All Figures

$\begin{figure} \par\includegraphics[width=13.4cm,clip]{2552fig1.eps} \end{figure}$ Figure 1: ( Top) visual light curve of FN Sgr in 1972-2002. Dots: visual observations from RASNZ, open circles: V magnitudes calculated from our spectra and those from Barbá et al. (1992), square: from Munari et al. (1992), and triangles: derived from FES counts. ( Bottom) evolution of emission line fluxes of H $\alpha$ , He II 4686 and [O III] 5007 (shifted by 0.5 for clarity) in 1988-2002. Bars mark times of photometric minima/times of the inferior spectroscopic conjunction of the red giant. Labelled arrows point to Van Winckel et al. (1993) data (1) and the available IUE spectra.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm]{2552fig2.eps} \end{figure}$ Figure 2: Periodogram ( top) and phased light curves ( bottom) for FN Sgr. Open circles represent normal points calculated from quiescent light curve (MJD $\sim$ 45 000-49 500, dots represent the light curve from the recent outburst (MJD $\sim$ 50 000-52 000).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{2552fig3.eps} \end{figure}$ Figure 3: Emission line profiles in FN Sgr. Each profile was normalized to maximum intensity. The profiles are shifted vertically for better display.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2552fig4.eps} \end{figure}$ Figure 4: Phase plot of [TiO]₁ indices ( top), H $\alpha$ (dots) and H $\beta$ (open circles), He I 5876 (dots), 6678 (open circles) and 7065 (triangles) ( middle), and He II 4686 emission line fluxes ( bottom). The He II 4686 fluxes obtained during the optical outburst maximum, in May 1997 and September 1998, respectively, have been omitted because the very dramatic change in He II flux is due to the outburst and not to orbital motion. The ordinate is logarithmic for line fluxes and linear for [TiO] indices.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{2552fig5.eps} \end{figure}$ Figure 5: Circular orbital solution for $P_{\rm orb} = 568.3$ days fitting the heliocentric radial velocity of the red giant in FN Sgr.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=14cm,clip]{2552fig6.eps} \end{figure}$ Figure 6: Radial velocity data and orbital solutions for FN Sgr. The solid and dotted lines repeat the circular orbit of the M-giant and the cF-abs features, respectively. The dashed lines gives the best elliptical fit to the blue absorption system ( $e = 0.33\pm 0.05$ , $\omega = 240^\circ \pm 9$ ). Triangles represent Van Winckel's data. The solutions correspond to a) M giant absorptions, b) cF-absorption lines, c) H $\alpha$ (open circles), H $\beta$ (open squares) and He II $\lambda$ 4686 wings (solid circles), d) Fe II emission lines, e) He I emission lines, f) He II emission lines, g) [O III] $\lambda$ 5007 line and h) [Fe VII] $\lambda$ 6085 line.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.2cm,clip]{2552fig7.eps} \end{figure}$ Figure 7: Evolution of the hot component in the HR diagram. The observations are separated into four intervals covering the outburst and its preceeding and subsequent quiescent periods as indicated in the legend. The dotted curves are the cooling curves for a 0.64 $M_\odot$ and 0.55 $M_\odot$ white dwarf (Schönberner 1989) and the dashed curves are the line of constant radius.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm]{2552fig2.eps} \end{figure}$	Figure 2: Periodogram ( top) and phased light curves ( bottom) for FN Sgr. Open circles represent normal points calculated from quiescent light curve (MJD $\sim$ 45 000-49 500, dots represent the light curve from the recent outburst (MJD $\sim$ 50 000-52 000).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{2552fig3.eps} \end{figure}$	Figure 3: Emission line profiles in FN Sgr. Each profile was normalized to maximum intensity. The profiles are shifted vertically for better display.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{2552fig5.eps} \end{figure}$	Figure 5: Circular orbital solution for $P_{\rm orb} = 568.3$ days fitting the heliocentric radial velocity of the red giant in FN Sgr.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=7.2cm,clip]{2552fig7.eps} \end{figure}$	Figure 7: Evolution of the hot component in the HR diagram. The observations are separated into four intervals covering the outburst and its preceeding and subsequent quiescent periods as indicated in the legend. The dotted curves are the cooling curves for a 0.64 $M_\odot$ and 0.55 $M_\odot$ white dwarf (Schönberner 1989) and the dashed curves are the line of constant radius.
Open with DEXTER