All Figures

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{0627f5.eps}\\ \includegraphics[width=6.5cm,clip]{0627f1a.eps} \end{figure}$ Figure 1: Values of minimum $\chi ^2$ for each model stellar atmosphere for fitting the interferometric data of $\psi$ Phe as a function of (top) $\theta _{\rm {LD}}$ and (bottom) $\theta _{\rm Ross}$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{0627f2a.eps}\par\includegraphics[width=6.5cm,clip]{0627f2b.eps} \end{figure}$ Figure 2: (Top) The visibilities calculated for three SATLAS models and the interferometric data for $\psi$ Phe. (Bottom) Close-up of the second lobe of the visibility amplitude. The dotted line refers to the model stellar atmosphere for $L = 1580~L_\odot$ , $M = 1.6~M_\odot$ , and $R = 60~R_\odot$ , the dot-dashed line represents a model with $L = 980~L_\odot$ , $M = 1.2~M_\odot$ , and $R = 80~R_\odot$ , and the dashed line is for $L = 630~L_\odot$ , $M = 0.6~M_\odot$ , and $R = 120~R_\odot$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{0627f3.eps} \end{figure}$ Figure 3: The visibilities calculated for three SATLAS models and the interferometric data for $\gamma$ Sge. The dotted line refers to the model stellar atmosphere for $L = 700~L_\odot$ , $M = 1.9~M_\odot$ , and $R = 30~R_\odot$ , the dot-dashed line represents a model with $L = 550~L_\odot$ , $M = 1.4~M_\odot$ , and $R = 50~R_\odot$ , and the dashed line is for $L = 400~L_\odot$ , $M = 1.0~M_\odot$ , and $R = 70~R_\odot$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{0627f4a.eps}\par\includegraphics[width=6.7cm,clip]{0627f4b.eps} \end{figure}$ Figure 4: (Top) The visibilities calculated for three SATLAS models and the interferometric data for $\alpha$ Cet. (Bottom) Close-up of the second lobe of the visibility amplitude. The dotted line refers to the model stellar atmosphere for $L = 2000~L_\odot$ , $M = 3.0~M_\odot$ , and $R = 60~R_\odot$ , the dot-dashed line represents a model with $L =1500~L_\odot$ , $M = 2.3~M_\odot$ , and $R = 80~R_\odot$ , and the dashed line is for $L = 1000~L_\odot$ , $M = 1.5~M_\odot$ , and $R = 100~R_\odot$ .
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0627f1b.eps} \end{figure}$ Figure 5: The best-fit effective temperature as a function of Rossland angular diameter found by fitting spectrophotometry (+'s) and interferometry ( $\times$ 's) for $\psi$ Phe.
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In the text

$\begin{figure} \par\includegraphics[]{0627f6.eps} \end{figure}$ Figure 6: Comparison of the derived effective temperatures and luminosities of the three stars relative the derived parameters from previous analyses. The lines are evolutionary tracks from Girardi et al. (2000), the points given by $\times$ 's are the predicted effective temperatures and luminosities found using the SATLAS models and the plusses are the values found using PHOENIX models.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{0627f5.eps}\\ \includegraphics[width=6.5cm,clip]{0627f1a.eps} \end{figure}$	Figure 1: Values of minimum $\chi ^2$ for each model stellar atmosphere for fitting the interferometric data of $\psi$ Phe as a function of (top) $\theta _{\rm {LD}}$ and (bottom) $\theta _{\rm Ross}$ .
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$\begin{figure} \par\includegraphics[width=7cm,clip]{0627f1b.eps} \end{figure}$	Figure 5: The best-fit effective temperature as a function of Rossland angular diameter found by fitting spectrophotometry (+'s) and interferometry ( $\times$ 's) for $\psi$ Phe.
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$\begin{figure} \par\includegraphics[]{0627f6.eps} \end{figure}$	Figure 6: Comparison of the derived effective temperatures and luminosities of the three stars relative the derived parameters from previous analyses. The lines are evolutionary tracks from Girardi et al. (2000), the points given by $\times$ 's are the predicted effective temperatures and luminosities found using the SATLAS models and the plusses are the values found using PHOENIX models.
Open with DEXTER