Abstract
In 1924 Hubble presented the first generally convincing evidence, from the identification of variable stars, that some of the brightest “spiral nebulae” are galaxies of stars well outside the bounds of our own Galaxy. This led him to reconsider the idea that the faint “spiral nebulae,” which were known to be much more abundant than bright ones, might be similar objects at greater distances. If the galaxies were uniformly distributed through space the number brighter than apparent magnitude m would vary as
Hubble (1926) tested this relation with the data shown in figure 1. The point at the extreme right hand side is based on Fath’s (1914) counts of nebulae with diameters greater than ~ 4”. The straight line shows the slope expected under the homogeneity assumption. The agreement is very encouraging, though, as we now recognize, it must be in part fortuitous because the counts at m ≲ 12 are influenced by the concentration of galaxies in and around the Virgo cluster, that is, the Local Supercluster, and also in the Local Group.
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Peebles, P.J.E., Grishchuk, L. (1978). Large Scale Clustering in the Universe. In: Longair, M.S., Einasto, J. (eds) The Large Scale Structure of the Universe. International Astronomical Union / Union Astronomique Internationale, vol 79. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-9843-8_23
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DOI: https://doi.org/10.1007/978-94-009-9843-8_23
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