Abstract
We want to show here that the distribution of galaxies in space may be described in terms of a self-similar arrangement of the clustering on scales of distances ranging from some Mpc to (30 – 40)h −1 Mpc. To this end, the classical two-point correlation function has been evaluated both in the angular and the spatial case on the Zwicky and Cfal catalogues, respectively. In contrast to previous works, the quantity 1 + w(θ) and its spatial equivalent 1 + ξ(r) have been analysed with respect to their scaling properties with the sample depth. We have not studied the local scaling properties of the distribution (multifractality) and have approximated it to a simple fractal set. The resulting estimate for the fractal dimension (or better, the correlation dimension) is D 2 ≈ 1.7 from angular data, while D 2 ≈ 2.3 from the spatial ones. If this value is confirmed, the clustering in the galaxy distribution results to be less strong, but more extended in space, than previously found.
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Calzetti, D., Giavalisco, M. (1991). Is the Spatial Distribution of Galaxies a Bounded Self—Similar Structure? Observational Evidences. In: Heck, A., Perdang, J.M. (eds) Applying Fractals in Astronomy. Lecture Notes in Physics Monographs, vol 3. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-47582-8_5
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