All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{0570fig1.ps} \end{figure}$ Figure 1: Spectrum of SN 1998bu obtained with SofI at the NTT on January 26, 1999.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{0570fig2.ps} \end{figure}$ Figure 2: Spectrum of SN 1998bu obtained with ISAAC at UT1 on May 1, 1999.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{0570fig3.ps} \end{figure}$ Figure 3: Light curve of SN 1998bu in the H-band. Early data from Meikle (2000) and template light curve from Elias (1983). For the observation at the epoch of 350 days the lower point (dotted circle) indicates the magnitude of the supernova after the removal of a possible contribution from continuum not arising from the ejecta.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{0570fig4.ps} \end{figure}$ Figure 4: Spectrum of SN 1998bu obtained with FORS1 at UT1 on June 11, 1999. The lower spectrum is a trace of the late light echo spectrum (Cappellaro et al. 2001) scaled by a factor of 2 upwards - see text for details.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{0570fig5.ps} \end{figure}$ Figure 5: A fit to the spectrum obtained with SOFI at the NTT using a simple NLTE [Fe I], [Fe II] and [Fe III] model and LTE [Co II]. The narrow (few pixel) spikes in the data are artifacts of the atmosphere and/or the detector.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{0570fig6.ps}\end{figure}$ Figure 6: A fit to the combined FORS1 and ISAAC spectrum using a simple NLTE [Fe I], [Fe II] and [Fe III] model and LTE [Co II], [Co III], [Ni II], [Ni III]. The FORS1 spectrum has been scaled to match the ISAAC one based on the photometric evolution (see text for details). The narrow (few pixel) spikes in the data are artifacts of the atmosphere and/or the detector.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.3cm,clip]{0570fig7.ps} \end{figure}$ Figure 7: Same as Fig. 5 but focused on the H-band. The long dashed line marks the [Fe II] spectrum and the short dashed line the [Co II]. The continuous line is the sum. The 1.55- $\mu$ m feature is fit by the 1.533 [Fe II] and 1.547 [Co II] lines.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.3cm,clip]{0570fig8.ps} \end{figure}$ Figure 8: Same as Fig. 6 but focused on the H-band. The spectra identification is as per Fig. 5. Additionally the dot-dash line marks the [Fe I] spectrum. The 1.55- $\mu$ m feature is fit by the 1.533 [Fe II] and 1.547 [Co II] lines.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{0570fig9.ps} \end{figure}$ Figure 9: The derived mass ratio of Co to Fe in the ejecta of SN 1998bu as a function of time after explosion. The line represents the theoretical evolution from radioactive decay and is not fit to the data. The error bars reflect a error of 1000 K in the assumed temperature for the electron gas.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{0570fig1.ps} \end{figure}$	Figure 1: Spectrum of SN 1998bu obtained with SofI at the NTT on January 26, 1999.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{0570fig2.ps} \end{figure}$	Figure 2: Spectrum of SN 1998bu obtained with ISAAC at UT1 on May 1, 1999.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{0570fig3.ps} \end{figure}$	Figure 3: Light curve of SN 1998bu in the H-band. Early data from Meikle (2000) and template light curve from Elias (1983). For the observation at the epoch of 350 days the lower point (dotted circle) indicates the magnitude of the supernova after the removal of a possible contribution from continuum not arising from the ejecta.
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$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{0570fig4.ps} \end{figure}$	Figure 4: Spectrum of SN 1998bu obtained with FORS1 at UT1 on June 11, 1999. The lower spectrum is a trace of the late light echo spectrum (Cappellaro et al. 2001) scaled by a factor of 2 upwards - see text for details.
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$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{0570fig5.ps} \end{figure}$	Figure 5: A fit to the spectrum obtained with SOFI at the NTT using a simple NLTE [Fe I], [Fe II] and [Fe III] model and LTE [Co II]. The narrow (few pixel) spikes in the data are artifacts of the atmosphere and/or the detector.
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$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{0570fig6.ps}\end{figure}$	Figure 6: A fit to the combined FORS1 and ISAAC spectrum using a simple NLTE [Fe I], [Fe II] and [Fe III] model and LTE [Co II], [Co III], [Ni II], [Ni III]. The FORS1 spectrum has been scaled to match the ISAAC one based on the photometric evolution (see text for details). The narrow (few pixel) spikes in the data are artifacts of the atmosphere and/or the detector.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.3cm,clip]{0570fig7.ps} \end{figure}$	Figure 7: Same as Fig. 5 but focused on the H-band. The long dashed line marks the [Fe II] spectrum and the short dashed line the [Co II]. The continuous line is the sum. The 1.55- $\mu$ m feature is fit by the 1.533 [Fe II] and 1.547 [Co II] lines.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.3cm,clip]{0570fig8.ps} \end{figure}$	Figure 8: Same as Fig. 6 but focused on the H-band. The spectra identification is as per Fig. 5. Additionally the dot-dash line marks the [Fe I] spectrum. The 1.55- $\mu$ m feature is fit by the 1.533 [Fe II] and 1.547 [Co II] lines.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{0570fig9.ps} \end{figure}$	Figure 9: The derived mass ratio of Co to Fe in the ejecta of SN 1998bu as a function of time after explosion. The line represents the theoretical evolution from radioactive decay and is not fit to the data. The error bars reflect a error of 1000 K in the assumed temperature for the electron gas.
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