Figure 1: Trajectories for the extended PS process (Markovian process, jagged curves, T=0) and for the non-Markovian process (smooth curves, T=0.23). | |
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Figure 2: Filter profiles W_{T}(k) as a function of comoving wavenumber k in units of for three values of the T parameter ( left: T=0.00, middle: T=0.23, right: T=0.50). Each panel shows two groups of filters. Left group: filter radius , right group: . Each group consists of three filter curves. From up to down: n=0 (continuous), -1 (dotted) ,-2 (dashed). The normalization of the power spectrum P_{0} is adjusted to give (at T=0). | |
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Figure 3: Mass functions f(M) for Gaussian fluctuation fields with a power spectrum with n=0,-1,-2. Mass M in solar units: T=0, (dashed lines), and T=0.23, (continuous lines). The computations assume the normalized cosmic mass density , the standard normalization and the normalized Hubble constant h=0.7. | |
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Figure 4: Mass functions f(M) for Gaussian fluctuation fields with a power spectrum with n=-2.0. Mass M in solar units. T=0, (dashed line), and T=0.23, (continuous line). Further normalizations as in Fig. 3. | |
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Figure 5: Best fit mass function f(M) with T=0.23, (continuous line) and the transformed mass function of Jenkins et al. (2001) with 20% Gaussian random errors (dots with error bars). Normalizations as in Fig. 3. | |
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Figure 6: distribution ( contours for three parameters) for the spectral index n=-2 obtained from the comparison of mass functions f(M) with different T and parameter values and the transformed Jenkins et al. (2001) mass function. Normalizations as in Fig. 3. The test assumes errors of 30% ( left), 20% ( middle), 10% ( right) of the Jenkins et al. mass function. | |
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Figure 7: distribution ( contours for three parameters) in the plane, assuming 10% errors of the Jenkins et al. (2001) mass function. | |
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