# Three-Component Kinematics of Multiple Stellar Populations in Globular Clusters with Gaia and VLT

## TL;DR

This study investigates the kinematics of multiple stellar populations in seven globular clusters using Gaia and VLT data, revealing rotation patterns and differences between populations that inform cluster formation theories.

## Contribution

It combines Gaia DR2 proper motions with VLT radial velocities to analyze the 3D kinematics of multiple populations in seven globular clusters, highlighting rotation and anisotropy differences.

## Key findings

- NGC 0104 and NGC 5904 show significant rotation.
- First- and second-population stars exhibit similar rotation in NGC 0104.
- 2P stars in NGC 0104 are more anisotropic than 1P.

## Abstract

The internal dynamics of multiple stellar populations in Globular Clusters (GCs) provides unique constraints on the physical processes responsible for their formation. Specifically, the present-day kinematics of cluster stars, such as rotation and velocity-dispersion, could be related to the initial configuration of the system. In recent work, we provided the first study of the kinematics of different stellar populations in NGC$\,$0104 over a large field of view in the plane of the sky, exploiting Gaia Data Release 2 (DR2) proper motions combined with multi-band ground-based photometry. In this paper, we combine Gaia DR2 proper motions with Very Large Telescope radial velocities to investigate the kinematics along the line of sight and in the plane of the sky of multiple populations in seven GCs, namely NGC$\,$0104, NGC$\,$0288, NGC$\,$5904, NGC$\,$6121, NGC$\,$6254, NGC$\,$6752 and NGC$\,$6838. Among the analyzed clusters only NGC$\,$0104 and NGC$\,$5904 show significant rotation. Separating our sample into two groups of first- and second-population stars (1P and 2P) we find that overall these two populations exhibit a similar rotation pattern in NGC$\,$0104. However, some hints of different rotation are observed in the external regions of this cluster. Interestingly, 1P and 2P stars in NGC$\,$5904 show different rotation curves, with distinct phases and such difference is significant at the $\sim$2.5-$\sigma$ level. The analysis of the velocity-dispersion profiles of multiple populations confirms that 2P stars of NGC$\,$0104 show stronger anisotropy than the 1P.