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Type: Artigo de periódico
Title: 'Fundamental Plane'-like relations from collisionless stellar dynamics: a comparison of mergers and collapses
Author: Dantas, CC
Capelato, HV
Ribeiro, ALB
de Carvalho, RR
Abstract: We present a new set of dissipationless N -body simulations aiming to better understand the pure dynamical aspects of the 'Fundamental Plane' (FP) of elliptical galaxies. We have extended our previous hierarchical merger scheme by considering the Hernquist profile for the initial galaxy model. Two-component Hernquist galaxy models were also used to study the effect of massive dark haloes on the end-product characteristics. We have also performed new collapse simulations including initial spin. We found that the one-component Hernquist mergers give results similar to those found for the one-component King models, namely both were able to build up small scatter FP-like correlations with slopes consistent with what is found for the near-infrared FP of nearby galaxies. The two-component models also reproduce a FP-like correlation, but with a significantly steeper slope. This is in agreement with what has been found for elliptical galaxies at higher redshift (0.1<z<0.6). We discuss some structural properties of the simulated galaxies and their ability to build up FP-like correlations. We confirm that collapses generally do not follow a FP-like correlation regardless of the initial spin. We suggest that the evolution of gradients in the gravitational field of the merging galaxies may be the main ingredient dictating the final non-homology property of the end products.
Subject: methods : N-body simulations
methods : numerical
galaxies : elliptical and lenticular, cD
galaxies : fundamental parameters
Country: Inglaterra
Editor: Blackwell Publishing Ltd
Citation: Monthly Notices Of The Royal Astronomical Society. Blackwell Publishing Ltd, v. 340, n. 2, n. 398, n. 410, 2003.
Rights: aberto
Identifier DOI: 10.1046/j.1365-8711.2003.06272.x
Date Issue: 2003
Appears in Collections:Unicamp - Artigos e Outros Documentos

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