All Figures

$\begin{figure} \par\includegraphics[width=12cm,clip]{5741fig1.eps} \end{figure}$ Figure 1: Upper left panel: V band light curve. Filled symbols represent our data points, empty symbols represent IAUC data. Vertical dotted lines represent maximum light, t₂, and t₃. Data points are affected by errors $\protect\la$ 0.04 mag in all bands but in U, where the error is 0.1 mag. Lower left panel: evolution of different colors: filled squares represent B-V, empty triangles U-B, crosses V-I and empty squares V-R. Upper right panel: J band light curve. Lower right panel: evolution of near-infrared colors: triangles represent J-H and squares H-K.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5741fig2.eps} \end{figure}$ Figure 2: Spectral energy distribution of V5114 Sgr one day after maximum. The magnitudes in the various bands have been corrected for interstellar extinction.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{5741fig3.eps} \end{figure}$ Figure 3: Dereddened spectra of V5114 Sgr (blue part). Fluxes are in logarithmic scale to show the less intense lines.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{5741fig4.eps} \end{figure}$ Figure 4: Dereddened spectra of V5114 Sgr (red part). Fluxes are in logarithmic scale to show the less intense lines.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{5741fig5.eps}\end{figure}$ Figure 5: Dereddened spectra of V5114 Sgr taken at CTIO and covering the region 3500-5200 $\AA$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12.7cm,clip]{5741fig6.eps}\end{figure}$ Figure 6: Dereddened IR spectrum of V5114 Sgr observed with NIRIS at Lick Observatory on June 22, 2004 UT. Upper panel shows the "blue'' part of the spectrum and the lower panel shows the "red'' part.
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In the text

$\begin{figure} \par\includegraphics[width=7.25cm,clip]{5741fig7.eps} \end{figure}$ Figure 7: Upper panel: evolution of Balmer lines fluxes. Triangles represent H $\alpha$ , squares H $\beta$ , pentagons H $\gamma$ and hexagons H $\delta$ . Filled symbols represent data from FEROS, empty symbols from the RC spectrograph at the 1.5-m telescope at CTIO. Lines connecting the FEROS symbols are meant to show the trend of the data. Lower panel: evolution of ratios of Balmer lines divided by the H $\beta$ flux (symbols refer to the same lines as in the upper panel). Horizontal lines represent the Balmer lines ratios for case B at 10 000 K as from Osterbrock (1989) (from top to bottom H $\alpha$ /H $\beta$ , H $\gamma$ /H $\beta$ and H $\delta$ /H $\beta$ ).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6.9cm,clip]{5741fig8.eps} \end{figure}$ Figure 8: Velocities of the ejecta. Measures are derived as average of P-Cyg profiles of Balmer lines. Squares refer to the faster absorption system and triangles to the slower one. Filled symbols refer to FEROS observations and empty sybols to CTIO observations. Continuous lines are exponential description of the evolution (see text).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5741fig2.eps} \end{figure}$	Figure 2: Spectral energy distribution of V5114 Sgr one day after maximum. The magnitudes in the various bands have been corrected for interstellar extinction.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{5741fig3.eps} \end{figure}$	Figure 3: Dereddened spectra of V5114 Sgr (blue part). Fluxes are in logarithmic scale to show the less intense lines.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{5741fig4.eps} \end{figure}$	Figure 4: Dereddened spectra of V5114 Sgr (red part). Fluxes are in logarithmic scale to show the less intense lines.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{5741fig5.eps}\end{figure}$	Figure 5: Dereddened spectra of V5114 Sgr taken at CTIO and covering the region 3500-5200 $\AA$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=12.7cm,clip]{5741fig6.eps}\end{figure}$	Figure 6: Dereddened IR spectrum of V5114 Sgr observed with NIRIS at Lick Observatory on June 22, 2004 UT. Upper panel shows the "blue'' part of the spectrum and the lower panel shows the "red'' part.
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$\begin{figure} \par\includegraphics[angle=-90,width=6.9cm,clip]{5741fig8.eps} \end{figure}$	Figure 8: Velocities of the ejecta. Measures are derived as average of P-Cyg profiles of Balmer lines. Squares refer to the faster absorption system and triangles to the slower one. Filled symbols refer to FEROS observations and empty sybols to CTIO observations. Continuous lines are exponential description of the evolution (see text).
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