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Figure 1: The central area is the amplitude of the matter fluctuations expressed in term of versus the normalization of the mass temperature (Eq. (1)) for a flat model with . Grey areas are our one, two and three sigma level contours. Filled squares are from Vauclair et al. (2003), open squares are Pierpaoli et al. (2001), around and Pierpaoli et al. (2003), symbol is from Evrard et al. (2002), Triangle is from Seljak (2002), inverted triangles are from Viana et al. (2002) and Viana et al. (2003).

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In the text

Figure 2: The red line is the central value of which is the normalization of the mass temperature relation Eq. (1). The WMAP relation between H0 and has been used, as well as the constraint on the baryon content of the Universe. One and two uncertainties arising from uncertainty on ( ) are shown as blue and yellow areas. Horizontal areas correspond to estimations of from hydrostatic methods (light green) obtained by Roussel et al. (2000) and Markevitch (1998) and from numerical simulations (light blue) obtained from Bryan & Norman (1998) and Evrard et al. (1996).

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In the text

Figure 3: a) Top: the amplitude of matter fluctuations from clusters abundance using the mass-temperature relation found in the present analysis compared to the amplitude of matter fluctuations derived from CMB data (Grainge et al. 2003; Pearson et al. 2003; Ruhl et al. 2003; Kuo et al. 2004). The grey area corresponds to 1, 2, 3 contours on two parameters, dashed lines are contours on one parameter. The one and two sigma amplitudes obtained from an average of recent weak shear measurements are also shown as dashed regions (see text for references). b) Bottom: amplitude of matter fluctuations from CMB data versus optical thickness.

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In the text

	Figure 4: Constraints on and given by the combined analysis of CMB and Cluster data. The dark energy component has been set to 0.7 in a flat cosmology.
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In the text