# Kinematic Decoupling of Globular Clusters with Extended Horizontal-Branch

## TL;DR

This study reveals that globular clusters with extended horizontal-branch stars are more massive, kinematically distinct, and likely have different origins compared to normal clusters, shedding light on the Milky Way's formation history.

## Contribution

It demonstrates the kinematic and mass differences of GCs with extended HB, suggesting heterogeneous origins and providing insights into galaxy formation processes.

## Key findings

- Extended HB GCs are more massive than normal GCs.
- Extended HB GCs are dominated by random motion with no metallicity correlation.
- Normal GCs in the outer halo share properties with extended HB GCs, indicating accretion origins.

## Abstract

About 25% of the Milky Way globular clusters (GCs) exhibit unusually extended color distribution of stars in the horizontal-branch (HB) phase. This phenomenon is now best understood as due to the presence of helium enhanced second generation subpopulations, which has raised a possibility that these peculiar GCs might have a unique origin. Here we show that these GCs with extended HB are clearly distinct from other normal GCs in kinematics and mass. The GCs with extended HB are more massive than normal GCs, and are dominated by random motion with no correlation between kinematics and metallicity. Surprisingly, however, when they are excluded, most normal GCs in the inner halo show clear signs of dissipational collapse that apparently led to the formation of the disk. Normal GCs in the outer halo share their kinematic properties with the extended HB GCs, which is consistent with the accretion origin. Our result further suggests heterogeneous origins of GCs, and we anticipate this to be a starting point for more detailed investigations of Milky Way formation, including early mergers, collapse, and later accretion.