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All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0]{fig1.ps}} \par\end{figure}$ Figure 1: The temperature power spectrum for the best-fit power-law $\Lambda$ CDM model (dotted black line) from Spergel et al. (2003), and for our broken-power-law model with $\Omega _\Lambda = 0$ (solid blue line), compared to data from WMAP and others experiments at small scales - CBI (Pearson et al. 2003), ACBAR (Kuo et al. 2002), BOOMERanG (Ruhl et al. 2002) and VSA (Grainge et al. 2003). Note the linear scale in $\ell$ for $\ell > 200$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0]{plotlam8.eps}}\par\end{figure}$ Figure 2: Velocity versus luminosity-distance for type Ia supernovae (filled circles), S-Z clusters (open circles) and gravitational lens time-delay systems (filled triangles), with z>0.05. All curves shown correspond to flat models and are labelled with the Hubble parameter in km s^-1 Mpc^-1.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0]{zsig.ps}}\par \end{figure}$ Figure 3: CMB angular power spectra for models with $\Omega _{\rm m}= 1$ , H₀ = 46 km s^-1 Mpc^-1 and $\Omega _{\rm b}h^2 = 0.019$ normalised to $\sigma _8=1$ with different power law indices for the primordial fluctuations. Note the constancy of the amplitude around $\ell \sim 900$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0]{fig2.ps}}\par \end{figure}$ Figure 4: The temperature power spectrum for the best-fit power-law $\Lambda$ CDM model (dotted black line) from Spergel et al. (2003), and for our broken-power-law models (both having $\Omega _\Lambda = 0$ ) with $\Omega _\nu = 0.12$ (dot-dashed blue line) and $\Omega _{\rm\scriptscriptstyle Q}=0.12$ (solid green line), compared to data from WMAP and other experiments (Grainge et al. 2003; Pearson et al. 2003; Kuo et al. 2002; Ruhl et al. 2002).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0]{fig5.ps}}\par\resizebox{8.8cm}{!}{\includegraphics[angle=0]{fig6.ps}}\par \end{figure}$ Figure 5: The temperature-polarization (TE) cross power-spectrum and the polarization (EE) power spectrum for our E-deS models with $\Omega _\nu = 0.12$ (dot-dashed blue line) and $\Omega _{\rm\scriptscriptstyle Q}=0.12$ (solid green line), both with $\tau = 0.1$ , compared to the concordance $\Lambda$ CDM model (dotted line). The thin lines are obtained adopting the higher optical depth ( $\tau = 0.17$ ) suggested by the WMAP fit to the TE data (Kogut et al. 2003).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0]{fig3.ps}}\par\resizebox{8.8cm}{!}{\includegraphics[angle=0]{fig4.ps}}\par \end{figure}$ Figure 6: The power spectrum of large scale structure at z=0 and z=2.3 for our E-deS models with $\Omega _\nu = 0.12$ (dot-dashed blue lines) and $\Omega _{\rm\scriptscriptstyle Q}=0.12$ (solid green lines). The Lyman- $\alpha$ data have been shifted downwards by 20% (corresponding to the $1\sigma$ uncertainty in the calibration).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0]{plotlam8.eps}}\par\end{figure}$	Figure 2: Velocity versus luminosity-distance for type Ia supernovae (filled circles), S-Z clusters (open circles) and gravitational lens time-delay systems (filled triangles), with z>0.05. All curves shown correspond to flat models and are labelled with the Hubble parameter in km s^-1 Mpc^-1.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0]{zsig.ps}}\par \end{figure}$	Figure 3: CMB angular power spectra for models with $\Omega _{\rm m}= 1$ , H₀ = 46 km s^-1 Mpc^-1 and $\Omega _{\rm b}h^2 = 0.019$ normalised to $\sigma _8=1$ with different power law indices for the primordial fluctuations. Note the constancy of the amplitude around $\ell \sim 900$ .
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0]{fig3.ps}}\par\resizebox{8.8cm}{!}{\includegraphics[angle=0]{fig4.ps}}\par \end{figure}$	Figure 6: The power spectrum of large scale structure at z=0 and z=2.3 for our E-deS models with $\Omega _\nu = 0.12$ (dot-dashed blue lines) and $\Omega _{\rm\scriptscriptstyle Q}=0.12$ (solid green lines). The Lyman- $\alpha$ data have been shifted downwards by 20% (corresponding to the $1\sigma$ uncertainty in the calibration).
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