All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4122f1.eps} \end{figure}$ Figure 1: Schematic picture of the lensing situation. $z_{\rm lim}\ (m_{\rm lim})$ is the limiting redshift (magnitude) without the lensing cluster. The shaded area indicates the volume where the SNe are bright enough to be detected and are visible within the field. Compare the four different areas 1-4 to the four different distinguishable z-bin ranges of Fig. 2.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f2.eps} \end{figure}$ Figure 2: Number of SNe detected per year in redshift bins of $\Delta z=0.05$ . Area 1 at redshifts smaller than the cluster redshift, $z_{\rm cl}$ , area 2 between the lens and $z_{\rm lim}$ , area 3 where the visible field limits the number of SNe and area 4 where the magnification is the limitation. The dashed line shows the number count without the lens and the solid line with a NFW lens redshift of $z_{\rm cl}=0.2$ and a field-of-view of 16 sq. arcmin.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f3.eps} \end{figure}$ Figure 3: Supernova rates versus redshift in bins of $\Delta z=0.05$ . For core collapse SNe the plot shows IIn+IIp+IIL+Ibc+87a-like. The increasing time dilation of the SN rate with redshift is taken into account. The distribution includes neither lensing nor observational selection effects.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f4.eps} \end{figure}$ Figure 4: Redshift dependence of the Einstein radius, within which strong lensing effects occur, for two different cluster redshifts, $z_{\rm cl}$ . The cluster virial mass is $1.4\times 10^{15}\ h^{-1}~M_{\odot}$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f5.eps} \end{figure}$ Figure 5: Redshift reach as a function of limiting (Z-band) magnitude in the supernova search. For comparison, the ACS/GOODS transient survey has a limiting magnitude around Z=25.5.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f6.eps} \end{figure}$ Figure 6: Number of Type Ia SNe detected per year and $\Delta z=0.05$ vs. z in the Z-band for various cluster redshifts, $z_{\rm cl}$ . The FOV is 16 sq. arcmin while the limiting magnitude is chosen to be what is currently used at ACS for the GOODS transient survey.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f7.eps} \end{figure}$ Figure 7: Number of Type IIn+p+L SNe detected per year and $\Delta z=0.05$ vs. z in the Z-band for two different cluster redshifts, $z_{\rm cl}$ . The FOV is 16 sq. arcmin.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{h4122f8.eps} \end{figure}$ Figure 8: Gain factor of Type IIn+p+L SNe detected vs. $m_{\rm lim}$ in the Z-band for two different cluster redshifts, $z_{\rm cl}$ . The FOV is 16 sq. arcmin.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f9.eps} \end{figure}$ Figure 9: Gain factor of Type IIn+p+L SNe detected vs. $\theta _{\rm lim}$ for two different cluster masses $M_{\rm cl}$ and $z_{\rm cl}=0.2$ . The limiting magnitude is 26 for this plot, using the J-band.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f10.eps} \end{figure}$ Figure 10: Number of Type IIn+p+L SNe detected per year and $\Delta z=0.05$ vs. z in the J-band. The cluster redshift is 0.5 and the FOV is 16 sq. arcmin. This plot shows the small difference between the NFW and SIS profiles at this limiting magnitude.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f11.eps} \end{figure}$ Figure 11: Gain factor of Type IIn+p+L SNe detected vs. $m_{\rm lim}$ in the J-band for two different cluster redshifts, $z_{\rm cl}$ . The small difference between NFW and SIS is also seen in this plot. The FOV is 16 sq. arcmin.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f12.eps} \end{figure}$ Figure 12: Number of Type IIn+p+L SNe detected per year and $\Delta z=0.05$ vs. z in the J-band for a cluster at z=0.2 and with a limiting magnitude of 24. The FOV is 16 sq. arcmin.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f13.eps} \end{figure}$ Figure 13: Number of Type IIn+p+L SNe detected per year vs. $m_{\rm lim}$ in the J-band for two different cluster redshifts, $z_{\rm cl}$ . The FOV is 16 sq. arcmin and the distribution is cumulative.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f14.eps} \end{figure}$ Figure 14: Gain factor of Type Ia SNe detected vs. $m_{\rm lim}$ in the J-band for two different cluster redshifts, $z_{\rm cl}$ . The FOV is 16 sq. arcmin.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f15.eps} \end{figure}$ Figure 15: Number of Type Ia SNe detected per year vs. $m_{\rm lim}$ for two different cluster redshifts, $z_{\rm cl}$ . The FOV is 16 sq. arcmin and the distribution is cumulative.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f16.eps} \end{figure}$ Figure 16: Gain factor of Type IIn+p+L SNe detected vs. $m_{\rm lim}$ . in the I- and J-bands for two different cluster redshifts, $z_{\rm cl}$ . The FOV is 16 sq. arcmin.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{h4122f17.eps} \end{figure}$ Figure 17: Magnification as a function of the impact parameter in the lens plane for a source at z=2. The lens redshift is 0.2.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4122f1.eps} \end{figure}$	Figure 1: Schematic picture of the lensing situation. $z_{\rm lim}\ (m_{\rm lim})$ is the limiting redshift (magnitude) without the lensing cluster. The shaded area indicates the volume where the SNe are bright enough to be detected and are visible within the field. Compare the four different areas 1-4 to the four different distinguishable z-bin ranges of Fig. 2.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f3.eps} \end{figure}$	Figure 3: Supernova rates versus redshift in bins of $\Delta z=0.05$ . For core collapse SNe the plot shows IIn+IIp+IIL+Ibc+87a-like. The increasing time dilation of the SN rate with redshift is taken into account. The distribution includes neither lensing nor observational selection effects.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f4.eps} \end{figure}$	Figure 4: Redshift dependence of the Einstein radius, within which strong lensing effects occur, for two different cluster redshifts, $z_{\rm cl}$ . The cluster virial mass is $1.4\times 10^{15}\ h^{-1}~M_{\odot}$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f5.eps} \end{figure}$	Figure 5: Redshift reach as a function of limiting (Z-band) magnitude in the supernova search. For comparison, the ACS/GOODS transient survey has a limiting magnitude around Z=25.5.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f6.eps} \end{figure}$	Figure 6: Number of Type Ia SNe detected per year and $\Delta z=0.05$ vs. z in the Z-band for various cluster redshifts, $z_{\rm cl}$ . The FOV is 16 sq. arcmin while the limiting magnitude is chosen to be what is currently used at ACS for the GOODS transient survey.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f7.eps} \end{figure}$	Figure 7: Number of Type IIn+p+L SNe detected per year and $\Delta z=0.05$ vs. z in the Z-band for two different cluster redshifts, $z_{\rm cl}$ . The FOV is 16 sq. arcmin.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{h4122f8.eps} \end{figure}$	Figure 8: Gain factor of Type IIn+p+L SNe detected vs. $m_{\rm lim}$ in the Z-band for two different cluster redshifts, $z_{\rm cl}$ . The FOV is 16 sq. arcmin.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f9.eps} \end{figure}$	Figure 9: Gain factor of Type IIn+p+L SNe detected vs. $\theta _{\rm lim}$ for two different cluster masses $M_{\rm cl}$ and $z_{\rm cl}=0.2$ . The limiting magnitude is 26 for this plot, using the J-band.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f10.eps} \end{figure}$	Figure 10: Number of Type IIn+p+L SNe detected per year and $\Delta z=0.05$ vs. z in the J-band. The cluster redshift is 0.5 and the FOV is 16 sq. arcmin. This plot shows the small difference between the NFW and SIS profiles at this limiting magnitude.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f11.eps} \end{figure}$	Figure 11: Gain factor of Type IIn+p+L SNe detected vs. $m_{\rm lim}$ in the J-band for two different cluster redshifts, $z_{\rm cl}$ . The small difference between NFW and SIS is also seen in this plot. The FOV is 16 sq. arcmin.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f12.eps} \end{figure}$	Figure 12: Number of Type IIn+p+L SNe detected per year and $\Delta z=0.05$ vs. z in the J-band for a cluster at z=0.2 and with a limiting magnitude of 24. The FOV is 16 sq. arcmin.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f13.eps} \end{figure}$	Figure 13: Number of Type IIn+p+L SNe detected per year vs. $m_{\rm lim}$ in the J-band for two different cluster redshifts, $z_{\rm cl}$ . The FOV is 16 sq. arcmin and the distribution is cumulative.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f14.eps} \end{figure}$	Figure 14: Gain factor of Type Ia SNe detected vs. $m_{\rm lim}$ in the J-band for two different cluster redshifts, $z_{\rm cl}$ . The FOV is 16 sq. arcmin.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f15.eps} \end{figure}$	Figure 15: Number of Type Ia SNe detected per year vs. $m_{\rm lim}$ for two different cluster redshifts, $z_{\rm cl}$ . The FOV is 16 sq. arcmin and the distribution is cumulative.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{h4122f16.eps} \end{figure}$	Figure 16: Gain factor of Type IIn+p+L SNe detected vs. $m_{\rm lim}$ . in the I- and J-bands for two different cluster redshifts, $z_{\rm cl}$ . The FOV is 16 sq. arcmin.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{h4122f17.eps} \end{figure}$	Figure 17: Magnification as a function of the impact parameter in the lens plane for a source at z=2. The lens redshift is 0.2.
Open with DEXTER