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What does the Dynamical Analsis of Clusters of Galaxies Tell us About Massive Neutrinos?

Published online by Cambridge University Press:  04 August 2017

G. Des Forêts ,
D. Gerbal ,
G. Mathez ,
A. Mazure  and
E. Salvador-Solé
G. Des Forêts
Affiliation:
Observatoire de Meudon
D. Gerbal
Affiliation:
Observatoire de Meudon
G. Mathez
Affiliation:
Observatoire de Meudon
A. Mazure
Affiliation:
Observatoire de Meudon
E. Salvador-Solé
Affiliation:
Observatoire de Meudon Universidad de Barcelona

Extract

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It is often claimed that massive neutrinos (v's) can solve the “missing mass” problem, but it is not so clear in the particular case of clusters of galaxies (C.O.G.). Let us assume that the unseen matter is composed by massive v's only. If they are cosmological, the v's should obey Fermi-Dirac statistics with a density of ∼ 100 v/cm3/species. But if “relic,” the v's would be so slow (1) that they cannot exist in this form (because of the previous Jeans instability or because they are trapped in wells generated by baryonic matter). Since the time when the v's decoupled from the primeval mixture (T ∼ 3–1 MeV), the v's can be considered as a “gravitational plasma,” so that violent relaxation occurs in inhomogeneous systems, leading to a Lynden-Bell distribution defined by three parameters: ην (numerical density), Vv (r.m.s. velocity) and the v-mass, mv, all unknown. All three of these parameters are, in fact, necessary to define a state of v-matter.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 104: Early Evolution of the Universe and Its Present Structure , 1983 , pp. 321 - 323
Copyright
Copyright © Reidel 1983 

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