The formation and evolution of tidal dwarf galaxies

在分级结构形成的情况下，今天的星系是由更小的、富含气体的物体积累而来的，这些物体是宇宙学的“积木”。由于角动量和能量守恒的结果，当两个这样的积木合并时，细长的富含气体的潮汐臂被驱逐出去。在一定条件下，这些潮汐臂可以分裂成一系列自重的矮星系。据估计，潮汐矮小星系(TDGs)的产生在早期宇宙中可能比今天更有效，因此TDGs可能对星系光度函数的暗端做出了重要贡献。这一建议旨在研究TDGs的形成效率与相互作用星系的气体分数、相互作用形态和质量比之间的关系。我们还旨在研究TDG的化学动力学历史，以了解它们的存活情况，并揭示有助于将它们与丰富的冷暗物质亚晕区分开来的可观测特征。

Within the hierarchical structure formation scenario today’s galaxies emerge from the accumulation of smaller, gas-rich objects, the cosmological “building blocks”. As a result of angular momentum and energy conservation long, thin and gas-rich tidal arms are expelled when two such building blocks merge. These tidal arms can fragment into a series of self-gravitating dwarf galaxies under certain conditions. It is expected that the production of tidal-dwarf galaxies (TDGs) may have been much more efficient in the early universe than today, and so TDGs may form an important contribution to the faint-end of the galaxy luminosity function. This proposal aims at investigating the efficiency of the formation of TDGs in dependence of the gas fraction, the interaction morphology and mass ratio of the interacting galaxies. We also aim at studying the chemodynamical history of TDGs, in order to understand their survival and to uncover observable features that would help distinguishing them from the abundant cold-dark-matter sub-halos.