All Figures

$\begin{figure} \par\mbox{\includegraphics[height=9.5cm,width=8.5cm]{1318fig1.ps}\includegraphics[height=9.5cm,width=8.2cm]{1318fig2.ps} } \end{figure}$ Figure 1: Spectral evolution of SN 1990I during the photospheric phase (A), and during the nebular phase (B). Days since maximum are shown. All the spectra have been corrected for the recession velocity of the host galaxy and shifted by an arbitrary amount for clarity. The strongest features are also reported.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=8.5cm,width=8cm]{1318fig3.ps}\end{figure}$ Figure 2: Possible location of He I lines in the photospheric phase of SN 1990I (short-dashed lines). The absorption features near 6050 Å and 6250 Å are marked (long-dashed lines; Sect. 2.1). Phases since maximum light are reported.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=7.2cm,width=7.3cm]{1318fig4.ps}\end{figure}$ Figure 3: The time evolution of the ratio F([Ca II])/F([O I]) of SN 1990I together with that of a sample of SNe. The difference between SN 1987A and the remaining SNe is clear. For convenience we refer to phases since explosion date (see Sect. 2.2).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=12.1cm,width=14cm]{1318fig5.ps}\end{figure}$ Figure 4: The time evolution, in velocity space, of the most prominent nebular lines: Mg I] 4571 Å, [O I] 6300,64 Å, [Ca II] 7307.5 Å and O I 7774 Å. [O II] 7322 Å may contribute on the red side of [Ca II] 7307.5 Å. Shown as well are the coefficients by which the spectra have been multiplied for clarity. Rest wavelengths are marked by vertical long-dashed lines.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=7.8cm,width=7.4cm]{1318fig6.ps}\end{figure}$ Figure 5: The strongest lines, in velocity space, of the 90 d spectrum. The features are clearly asymmetric and flat topped, with the presence of fine structures. Two bumps with similar velocities in the [Ca II] 7307.5 Å and Ca II IR-triplet lines are marked.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=9.6cm,width=8.5cm]{1318fig7.ps}\end{figure}$ Figure 6: The [O I]6300,64 Å line profile of SN 1990I at three different epochs of evolution (since maximum light). Comparison with SNe 1993J and SN 1998bw is made, indicating the high velocity nature of SN 1990I and the presence of a " depletion'' structure in the blue edge of the emission profile ( lower panel).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=8.5cm,width=8.7cm]{1318fig8.ps}\end{figure}$ Figure 7: Fit to the 237 d [O I] 6300,64 Å line profile of SN 1990I. Shown in thick line is the sum of the three Gaussians for [O I] 6300 Å, [O I] 6364 Å and Fe II 6239 Å (dashed lines; see text). The residuals are displayed in the lower panel.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=10cm,width=12.3cm]{1318fig9.ps}\end{figure}$ Figure 8: B, V, R, and I light curves of SN 1990I. The light curves have been shifted by the reported amounts. Also shown are the fits to the V-light curve tail (dotted lines) and as well the ⁵⁶Co to ⁵⁶Fe decay slope (long-dashed line).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=9.5cm,width=12cm]{1318fig10.ps}\end{figure}$ Figure 9: Comparison of the V absolute light curve of SN 1990I with those of other Ib/c events. The ⁵⁶Co to ⁵⁶Fe decay slope is shown (short-dashed line). The used parameters are reported in Table 5.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=8.8cm,width=8.5cm]{1318fig11.ps}\end{figure}$ Figure 10: The evolution of the B-V intrinsic colour of SN 1990I, compared to those of other Ib/c events. The adopted reddening for each event is reported in Table 5.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=8.9cm,width=12cm]{1318fig12.ps}\end{figure}$ Figure 11: The computed " BVRI'' bolometric light curve of SN 1990I together with that of SN 1993J for comparison. SNe 1990I and 1993J luminosities are shifted upward to take account of a " JHK'' contribution of the order of 35 $\%$ . The best fit with a simplified $\gamma$ -ray deposition model from ⁵⁶Ni $\rightarrow$ ⁵⁶Co $\rightarrow$ ⁵⁶Fe is shown. It corresponds to $M_{\rm ej} \sim$ 3.7 $M_{\odot }$ and M(Ni) $\sim$ 0.11 $M_{\odot }$ . The window displays the evolution of the fraction of the $\gamma$ -ray luminosity deposited in the envelope corresponding to the best fit.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\includegraphics[height=9.5cm,width=8.5cm]{1318fig1.ps}\includegraphics[height=9.5cm,width=8.2cm]{1318fig2.ps} } \end{figure}$	Figure 1: Spectral evolution of SN 1990I during the photospheric phase (A), and during the nebular phase (B). Days since maximum are shown. All the spectra have been corrected for the recession velocity of the host galaxy and shifted by an arbitrary amount for clarity. The strongest features are also reported.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=8.5cm,width=8cm]{1318fig3.ps}\end{figure}$	Figure 2: Possible location of He I lines in the photospheric phase of SN 1990I (short-dashed lines). The absorption features near 6050 Å and 6250 Å are marked (long-dashed lines; Sect. 2.1). Phases since maximum light are reported.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=7.2cm,width=7.3cm]{1318fig4.ps}\end{figure}$	Figure 3: The time evolution of the ratio F([Ca II])/F([O I]) of SN 1990I together with that of a sample of SNe. The difference between SN 1987A and the remaining SNe is clear. For convenience we refer to phases since explosion date (see Sect. 2.2).
Open with DEXTER

$\begin{figure} \par\includegraphics[height=12.1cm,width=14cm]{1318fig5.ps}\end{figure}$	Figure 4: The time evolution, in velocity space, of the most prominent nebular lines: Mg I] 4571 Å, [O I] 6300,64 Å, [Ca II] 7307.5 Å and O I 7774 Å. [O II] 7322 Å may contribute on the red side of [Ca II] 7307.5 Å. Shown as well are the coefficients by which the spectra have been multiplied for clarity. Rest wavelengths are marked by vertical long-dashed lines.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=7.8cm,width=7.4cm]{1318fig6.ps}\end{figure}$	Figure 5: The strongest lines, in velocity space, of the 90 d spectrum. The features are clearly asymmetric and flat topped, with the presence of fine structures. Two bumps with similar velocities in the [Ca II] 7307.5 Å and Ca II IR-triplet lines are marked.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=9.6cm,width=8.5cm]{1318fig7.ps}\end{figure}$	Figure 6: The [O I]6300,64 Å line profile of SN 1990I at three different epochs of evolution (since maximum light). Comparison with SNe 1993J and SN 1998bw is made, indicating the high velocity nature of SN 1990I and the presence of a " depletion'' structure in the blue edge of the emission profile ( lower panel).
Open with DEXTER

$\begin{figure} \par\includegraphics[height=8.5cm,width=8.7cm]{1318fig8.ps}\end{figure}$	Figure 7: Fit to the 237 d [O I] 6300,64 Å line profile of SN 1990I. Shown in thick line is the sum of the three Gaussians for [O I] 6300 Å, [O I] 6364 Å and Fe II 6239 Å (dashed lines; see text). The residuals are displayed in the lower panel.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=10cm,width=12.3cm]{1318fig9.ps}\end{figure}$	Figure 8: B, V, R, and I light curves of SN 1990I. The light curves have been shifted by the reported amounts. Also shown are the fits to the V-light curve tail (dotted lines) and as well the ⁵⁶Co to ⁵⁶Fe decay slope (long-dashed line).
Open with DEXTER

$\begin{figure} \par\includegraphics[height=9.5cm,width=12cm]{1318fig10.ps}\end{figure}$	Figure 9: Comparison of the V absolute light curve of SN 1990I with those of other Ib/c events. The ⁵⁶Co to ⁵⁶Fe decay slope is shown (short-dashed line). The used parameters are reported in Table 5.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=8.8cm,width=8.5cm]{1318fig11.ps}\end{figure}$	Figure 10: The evolution of the B-V intrinsic colour of SN 1990I, compared to those of other Ib/c events. The adopted reddening for each event is reported in Table 5.
Open with DEXTER