IAU-FM6-- Angular momentum -- Conference summary

TL;DR

This conference summary discusses the importance of angular momentum in galaxy formation, highlighting recent observational advances and future prospects for understanding how galaxies acquire and evolve their angular momentum through various processes.

Contribution

It provides an overview of current knowledge on galaxy angular momentum, emphasizing the role of outer regions and upcoming observational opportunities.

Findings

Outer galaxy regions retain most of the angular momentum.

Recent IFU surveys have enriched kinematic data in the local universe.

Future observations will expand understanding at high redshift and in atomic gas.

Abstract

Angular momentum (AM) is a key parameter to understand galaxy formation and evolution. AM originates in tidal torques between proto-structures at turn around, and from this the specific AM is expected to scale as a power-law of slope 2/3 with mass. However, subsequent evolution re-shuffles this through matter accretion from filaments, mergers, star formation and feedback, secular evolution and AM exchange between baryons and dark matter. Outer parts of galaxies are essential to study since they retain most of the AM and the diagnostics of the evolution. Galaxy IFU surveys have recently provided a wealth of kinematical information in the local universe. In the future, we can expect more statistics in the outer parts, and evolution at high z, including atomic gas with SKA.