All Figures

$\begin{figure} {\resizebox{7.9cm}{!}{ \includegraphics[clip]{Fh041_f1.eps}} } \end{figure}$ Figure 1: The photometry collected from different resources; from IAUCs: triangles - V. Tabur (possibly spurious detections - see text), diamonds - AAVSO, squares - others in IAUCs; crosses: ASAS-3. The R band CCD values of Tabur were shifted down by 1 $.\!\!^{\rm m}$ 0 to correspond to the visual and V band measurements.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{Fh041_f2.eps} \end{figure}$ Figure 2: The scatter diagram of the astrometric calibration sources around the target.
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In the text

$\begin{figure} {\resizebox{!}{4cm}{ \includegraphics{Fh041_f3a.eps}}\phantom{XX}\resizebox{!}{4cm} {\includegraphics{Fh041_f3b.eps}} } \end{figure}$ Figure 3: The finding chart for the target from our ESO NTT observations (left) and from SuperCOSMOS scans of the UKIST B plate. The coordinates from the astrometry are centered (fineline +). There is a faint ( $B\geq20\hbox{$.\!\!^{\rm m}$ }5$ , $R>19\hbox{$.\!\!^{\rm m}$ }5$ ) star ( $\times$ ) which might be the progenitor (see text).
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In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{Fh041_f4.eps} \end{figure}$ Figure 4: The overall spectrum of V2573 Oph. H $_{\alpha }$ and CaII _849+854+866 are displaced exceeding the box in order to see all the weaker features. All P-Cygni profiles show more or less the same global expansion, but with different substructures. The maximum expansion velocity is about 2200 km s^-1. Most of the lines at the red end are blends of OI, NI and metal lines. They are thus not labelled individually.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{Fh041_f5.eps} \end{figure}$ Figure 5: The P-Cygni profile of the hydrogen Balmer line. The line peak grows significantly from day to day while it gets smaller. Especially the emission wing around -1000 km s^-1 vanishes more and more.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{Fh041_f6.eps} \end{figure}$ Figure 6: The profile of the OI line at 777 nm shows the highest expansion (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{Fh041_f7.eps} \end{figure}$ Figure 7: The profile of the Na-D line shows nearly the same profile like the Balmer lines. The emission feature at -1000 km s^-1 also faded during the observation period.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{Fh041_f8.eps} \end{figure}$ Figure 8: The profile of the IR CA II lines at 866 nm (upper panel) and at 849+854 nm (lower panel). They show now P-Cygni type absorption but a nicely pronounced optically thin shell structure with an expansion of 550 km s^-1. The structure is blueshifted by about 150 km s^-1.
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In the text

$\begin{figure} {\resizebox{7.9cm}{!}{ \includegraphics[clip]{Fh041_f1.eps}} } \end{figure}$	Figure 1: The photometry collected from different resources; from IAUCs: triangles - V. Tabur (possibly spurious detections - see text), diamonds - AAVSO, squares - others in IAUCs; crosses: ASAS-3. The R band CCD values of Tabur were shifted down by 1 $.\!\!^{\rm m}$ 0 to correspond to the visual and V band measurements.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{Fh041_f2.eps} \end{figure}$	Figure 2: The scatter diagram of the astrometric calibration sources around the target.
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$\begin{figure} {\resizebox{!}{4cm}{ \includegraphics{Fh041_f3a.eps}}\phantom{XX}\resizebox{!}{4cm} {\includegraphics{Fh041_f3b.eps}} } \end{figure}$	Figure 3: The finding chart for the target from our ESO NTT observations (left) and from SuperCOSMOS scans of the UKIST B plate. The coordinates from the astrometry are centered (fineline +). There is a faint ( $B\geq20\hbox{$.\!\!^{\rm m}$ }5$ , $R>19\hbox{$.\!\!^{\rm m}$ }5$ ) star ( $\times$ ) which might be the progenitor (see text).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{Fh041_f5.eps} \end{figure}$	Figure 5: The P-Cygni profile of the hydrogen Balmer line. The line peak grows significantly from day to day while it gets smaller. Especially the emission wing around -1000 km s^-1 vanishes more and more.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{Fh041_f6.eps} \end{figure}$	Figure 6: The profile of the OI line at 777 nm shows the highest expansion (see text).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{Fh041_f7.eps} \end{figure}$	Figure 7: The profile of the Na-D line shows nearly the same profile like the Balmer lines. The emission feature at -1000 km s^-1 also faded during the observation period.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{Fh041_f8.eps} \end{figure}$	Figure 8: The profile of the IR CA II lines at 866 nm (upper panel) and at 849+854 nm (lower panel). They show now P-Cygni type absorption but a nicely pronounced optically thin shell structure with an expansion of 550 km s^-1. The structure is blueshifted by about 150 km s^-1.
Open with DEXTER