Abstract
We present a new statistical analysis of the large-scale stellar mass distribution in the Sloan Digital Sky Survey (data release 7). A set of volume-limited samples shows that the stellar mass of galaxies is concentrated in a range of galaxy luminosities that is very different from the range selected by the usual analysis of galaxy positions. Nevertheless, the two-point correlation function is a power-law with the usual exponent γ = 1.71 − 1.82 , which varies with luminosity. The mass concentration property allows us to make a meaningful analysis of the angular distribution of the full flux-limited sample. With this analysis, after suppressing the shot noise, we extend further the scaling range and thus obtain γ = 1.83 and a clustering length r 0 = 5.8 − 7.0 h − 1 Mpc . Fractional statistical moments of the coarse-grained stellar mass density exhibit multifractal scaling. Our results support a multifractal model with a transition to homogeneity at about 10 h − 1 Mpc .
Highlights
It is claimed that we are entering the era of precision cosmology, in which the fundamental parameters of the universe are known within a few percent precision and only remain to progressively refine them [1, 2]
We make here, following up on Gaite [15], a new statistical analysis of the large-scale structure, adding an important ingredient: the stellar masses of galaxies, that is to say, we study the large-scale distribution of stellar mass. e distribution of stellar mass in the SDSS has already been studied by Li and White [16], employing the projected correlation function w(rp), on scales rp < 30 h− 1Mpc
What we conclude from the analysis of VLS1 is that the statistical analysis of the stellar mass distribution in the SDSS DR7 by means of volume-limited samples is plagued with errors, especially, discreteness errors
Summary
We present a new statistical analysis of the large-scale stellar mass distribution in the Sloan Digital Sky Survey (data release 7). A set of volume-limited samples shows that the stellar mass of galaxies is concentrated in a range of galaxy luminosities that is very different from the range selected by the usual analysis of galaxy positions. E mass concentration property allows us to make a meaningful analysis of the angular distribution of the full flux-limited sample. The two-point correlation function is a power-law with the usual exponent c 1.71 − 1.82, which varies with luminosity. With this analysis, after suppressing the shot noise, we extend further the scaling range and obtain c 1.83 and a clustering length r0 5.8 − 7.0 h− 1Mpc. Fractional statistical moments of the coarse-grained stellar mass density exhibit multifractal scaling. Our results support a multifractal model with a transition to homogeneity at about 10h− 1 Mpc
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