All Figures

$\begin{figure} { \psfig{figure=0580f1.eps,width=15.8cm,clip=} } \end{figure}$ Figure 1: $120^{\prime \prime }\times 120^{\prime \prime }$ fields centered on V1494 Aql. Left to right: POSS2 red, R-band image at HJD = 2 452 930.9568 (stellar $FWHM=1\hbox{$.\!\!^{\prime\prime}$ }4$ ), I-band image at HJD = 2 452 930.9526 ( $FWHM=1\hbox{$.\!\!^{\prime\prime}$ }2$ ). Dashes point to the nova, identified through the eclipses. North is up, east is to the left.
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In the text

$\begin{figure} { \psfig{figure=0580f2.eps,width=6.5cm,clip=} } \end{figure}$ Figure 2: A comparison of the new astrometric solution and published coordinates of the nova and the suspected progenitor (Pereira et al. 1999). The cross in the left corner shows the uncertainty.
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In the text

$\begin{figure} { \psfig{figure=0580f3.eps,width=7.3cm,clip=} } \end{figure}$ Figure 3: Eclipsing light curves. Upper curve: integrated magnitudes calculated from the flux-calibrated AAT spectra; middle curve: phase diagram of all data taken in August, 2003; lower curve: the same after correcting for the secondary light.
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In the text

$\begin{figure} { \psfig{figure=0580f4.eps,width=8.2cm,clip=} } \end{figure}$ Figure 4: Top panel: a sample AAT-spectrum of V1494 Aql. Note the symmetric structure of the H $\alpha$ profile. Bottom panel: a close-up view of the bluest quarter compared to the flux-standard.
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In the text

$\begin{figure} { \psfig{figure=0580f1.eps,width=15.8cm,clip=} } \end{figure}$	Figure 1: $120^{\prime \prime }\times 120^{\prime \prime }$ fields centered on V1494 Aql. Left to right: POSS2 red, R-band image at HJD = 2 452 930.9568 (stellar $FWHM=1\hbox{$.\!\!^{\prime\prime}$ }4$ ), I-band image at HJD = 2 452 930.9526 ( $FWHM=1\hbox{$.\!\!^{\prime\prime}$ }2$ ). Dashes point to the nova, identified through the eclipses. North is up, east is to the left.
Open with DEXTER

$\begin{figure} { \psfig{figure=0580f2.eps,width=6.5cm,clip=} } \end{figure}$	Figure 2: A comparison of the new astrometric solution and published coordinates of the nova and the suspected progenitor (Pereira et al. 1999). The cross in the left corner shows the uncertainty.
Open with DEXTER

$\begin{figure} { \psfig{figure=0580f3.eps,width=7.3cm,clip=} } \end{figure}$	Figure 3: Eclipsing light curves. Upper curve: integrated magnitudes calculated from the flux-calibrated AAT spectra; middle curve: phase diagram of all data taken in August, 2003; lower curve: the same after correcting for the secondary light.
Open with DEXTER

$\begin{figure} { \psfig{figure=0580f4.eps,width=8.2cm,clip=} } \end{figure}$	Figure 4: Top panel: a sample AAT-spectrum of V1494 Aql. Note the symmetric structure of the H $\alpha$ profile. Bottom panel: a close-up view of the bluest quarter compared to the flux-standard.
Open with DEXTER