Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0216fig1.eps} \end{figure}$ Figure 1: Panel a): the cross-correlation of the spectrum of HD 11413 taken on Nov. 16th, 1992 with a computed spectrum ( $T_{\rm eff }$ = 7950 K, $\log~g = 3.84$ , $v\sin i=5$ ${\rm km~ s^{-1}}$ ) over the range 420-450 nm. In both spectra H $_\gamma$ has been artificially suppressed (see text). Panel b): the cross-correlation of the spectrum of HD 11413 taken on Sep. 9th, 1993 with the same computed spectrum as used in panel a); also the spectral range is the same and H $_\gamma$ has been likewise suppressed. Panel c): the cross-correlation of the spectrum of Sirius; with a ( $T_{\rm eff }$ = 9830 K, $\log~g = 4.07$ , $v\sin i=5$ ${\rm km~ s^{-1}}$ ) suitable synthetic spectrum, the spectral range is the same and H $_\gamma$ has been suppressed as for HD 11413.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0216fig2.eps} \end{figure}$ Figure 2: The H $_\gamma$ profile of HD 79108 compared with a spectrum computed with $T_{\rm eff }$ = 9830 K, $\log~g = 4.07$ and $v~\sin i$ = 160 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0216fig3.eps} \end{figure}$ Figure 3: The cross-correlation of the spectrum of HD 79108 with the synthetic spectrum computed with $T_{\rm eff }$ = 9830 K, $\log~g = 4.07$ and $v\sin i=5$ ${\rm km~ s^{-1}}$ and with H $_\gamma$ suppressed (see text).
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{0216fig4.eps} \end{figure}$ Figure 4: The observed spectrum of HD 141851 (solid line) superimposed on the combined spectrum (short dashed line) obtained by combining two synthetic spectra as described in the text ( upper panel). In the lower panel the same observed spectrum is compared with two synthetic spectra computed with solar abundances and parameters $T_{\rm eff }$ and log g derived from the photometry: 8080 K, 3.86 (long dashed line) and 8258 K, 3.69 (dotted line); the two computed spectra are almost identical as can be seen in the inset.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0216fig5.eps} \end{figure}$ Figure 5: The observed Mg I triplet of HD 141851 compared with two synthetic spectra: that computed with MD parameters (dotted line) and that obtained from the combination described in the text (long dashed line).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{0216fig6.eps} \end{figure}$ Figure 6: The UV flux (and associated error bars) of HD 196821 measured by TD1 compared to the theoretical flux (dash-dot line) computed with solar abundances.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0216fig7.eps} \end{figure}$ Figure 7: The OI 777.4 triplet of HD 196821 compared with the theoretical spectrum computed by assuming solar abundances.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0216fig8.eps} \end{figure}$ Figure 8: The cross-correlations of the three spectra of HD 210111 (taken on Sep. 7th, 1993 (solid line), Sep. 18th, 1994 (long-dashed line) and on Nov. 14th, 1994 (dotted line)) with a computed spectrum ( $T_{\rm eff }$ = 7500 K, $\log~g = 4.0~v\sin i=5$ ${\rm km~ s^{-1}}$ ) over the range 420-450 nm. Both in the synthetic and observed spectra the H $_\gamma$ has been artificially suppressed (see text).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{0216fig9.eps} \end{figure}$ Figure 9: The UV flux of HD 210111 and associated error bars (thick lines) compared to the theoretical flux ( $T_{\rm eff }$ = 7500 K, $\log~g = 4.00$ abundances 1 dex lower than solar) (dash-dot line) and solar abundances (dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0216fig10.eps} \end{figure}$ Figure 10: The OI 777.4 profile of HD 149303 compared with that computed in the hypothesis that the star is a single object rotating at 275 ${\rm km~ s^{-1}}$ ; the fictious fit has been obtained by adopting the MD parameters, but increasing the oxygen abundance by 1 dex to simulate the NLTE effect on this triplet.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0216fig11.eps} \end{figure}$ Figure 11: The NaI doublet appears as a single very broad feature in the spectrum of HD 149303 (thick line); the synthetic spectrum has been computed by assuming that the star is a single object rotating at 275 ${\rm km~ s^{-1}}$ . The convolution of such broad lines produces the fictious central peak.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0216fig2.eps} \end{figure}$	Figure 2: The H $_\gamma$ profile of HD 79108 compared with a spectrum computed with $T_{\rm eff }$ = 9830 K, $\log~g = 4.07$ and $v~\sin i$ = 160 km s^-1.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0216fig3.eps} \end{figure}$	Figure 3: The cross-correlation of the spectrum of HD 79108 with the synthetic spectrum computed with $T_{\rm eff }$ = 9830 K, $\log~g = 4.07$ and $v\sin i=5$ ${\rm km~ s^{-1}}$ and with H $_\gamma$ suppressed (see text).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0216fig5.eps} \end{figure}$	Figure 5: The observed Mg I triplet of HD 141851 compared with two synthetic spectra: that computed with MD parameters (dotted line) and that obtained from the combination described in the text (long dashed line).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{0216fig6.eps} \end{figure}$	Figure 6: The UV flux (and associated error bars) of HD 196821 measured by TD1 compared to the theoretical flux (dash-dot line) computed with solar abundances.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0216fig7.eps} \end{figure}$	Figure 7: The OI 777.4 triplet of HD 196821 compared with the theoretical spectrum computed by assuming solar abundances.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{0216fig9.eps} \end{figure}$	Figure 9: The UV flux of HD 210111 and associated error bars (thick lines) compared to the theoretical flux ( $T_{\rm eff }$ = 7500 K, $\log~g = 4.00$ abundances 1 dex lower than solar) (dash-dot line) and solar abundances (dashed line).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0216fig10.eps} \end{figure}$	Figure 10: The OI 777.4 profile of HD 149303 compared with that computed in the hypothesis that the star is a single object rotating at 275 ${\rm km~ s^{-1}}$ ; the fictious fit has been obtained by adopting the MD parameters, but increasing the oxygen abundance by 1 dex to simulate the NLTE effect on this triplet.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0216fig11.eps} \end{figure}$	Figure 11: The NaI doublet appears as a single very broad feature in the spectrum of HD 149303 (thick line); the synthetic spectrum has been computed by assuming that the star is a single object rotating at 275 ${\rm km~ s^{-1}}$ . The convolution of such broad lines produces the fictious central peak.
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