In the past years a wealth of observations has allowed us to unravel the structural properties of the Dark and Luminous mass distribution in spirals. As result, it has been found that their rotation curves follow, out their virial radius, an Universal function (URC) made by two terms: one due to the gravitational potential of a Freeman stellar disk and the other due to that of a dark halo. The importance of the latter is found to decrease with galaxy mass. Individual objects reveal in detail that dark halos have a density core, whose size correlates with its central value. These properties will guide CDM Cosmology to evolve to match the challenge that observations presently pose. © 2008 International Astronomical Union.

The mass distribution in spiral galaxies / Salucci, P.; Martins, C. F.. - 36(2009), pp. 133-140. ((Intervento presentato al convegno Dark energy and dark matter : observations, experiments and theories : Lyon, France, July 7-11, 2008 / tenutosi a Univ Lyon, Lyon, FRANCE nel July 7-11, 2008 [10.1051/eas/0936018].

The mass distribution in spiral galaxies

Salucci, P.;
2009

Abstract

In the past years a wealth of observations has allowed us to unravel the structural properties of the Dark and Luminous mass distribution in spirals. As result, it has been found that their rotation curves follow, out their virial radius, an Universal function (URC) made by two terms: one due to the gravitational potential of a Freeman stellar disk and the other due to that of a dark halo. The importance of the latter is found to decrease with galaxy mass. Individual objects reveal in detail that dark halos have a density core, whose size correlates with its central value. These properties will guide CDM Cosmology to evolve to match the challenge that observations presently pose. © 2008 International Astronomical Union.
Dark energy and dark matter : observations, experiments and theories : Lyon, France, July 7-11, 2008 /
36
133
140
978-2-7598-0439-9
https://arxiv.org/abs/0707.4370
EDP Sciences
Salucci, P.; Martins, C. F.
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/20.500.11767/15282
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