Secular evolution and the assembly of bulges

Abstract

Bulges are of different types, morphologies and kinematics, from pseudo-bulges, close to disk properties (Sersic index, rotation fraction, flatenning), to classical de Vaucouleurs bulges, close to elliptical galaxies. Secular evolution and bar development can give rise to pseudo-bulges. To ensure prolonged secular evolution, gas flows are required along the galaxy life-time. There is growing evidence for cold gas accretion around spiral galaxies. This can explain the bar cycle of destruction and reformation, together with pseudo-bulge formation. However, bulges can also be formed through major mergers, minor mergers, and massive clumps early in the galaxy evolution. Bulge formation is so efficient that it is difficult to explain the presence of bulgeless galaxies today.

arXiv comment8 pages, 5 figures, invited review in "Galaxy Evolution: Emerging Insights and Future Challenges", S. Jogee, L. Hao, G. Blanc, I. Marinova, eds

References in corpus (3)

• On The Survival and Abundance of Disk-dominated Galaxies
• The Impact of Mergers on the Survival and Abundance of Disk-Dominated Galaxies
• Pattern speed evolution and bar reformation

Cited by in corpus (4)

• Galaxy Zoo: Morphological Classifications for 120,000 Galaxies in HST Legacy Imaging
• The build-up of pseudobulges in a hierarchical universe
• Galaxy Structural Analysis with the Curvature of the Brightness Profile
• Saying Hallo to M94's Stellar Halo: Investigating the Accretion History of the Largest Pseudobulge Host in the Local Universe