Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=13cm,clip]{1227orb.eps} \end{figure}$ Figure 1: Orbital fit based on 2 years of bi-site spectroscopic observations of HD104237. HJD = 2 450 000 + $\Delta$ HJD. The top panel corresponds to the SAAO observations in April 1999, the middle panel to the bi-site campaign in April 2000 (SAAO and Mt. Stromlo), the lower panel to the additional data set obtained at SAAO in May 2000.The dispersion in radial velocity around the adjusted orbital fit shows the intrinsic stellar oscillations. It is striking to observe the difference in oscillation amplitude between the 1999 and the 2000 data sets.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{1227evol.eps}\end{figure}$ Figure 2: Location of the HD 104237 primary (A) and spectroscopic secondary component HD 104237 b (location B) in the HR diagram. The luminosity and effective temperature pairs reported in van den Ancker et al. (1998) (VA) and Grady et al. (2004) (GR) are shown in the diagram, including error bars. Evolutionary tracks (1.5, 2.0 and 2.5 $M_\odot$ ) and isochrones are by Palla & Stahler (2001). We produced small parts of a 2.25 and 1.75 $M_\odot$ track by roughly interpolating Palla & Stahler's evolutionary tracks. The Marconi & Palla (1998) instability strip is represented by the shaded area.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1227bin.eps}\end{figure}$ Figure 3: LSD profiles obtained before and after the periastron at $\Delta _{{\rm HJD}}$ = 1289.4032 (continuous) and 1290.4893 (dot-dashed). The spectroscopic binary movement during one day is easily observed.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1227w99.eps} \end{figure}$ Figure 4: Spectral window of the SAAO 1999 data set.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1227wtot.eps} \end{figure}$ Figure 5: Spectral window of the total 2000 data set.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1227w00t.eps} \end{figure}$ Figure 6: Spectral window of the SAAO 2000 data set only.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{1227aF6.eps} \end{figure}$ Figure 7: f₆ from the SAAO 1999 data set. Overplotted (dotted) is the periodogram corresponding to an artificial radial velocity curve with the frequency, amplitude and phase of this frequency calculated at the SAAO 1999 time grid, i.e. a convolution of the window function with the results of the frequency analysis for the 6th frequency.
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In the text

$\begin{figure} \par\includegraphics[width=12.6cm,clip]{1227p99.eps} \end{figure}$ Figure 8: Periodograms of the radial velocity oscillations in HD 104237 observed at SAAO in 1999. The sequence from top to bottom shows the change of the amplitude periodogram pre-whitened by f₁, f₂, f₃, f₄ and f₅, respectively. The 99.9% confidence level is plotted (continuous), as well as the 99% level (dotted) and the 90% level (dashed). These levels correspond to a 4.0, 3.6 and 3.2-mean-amplitude-level calculated on 10 d^-1 (cycles/day) sliding windows before prewhitening with the tested frequency (see text).
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In the text

$\begin{figure} \par\includegraphics[width=12.6cm,clip]{1227p99r.eps} \end{figure}$ Figure 9: Periodograms of the radial velocity oscillations in HD 104237 observed in 1999, showing the frequencies f₇, f₈, and the residual. Figure 8, continued.
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In the text

$\begin{figure} \par\includegraphics[width=12.6cm,clip]{1227ptot.eps} \end{figure}$ Figure 10: Periodograms of the radial velocity oscillations in HD 104237 observed in 2000, including the April/May 2000 bi-site campaign. The sequence from top to bottom shows the change of the amplitude periodogram pre-whitened by f₁, f₂, f₃, f₄ and f₅, respectively. The 99.9% confidence level is plotted (continuous), as well as the 99% level (dotted) and the 90% level (dashed). These levels correspond to a 4.0, 3.6 and 3.2-mean-amplitude-level calculated on 10 cycles/day sliding windows before prewhitening with the tested frequency (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1227aF50.eps} \end{figure}$ Figure 11: f₅ from the global 2000 data set. Overplotted (dotted) is the periodogram corresponding to an artificial radial velocity curve with the frequency, amplitude and phase of this frequency calculated on the time grid for the year 2000, i.e. a convolution of the window function with the results of the frequency analysis for the 6th frequency.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1227comp.eps} \end{figure}$ Figure 12: f₆ from the 1999 data set (continuous line) versus f₅ from the global 2000 data set (dotted). Most likely the two frequencies are identical.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{1227ts99.eps} \end{figure}$ Figure 13: Pulsations of HD 104237 during the SAAO 1999 run. Superimposed (continuous line) is the result of the frequency analysis (Table 4). Time is expressed in HJD = 2 450 000 + $\Delta$ HJD.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{1227ts0a.eps} \end{figure}$ Figure 14: Pulsations of HD 104237 during the SAAO April 2000 run. Superimposed (continuous line) is the result of the frequency analysis (Table 5), based on all observations obtained in 2000, including the Mt. Stromlo April 2000 observations. Time is expressed in HJD = 2 450 000 + $\Delta$ HJD.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{1227ts0b.eps} \end{figure}$ Figure 15: Pulsations of HD 104237 during the SAAO May 2000 run. Superimposed (continuous line) is the result of the frequency analysis (Table 5), based on all observations obtained in 2000, including the April 2000 observations. Time is expressed in HJD = 2 450 000 + $\Delta$ HJD.
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In the text

$\begin{figure} \par\includegraphics[width=16.15cm,clip]{1227tsms.eps} \end{figure}$ Figure 16: Pulsations of HD 104237 during the Mt. Stromlo 2000 run (filled circles), and SAAO 2000 run (diamonds). Superimposed (continuous line) is the result of the global frequency analysis (Table 5), based on all observations obtained in 2000. Time is expressed in HJD = 2 450 000 + $\Delta$ HJD.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1227sec.eps} \end{figure}$ Figure 17: Amplitude spectrum of the secondary component HD 104237 b, based on SAAO 2000 observations of April 11th and 12th. The continuous envelope indicates the 99.9% probability level (99.0% for the dashed line), the dot-dashed line correspond to an artificial profile with parameters of the main frequency and window function distribution. Probability levels have been calculated based on a sliding 20 cd^-1 window.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1227bin.eps}\end{figure}$	Figure 3: LSD profiles obtained before and after the periastron at $\Delta _{{\rm HJD}}$ = 1289.4032 (continuous) and 1290.4893 (dot-dashed). The spectroscopic binary movement during one day is easily observed.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1227w99.eps} \end{figure}$	Figure 4: Spectral window of the SAAO 1999 data set.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1227wtot.eps} \end{figure}$	Figure 5: Spectral window of the total 2000 data set.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1227w00t.eps} \end{figure}$	Figure 6: Spectral window of the SAAO 2000 data set only.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{1227aF6.eps} \end{figure}$	Figure 7: f₆ from the SAAO 1999 data set. Overplotted (dotted) is the periodogram corresponding to an artificial radial velocity curve with the frequency, amplitude and phase of this frequency calculated at the SAAO 1999 time grid, i.e. a convolution of the window function with the results of the frequency analysis for the 6th frequency.
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$\begin{figure} \par\includegraphics[width=12.6cm,clip]{1227p99r.eps} \end{figure}$	Figure 9: Periodograms of the radial velocity oscillations in HD 104237 observed in 1999, showing the frequencies f₇, f₈, and the residual. Figure 8, continued.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1227aF50.eps} \end{figure}$	Figure 11: f₅ from the global 2000 data set. Overplotted (dotted) is the periodogram corresponding to an artificial radial velocity curve with the frequency, amplitude and phase of this frequency calculated on the time grid for the year 2000, i.e. a convolution of the window function with the results of the frequency analysis for the 6th frequency.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1227comp.eps} \end{figure}$	Figure 12: f₆ from the 1999 data set (continuous line) versus f₅ from the global 2000 data set (dotted). Most likely the two frequencies are identical.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{1227ts99.eps} \end{figure}$	Figure 13: Pulsations of HD 104237 during the SAAO 1999 run. Superimposed (continuous line) is the result of the frequency analysis (Table 4). Time is expressed in HJD = 2 450 000 + $\Delta$ HJD.
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$\begin{figure} \par\includegraphics[width=16cm,clip]{1227ts0a.eps} \end{figure}$	Figure 14: Pulsations of HD 104237 during the SAAO April 2000 run. Superimposed (continuous line) is the result of the frequency analysis (Table 5), based on all observations obtained in 2000, including the Mt. Stromlo April 2000 observations. Time is expressed in HJD = 2 450 000 + $\Delta$ HJD.
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{1227ts0b.eps} \end{figure}$	Figure 15: Pulsations of HD 104237 during the SAAO May 2000 run. Superimposed (continuous line) is the result of the frequency analysis (Table 5), based on all observations obtained in 2000, including the April 2000 observations. Time is expressed in HJD = 2 450 000 + $\Delta$ HJD.
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$\begin{figure} \par\includegraphics[width=16.15cm,clip]{1227tsms.eps} \end{figure}$	Figure 16: Pulsations of HD 104237 during the Mt. Stromlo 2000 run (filled circles), and SAAO 2000 run (diamonds). Superimposed (continuous line) is the result of the global frequency analysis (Table 5), based on all observations obtained in 2000. Time is expressed in HJD = 2 450 000 + $\Delta$ HJD.
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