All Figures

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5530fig1.eps} \end{figure}$ Figure 1: The location of SN 2006aj is shown here in a VLT/FORS2 R-band image taken on 2006 March 1, at 00:52 UT (30 s exposure time). The field of view is approximately 2 $\times$ 3 arcmin.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5530fig2.eps} \end{figure}$ Figure 2: The light curves of SN 2006aj based on our $\it BVRI$ data after correcting for extinction and host flux contribution. The data were fitted using the light curves of SN 1998bw as a template, not considering data from SN 2006aj that was taken before 8.8 days post burst. The residuals $\Delta$ m represent observed values minus the fit.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5530fig3.eps} \end{figure}$ Figure 3: The light curves of SN 2006aj fitted by including an additional early component which decays according to a power-law. Solid lines mark the fit, the dashed lines are the power-law component and the dotted lines are the SN component. The time scale is logarithmic to show in detail the earlier data.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5530fig4.eps} \end{figure}$ Figure 4: The distribution of the luminosity factor k in the R band with redshift z. There is no apparent correlation with redshift, even though we caution that all the k values refer to the R band in the observer frame, corresponding to different wavelengths in the host frame. Filled symbols mark the k values that have been corrected for host extinction, open symbols represent supernovae for which this correction could not be applied. A star marks the value derived from the R-band light curve of SN 2006aj by removing data before 8.8 days from the fit. SN 1998bw is at k=1, by definition.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{5530fig5.eps} \end{figure}$ Figure 5: Luminosity factor k versus stretch factor s in the R band for all GRB-SNe in our sample (Table 3). The symbols are identical to those used in Fig. 4. SN 1998bw defines k=1, s=1. Note that in the case of SN 2006aj the values for $\it BVRI$ are plotted. Furthermore, we plot the type Ic supernova SN 1994I and the type Ic broad-lined SN 2002ap, neither of which are associated with GRBs. Both are fainter than any GRB-SN in our sample for which the host extinction has been corrected.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5530fig6.eps} \end{figure}$ Figure 6: The absolute V-band magnitude $M_{\rm V}$ of stripped-envelope supernovae versus their distance modulus. This is an expanded version of Figure 1 in RBB06, and the values for SN of type IIb, Ib and Ic have been taken from that work but transformed according to the world model used here. The individual GRB-SNe have the same numbers as in Fig. 7. We have also labeled two local type Ic SNe we have included in our study (Fig. 5; Appendix). GRB-SNe without known host extinction are not included. The dashed line at $M_{\rm V}=-19.5$ denotes the typical absolute magnitude of type Ia SNe (the "ridgeline''). The slanted dotted line denotes a constant visual magnitude $m_{\rm V}=16$ in the case of no extinction.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5530fig7.eps} \end{figure}$ Figure 7: The visual host-galaxy extinction $A_{\rm V}$ (in the host frame) of stripped-envelope supernovae versus their distance modulus. The values for SNe of type IIb, Ib and Ic have been taken from RBB06, while the data for the GRB-SNe are from K06. We labeled individual GRB-SNe and the two type Ic SNe we have also studied. GRB-SNe without known host extinction were not included.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5530fig8.eps} \end{figure}$ Figure A.1: The two local type Ic supernovae SN 1994I and SN 2002ap fitted with the model light curve of SN 1998bw at the respective redshifts. In both cases, the light curve of SN 1998bw does not fit the light curves of the other SNe completely. The best agreement is obtained for SN 2002ap, where data after ten days up to 60 days are fitted well by the SN 1998bw light curve. For SN 1994I data before and after the maximum had to be excluded from the fit.

In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5530fig1.eps} \end{figure}$	Figure 1: The location of SN 2006aj is shown here in a VLT/FORS2 R-band image taken on 2006 March 1, at 00:52 UT (30 s exposure time). The field of view is approximately 2 $\times$ 3 arcmin.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5530fig2.eps} \end{figure}$	Figure 2: The light curves of SN 2006aj based on our $\it BVRI$ data after correcting for extinction and host flux contribution. The data were fitted using the light curves of SN 1998bw as a template, not considering data from SN 2006aj that was taken before 8.8 days post burst. The residuals $\Delta$ m represent observed values minus the fit.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5530fig3.eps} \end{figure}$	Figure 3: The light curves of SN 2006aj fitted by including an additional early component which decays according to a power-law. Solid lines mark the fit, the dashed lines are the power-law component and the dotted lines are the SN component. The time scale is logarithmic to show in detail the earlier data.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5530fig7.eps} \end{figure}$	Figure 7: The visual host-galaxy extinction $A_{\rm V}$ (in the host frame) of stripped-envelope supernovae versus their distance modulus. The values for SNe of type IIb, Ib and Ic have been taken from RBB06, while the data for the GRB-SNe are from K06. We labeled individual GRB-SNe and the two type Ic SNe we have also studied. GRB-SNe without known host extinction were not included.
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