All Figures

$\begin{figure} \par\includegraphics[width=14cm,clip]{0256fig1.eps}\end{figure}$ Figure 1: Evolution of the radiation temperature for different decaying ${\Lambda }$ -cosmologies.
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In the text

$\begin{figure} \par\includegraphics[width=11.8cm,clip]{0256fig2.eps}\end{figure}$ Figure 2: Evolution of the radiation temperature for different decaying ${\Lambda }$ -cosmologies; a) shows the evolution between 1+z=1 and 1+z=5, b) is relative to the range 1+z=1 and 1+z=1.25. Current measurements of some extragalactic cosmic microwave background temperatures are labeled as follows: (1) $T_{\rm Molaro}$ , (2) $T_{\rm Srianand}$ , (3) $T_{\rm Ge}$ , (4) $T_{\rm Songaila}$ , (5) $T_{\rm Melchiorri1}$ , (6) $T_{\rm Melchiorri2}$ .
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{0256fig3.eps}\end{figure}$ Figure 3: Bounds on $\Omega _{\Lambda ,2}$ given by the observations. a) and b) corresponds to Songaila observations, c) and d) to Ge observations, e) and f) to Srianand observations. The left panels give the limit on $\Omega _{\Lambda ,2}^-$ when the right panels are relative to $\Omega _{\Lambda ,2}^+$ . Cross-hatching indicates the non-allowed regions. The vertical axis corresponds to $\Omega _{\Lambda ,2}$ and the horizontal axis to m.
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{0256fig4.eps}\end{figure}$ Figure 4: Bounds on $\Omega _{\Lambda ,2}$ given by the observations. a) and b) correspond to Molaro observations, c) and d) to Melchiorri1 observations, e) and f) to Melchiorri2 observations. The left panels give the limit on $\Omega _{\Lambda ,2}^-$ , the right panels are relative to $\Omega _{\Lambda ,2}^+$ . Cross-hatching indicates non-allowed regions. The vertical axis corresponds to $\Omega _{\Lambda ,2}$ and the horizontal axis to m.
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In the text

$\begin{figure} \par\includegraphics[width=12.1cm,clip]{0256fig5.eps}\end{figure}$ Figure 5: Total bounds on $\Omega _{\Lambda ,2}$ given by the observations. The left panel gives the limit on $\Omega _{\Lambda ,2}^-$ and the right panels is relative to $\Omega _{\Lambda ,2}^+$ . The black area represents the excluded regions. The vertical axis corresponds to $\Omega _{\Lambda ,2}$ and the horizontal axis to m.
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In the text

$\begin{figure} \par\includegraphics[width=11.4cm,clip]{0256fig6.eps}\end{figure}$ Figure 6: Ratio of temperatures between a ${\Lambda }$ -run and the standard case $\Omega _{\Lambda }=\rm constant$ . Bold curves represent the ratio of radiation temperatures, dotted curves is the ratio of matter temperatures.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{0256fig1.eps}\end{figure}$	Figure 1: Evolution of the radiation temperature for different decaying ${\Lambda }$ -cosmologies.
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$\begin{figure} \par\includegraphics[width=12.1cm,clip]{0256fig5.eps}\end{figure}$	Figure 5: Total bounds on $\Omega _{\Lambda ,2}$ given by the observations. The left panel gives the limit on $\Omega _{\Lambda ,2}^-$ and the right panels is relative to $\Omega _{\Lambda ,2}^+$ . The black area represents the excluded regions. The vertical axis corresponds to $\Omega _{\Lambda ,2}$ and the horizontal axis to m.
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$\begin{figure} \par\includegraphics[width=11.4cm,clip]{0256fig6.eps}\end{figure}$	Figure 6: Ratio of temperatures between a ${\Lambda }$ -run and the standard case $\Omega _{\Lambda }=\rm constant$ . Bold curves represent the ratio of radiation temperatures, dotted curves is the ratio of matter temperatures.
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