All Figures

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{5316fig1a.eps}\hspace*{1.5... ...space*{1.5cm} \includegraphics[width=7.1cm,clip]{5316fig1d.eps}\par \end{figure}$ Figure 1: Model fits ( thick curves) to the hydrogen and helium lines ( thin curves) available in the 4000-4950 Å spectral range in our time-averaged spectrum RS6 ( upper left panel), PB6 ( upper right panel), BG9 ( lower left panel), and MMT1 ( lower right panel).
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{5316fig2.eps} \end{figure}$ Figure 2: Model fits ( dotted curves) to the He I 4471 line ( solid curves) in our MMT spectrum of PG 1325+101 assuming various values of the projected rotational velocity Vsin i.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8.2cm]{5316fig3a.eps}\hspace{4mm} \includegraphics[width=8.2cm]{5316fig3b.eps} }\end{figure}$ Figure 3: Left panel: slice of the S²-function (in logarithmic units) along the $\log g{-}T_{\rm eff}$ plane at fixed parameters M_* and $\log q(H)$ , set to their optimal values found from the best-fit model solution ( M_*=0.4988 $M_{\odot }$ and $\log q(H)=-4.2747$ ). The black dot-dot-dashed-line, dashed-line, dot-dashed-line, and dotted-line rectangles represent the various spectroscopic estimates and their uncertainties for the atmospheric parameters of PG 1325+101. They correspond to the MMT1, BG9, PB6, and Telting & Østensen (2004) measurements, respectively. The mean values derived from these measurements appear as the black solid-line rectangle. The red dotted-line rectangle shows the estimated error box associated with our asteroseismic determination of the parameters $\log g$ and $T_{{\rm eff}}$ . The red cross indicates the position of the best-fit solution. The white dotted-line delimits the region in the $\log g{-}T_{\rm eff}$ plane where all the observed periods are identified with modes predicted to be unstable according to nonadiabatic theory. Right panel: slice of the S²-function (in logarithmic units) along the $M_{*}{-}\log q(H)$ plane at fixed parameters $T_{{\rm eff}}$ and $\log g$ , set to their optimal values found from the best-fit model solution ( $T_{{\rm eff}}=$ 35,050 K and $\log g=5.8105$ ). The red dotted-line rectangle shows the estimated error box associated with our asteroseismic determination of the parameters $\log g$ and $T_{{\rm eff}}$ . The red cross indicates the position of the best-fit solution.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{5316fig4.eps} \end{figure}$ Figure 4: Slice of the "projected'' S²-function (in logarithmic units) along the $\log g{-}T_{\rm eff}$ plane at fixed parameter M_*, set to its optimal value from the best-fit model solution ( M_*=0.4988 $M_{\odot }$ ). The projected $\log q(H)$ parameter was varied between -2.0 and -5.0, in steps of 0.025. The labelled axis positioned along the valley of minimum S² indicates the location of the local minimum of S² for the given values of $\log q(H)$ . The dot-dot-dashed-line, dashed-line, dot-dashed-line, and dotted-line rectangles represent the various spectroscopic estimates with their uncertainties for the atmospheric parameters of PG 1325+101. They correspond to the MMT1, BG9, PB6, and Telting & Østensen (2004) measurements, respectively. The mean values derived from these measurements appear as the solid-line rectangle.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{5316fig5.eps} \end{figure}$ Figure 5: Slice of the "projected'' S²-function (in logarithmic units) along the $\log g{-}T_{\rm eff}$ plane at fixed parameter $\log q(H)$ set to its optimal value found for the best-fit model solution ( $\log q(H)=-4.2747$ ). The projected, M_* parameter was varied between 0.40 $M_{\odot }$ and 0.60 $M_{\odot }$ (by steps of 0.0025 $M_{\odot }$ ). The labelled axis positioned along the valley of minimum S² indicates the location of the local minimum of S² for the given values of M_*. The solid-line, dashed-line, dot-dashed-line, and dotted-line rectangles represent the various spectroscopic estimates and their uncertainties for the atmospheric parameters of PG 1325+101. They correspond to the MMT1, BG9, PB6, and Telting & Østensen (2004) measurements, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5316fig6.eps} \end{figure}$ Figure 6: Comparison of the observed period spectrum of PG 1325+101 (thick dashed-dotted-line red segments) with the theoretical pulsation spectrum of the optimal model. For the latter spectrum, solid-line segments indicate excited modes, while dotted-line segments correspond to damped modes. All pulsation modes with $\ell =0$ , 1, 2, 3, and 4 in the period interval 60-210 s are illustrated. The values of the radial order k are also indicated for each mode. These modes are all acoustic waves (including the f-modes). The g-modes have periods that fall outside the range of interest for PG 1325+101.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{5316fig1a.eps}\hspace{1.5... ...space{1.5cm} \includegraphics[width=7.1cm,clip]{5316fig1d.eps}\par \end{figure}$	Figure 1: Model fits ( thick curves) to the hydrogen and helium lines ( thin curves) available in the 4000-4950 Å spectral range in our time-averaged spectrum RS6 ( upper left panel), PB6 ( upper right panel), BG9 ( lower left panel), and MMT1 ( lower right panel).
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$\begin{figure} \par\includegraphics[width=8cm]{5316fig2.eps} \end{figure}$	Figure 2: Model fits ( dotted curves) to the He I 4471 line ( solid curves) in our MMT spectrum of PG 1325+101 assuming various values of the projected rotational velocity Vsin i.
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