Hierarchical Star Formation: Stars and Stellar Clusters in the Gould Belt

TL;DR

This study analyzes the spatial and kinematic distribution of young open clusters in the Gould Belt, revealing differences in cluster content and dynamics between regions, and proposing a larger complex origin within the Galactic disk.

Contribution

It provides a detailed classification of clusters in the Gould Belt and links their properties to their positions within the Local Arm, offering new insights into local star formation structures.

Findings

Ori OB1 is rich in open clusters, Sco OB2 has few or none.

Clusters are more abundant in Ori OB1's kinematic region.

The Gould Belt may be part of a larger star cluster complex in the Local Arm.

Abstract

We perform a study of the spatial and kinematical distribution of young open clusters in the solar neighborhood, discerning between bound clusters and transient stellar condensations within our sample. Then, we discriminate between Gould Belt (GB) and local Galactic disk (LGD) members, using a previous estimate of the structural parameters of both systems obtained from a sample of O-B6 Hipparcos stars. Using this classified sample we analyze the spatial structure and the kinematic behavior of the cluster system in the GB. The two star formation regions that dominate and give the GB its characteristic inclined shape show a striking difference in their content of star clusters: while Ori OB1 is richly populated by open clusters, not a single one can be found within the boundaries of Sco OB2. This is mirrored in the velocity space, translating again into an abundance of clusters in the region of the kinematic space populated by the members of Ori OB1, and a marginal number of them associated to Sco OB2. In the light of these results we study the nature of the GB with respect to the optical segment of the Orion Arm, and we propose that the different content of star clusters, the different heights over the Galactic plane and the different residual velocities of Ori OB1 and Sco OB2 can be explained in terms of their relative position to the density maximum of the Local Arm in the solar neighborhood. Although morphologically intriguing, the GB appears to be the result of our local and biased view of a larger star cluster complex in the Local Arm, that could be explained by the internal dynamics of the Galactic disk.