Abstract
Several scenarios have been proposed to account for the formation and evolution of galactic bulges and to explain the variety of their observed properties. Both the intrinsic shape and dynamical structure of bulges depend on the mechanisms and timescales of their formation. We are deriving the intrinsic axial ratios of the bulges of a sample of unbarred lenticular galaxies to look for a possible relationship with their known orbital structure. Preliminary results show that the orbits of stars of the triaxial bulge of NGC 4476 are more anisotropic than those in the axisymmetric bulge of NGC 4249 hinting at a different formation process.
Highlights
Several formation scenarios were proposed to explain the variety of photometric, kinematic, dynamical, and stellar population properties observed in bulges of lenticular and spiral galaxies
We have found that the bulge of NGC 4249 is axisymmetric and almost spherical, whereas the bulge of NGC 4476 is triaxial and partially prolate
From the location of NGC 4249 and NGC 4476 in the (, V /σ) diagram, we conclude that the orbits of stars of the triaxial bulge of NGC 4476 are more anisotropic than those in the axisymmetric bulge of NGC 4249
Summary
1. Introduction Several formation scenarios were proposed to explain the variety of photometric, kinematic, dynamical, and stellar population properties observed in bulges of lenticular and spiral galaxies. We started a project to analyze the structural and dynamical properties of the bulges of a sample of unbarred lenticular galaxies in order to study the relationship between their intrinsic
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