All Figures

$\begin{figure} \mbox{\includegraphics[width=4.3cm,clip]{0424f1a.ps}\hspace*{2mm} \includegraphics[width=4.3cm,clip]{0424f1b.ps} }\end{figure}$ Figure 1: Histograms of the x and y residuals obtained from modeling V1223 Sgr and its reference frame.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{0424f2.ps} \end{figure}$ Figure 2: Overall energy distribution of V1223 Sgr for $\lambda > 1000$ Å (see text). The data are shown twice with two different model fits. Model A (top data set, fluxes multiplied by 10) is for a luminous steady state accretion disk and model B (bottom data set, fluxes as observed) is for a truncated disk plus reprocessed component.
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In the text

$\begin{figure} \mbox{\includegraphics[width=4.3cm,clip]{0424f1a.ps}\hspace*{2mm} \includegraphics[width=4.3cm,clip]{0424f1b.ps} }\end{figure}$	Figure 1: Histograms of the x and y residuals obtained from modeling V1223 Sgr and its reference frame.
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$\begin{figure} \par\includegraphics[width=8.8cm]{0424f2.ps} \end{figure}$	Figure 2: Overall energy distribution of V1223 Sgr for $\lambda > 1000$ Å (see text). The data are shown twice with two different model fits. Model A (top data set, fluxes multiplied by 10) is for a luminous steady state accretion disk and model B (bottom data set, fluxes as observed) is for a truncated disk plus reprocessed component.
Open with DEXTER