \par\includegraphics[width=3.7cm,clip]{9992fg04.ps}\hspace*{3mm} \includegraphics[width=3.7cm,clip]{9992fg05.ps}\end{figure}$ Figure 4: Left: a selection of LSD profiles calculated from the HERCULES, SOPHIE, FEROS and FOCES spectra of HD 49434. Right: a selection of SOPHIE and FEROS spectra of HD 49434, centred on the Ti II 4501.273 Å and Fe II 4508.288 Å profiles. The spectra are offset for clarity.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9992fg06.ps}\end{figure}$ Figure 5: Lower part: Bi-dimensional plot of the temporal evolution (on an arbitrary scale) of the residual FEROS, SOPHIE and HERCULES LSD profiles of the star HD 49434. Upper part: from bottom to top are successively represented the mean spectrum, the individual residual spectra and the dispersion $\sigma$ around the mean residual.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{9992fg07.ps}\end{figure}$ Figure 6: Summed power over each pixel of the LSD profiles of the Fourier power spectra calculated from the combined dataset of FEROS, SOPHIE and HERCULES LSD spectra, which is a measure for the amplitude of the variability. The top panel gives the power spectra calculated from the original profiles. The middle panel shows the power spectra after removal of the dominant frequency (9.302 d^-1). At the bottom the residual power spectra are shown after prewhitening the six frequencies 9.3070 d^-1, 5.3311 d^-1, 12.0332 d^-1, 9.1527 d^-1, 6.6841 d^-1 and 1.483 d^-1, which are indicated by the light grey dotted lines.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{9992fg08.ps}\end{figure}$ Figure 7: First normalised moments (RVs) calculated from the FEROS (stars), SOPHIE (bullets), HERCULES (open circles) and FOCES (triangles) spectra of HD 49434. Top panel: $\langle v\rangle$ calculated from the LSD profiles after correction for the small velocity shifts between different datasets resulting from systematical instrumental differences. Bottom panel: average value of $\langle v\rangle$ calculated from the Ti II and Fe II profiles near 4500 Å of the FEROS and SOPHIE spectra. We used the same relative scale in y-axis in top and bottom panel to illustrate the scatter difference between the RVs measured from the LSD profiles and from the individual profiles.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{9992fg09.ps}\end{figure}$ Figure 8: SCARGLE periodograms calculated from the first moment of the combined FEROS, SOPHIE, and HERCULES LSD profiles. The top panel indicates the associated spectral window. We then plot, from top to bottom: the periodogram of the first moment, the one after prewhitening with 1.2732 d^-1, and the one after additional removal of 2.666 d^-1, 0.234 d^-1, 1.489 d^-1 and 5.583 d^-1. The listed frequencies are indicated by light grey lines. The amplitudes are expressed in km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{9992fg10.ps}\end{figure}$ Figure 9: IPS diagrams calculated from the FEROS, SOPHIE and HERCULES LSD profiles for the frequencies 1.4831 d^-1, 5.3311 d^-1, 9.3070 d^-1, 7.6841 (6.6841) d^-1, 10.1527 (9.1527) d^-1, and 12.0332 (11.0332) d^-1. From top to bottom: average line profile, phase and amplitude distribution across the line profile. Black and gray lines indicate phase and amplitude of a frequency and its harmonic, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9992fg11.ps}\end{figure}$ Figure 10: Element abundances of HD 49434 derived in this paper (red bullets) compared to the solar values (Grevesse & Sauval 1998, $\odot$ ), and the values obtained for HD 49434 by Bruntt et al. (2002, blue squares), Bruntt et al. (2004, black diamonds) and Gillon & Magain (2006, green crosses).
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In the text

$\begin{figure} \par\includegraphics[width=3.7cm,clip]{9992fg04.ps}\hspace*{3mm} \includegraphics[width=3.7cm,clip]{9992fg05.ps}\end{figure}$	Figure 4: Left: a selection of LSD profiles calculated from the HERCULES, SOPHIE, FEROS and FOCES spectra of HD 49434. Right: a selection of SOPHIE and FEROS spectra of HD 49434, centred on the Ti II 4501.273 Å and Fe II 4508.288 Å profiles. The spectra are offset for clarity.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9992fg06.ps}\end{figure}$	Figure 5: Lower part: Bi-dimensional plot of the temporal evolution (on an arbitrary scale) of the residual FEROS, SOPHIE and HERCULES LSD profiles of the star HD 49434. Upper part: from bottom to top are successively represented the mean spectrum, the individual residual spectra and the dispersion $\sigma$ around the mean residual.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9992fg11.ps}\end{figure}$	Figure 10: Element abundances of HD 49434 derived in this paper (red bullets) compared to the solar values (Grevesse & Sauval 1998, $\odot$ ), and the values obtained for HD 49434 by Bruntt et al. (2002, blue squares), Bruntt et al. (2004, black diamonds) and Gillon & Magain (2006, green crosses).
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