All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5853fig1.ps}\end{figure}$ Figure 1: Incoherent integration. Off-fringe squared visibility amplitude, i.e. the visibility bias that remains for data off the fringe packet and that is compensated after the Z² compensation (see text for more details). This bias can be described by a power law as a function of photon rate P. As an example, the residual bias is shown for the four reddest channels on the EW baseline. Data are 2 ms incoherent integrations from July 22. Channels 1 though 4 use symbols plus, star, diamond, and triangle, respectively. Power-law fit coefficients are given for each channel, in the same order as shown on the corresponding plot for the coherent analysis in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{5853fig2.ps}\end{figure}$ Figure 2: Coherent integration. As Fig. 1, but for 200 ms coherent integrations as used in this paper. For reasons of comparison, the bin counts are renormalised to 2 ms intervals. It is an additional benefit of the coherent integration that this residual bias shown here is clearly reduced compared to the incoherent integration in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=5.65cm,clip]{5853fig3.ps}\includegraph... ...m,clip]{5853fig7.ps}\includegraphics[width=5.65cm,clip]{5853fig8.ps}\end{figure}$ Figure 3: Squared visibility amplitudes of $\gamma$ Sge obtained from NPOI on the EW baseline. Also shown are synthetic visibility curves of the best fitting model atmospheres as described below in Sect. 4. Each model fit is performed to all NPOI visibility data (squared visibility amplitudes, triple amplitudes, and closure phases) simultaneously. The parameters of the plotted model curves are listed in Table 5. The synthetic visibility values are calculated for each specific bandpass of our observation and these points are connected by straight lines. A 7th used NPOI observation is not included for the sake of clarity of the figure and because its projected baseline length is much shorter and this observation thus contains little information in the 2nd lobe.
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In the text

$\begin{figure} \par\hspace*{1.5mm}\includegraphics[width=5.35cm,clip]{5853figa.p... ...m,clip]{5853fige.ps}\includegraphics[width=5.45cm,clip]{5853figf.ps}\end{figure}$ Figure 4: As Fig. 3, but showing the squared visibility amplitudes on the NPOI CW baseline.
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In the text

$\begin{figure} \par\includegraphics[width=5.35cm,clip]{5853figg.ps}\hspace*{2mm}... ...gk.ps}\hspace*{2mm} \includegraphics[width=5.35cm,clip]{5853figl.ps}\end{figure}$ Figure 5: As Fig. 3, but showing the squared visibility amplitudes on the NPOI CE baseline.
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In the text

$\begin{figure} \par\hspace*{1.5mm}\includegraphics[width=5.6cm,clip]{5853figm.ps... ...cm,clip]{5853figq.ps}\includegraphics[width=5.6cm,clip]{5853figr.ps}\end{figure}$ Figure 6: As Fig. 3, but showing the NPOI triple amplitudes.
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In the text

$\begin{figure} \par\includegraphics[width=5.2cm,clip]{5853figs.ps}\hspace*{3mm} ... ...igw.ps}\hspace*{3mm} \includegraphics[width=5.2cm,clip]{5853figx.ps}\end{figure}$ Figure 7: As Fig. 3, but showing the NPOI closure phases. Note that the slope of the model flip from 0 to $\pi$ is an artifact because the model values are only calculated for each NPOI spectral channel.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{5853figy.ps}\end{figure}$ Figure 8: Measured $\gamma$ Sagittae squared visibility amplitudes obtained with VLTI/VINCI in June to September 2002, together with the synthetic visibility curves of the best fitting models.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{5853figz.ps}\end{figure}$ Figure 9: Flux of $\gamma$ Sge from Alekseeva et al. (1997) in the wavelength range of our NPOI observations, compared to the model atmosphere predictions with model parameters listed in Table 5. The limb-darkened 0% diameter values $\Theta _{\rm LD}$ derived from the fit to the interferometric data were used to scale the model SEDs. The spectral resolution of the model SEDs is convolved to the resolution of the data used, i.e. to 10 nm.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{5853fig2.ps}\end{figure}$	Figure 2: Coherent integration. As Fig. 1, but for 200 ms coherent integrations as used in this paper. For reasons of comparison, the bin counts are renormalised to 2 ms intervals. It is an additional benefit of the coherent integration that this residual bias shown here is clearly reduced compared to the incoherent integration in Fig. 1.
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$\begin{figure} \par\hspace*{1.5mm}\includegraphics[width=5.35cm,clip]{5853figa.p... ...m,clip]{5853fige.ps}\includegraphics[width=5.45cm,clip]{5853figf.ps}\end{figure}$	Figure 4: As Fig. 3, but showing the squared visibility amplitudes on the NPOI CW baseline.
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$\begin{figure} \par\includegraphics[width=5.35cm,clip]{5853figg.ps}\hspace{2mm}... ...gk.ps}\hspace{2mm} \includegraphics[width=5.35cm,clip]{5853figl.ps}\end{figure}$	Figure 5: As Fig. 3, but showing the squared visibility amplitudes on the NPOI CE baseline.
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$\begin{figure} \par\hspace*{1.5mm}\includegraphics[width=5.6cm,clip]{5853figm.ps... ...cm,clip]{5853figq.ps}\includegraphics[width=5.6cm,clip]{5853figr.ps}\end{figure}$	Figure 6: As Fig. 3, but showing the NPOI triple amplitudes.
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$\begin{figure} \par\includegraphics[width=5.2cm,clip]{5853figs.ps}\hspace{3mm} ... ...igw.ps}\hspace{3mm} \includegraphics[width=5.2cm,clip]{5853figx.ps}\end{figure}$	Figure 7: As Fig. 3, but showing the NPOI closure phases. Note that the slope of the model flip from 0 to $\pi$ is an artifact because the model values are only calculated for each NPOI spectral channel.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{5853figy.ps}\end{figure}$	Figure 8: Measured $\gamma$ Sagittae squared visibility amplitudes obtained with VLTI/VINCI in June to September 2002, together with the synthetic visibility curves of the best fitting models.
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