H. Aceves and H. Velázquez
Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 877, 22800 Ensenada, B. C., México (aceves@astrosen.unam.mx; hmv@astrosen.unam.mx).
Received 2005 May 27
Accepted 2005 November 7
]]> RESUMEN
Se efectuaron tres simulaciones auto-consistentes de N-cuerpos de fusiones entre galaxias, con un perfil pronunciado de materia oscura, para estudiar si la pendiente interna del perfil de densidad oscura se preserva en los remanentes. En estas simulaciones los progenitores incluyen un disco estelar y un espín intrínseco en el halo a diferencia de estudios similares. La razón de masas de las galaxias progenitoras es de alrededor de 1:1, 1:3 y 1:10. Encontramos que el perfil de densidad inicial pronunciado de los halos oscuros se preserva en los remanentes para los casos considerados aquí.
ABSTRACT
We carried out three self-consistent N-body simulations of galaxy mergers, with a cuspy dark matter profile, in order to study if the inner dark density slope is preserved in the remnants. In these simulations the progenitors include both a stellar disk and an intrinsic angular momentum for the halos, unlike previous similar studies. The mass-ratios of progenitor galaxies are about 1:1, 1:3, and 1:10. We find that the initial cuspy density profile of the dark halos is preserved in the remnants for the cases considered here.
Key Words: GALAXIES: INTERACTIONS — GALAXIES: KINEMATICS AND DYNAMICS — METHODS: N-BODY SIMULATIONS.
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ACKNOWLEDGEMENTS
]]> We thank CONACyT, Mexico, for financial support through Project 37506-E. An anonymous referee is thanked for providing important comments that helped to improve the presentation of this work.
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