Topography of the Young Galactic Disk: Spatial and Kinematic Patterns of the Clustered Star Formation in the Solar Neighborhood

TL;DR

This study uses Gaia data and Kriging interpolation to map the 3D spatial and vertical velocity structure of young open clusters in the Solar neighborhood, revealing complex substructures and physical mechanisms shaping star formation in the Galactic disk.

Contribution

It applies Kriging to Gaia YOC data to map the Galactic disk's structure and analyze hierarchical star formation patterns with detailed spatial and kinematic maps.

Findings

Revealed complex disk structure with substructures and hierarchies.

Identified warp, corrugations, and deviations in Z and V_Z.

Connected physical mechanisms shaping star formation patterns.

Abstract

The accuracy in determining the spatial-kinematical parameters of open clusters makes them ideal tracers of the Galactic structure. Young open clusters (YOCs) are the main representative of the clustered star formation mode, which identifies how most of the stars in the Galaxy form. We apply the Kriging technique to a sample of Gaia YOCs within a 3.5 kpc radius around the Sun and log(age) $\leq$ 7.5, age in years, to obtain the $Z(X,Y)$ and $V_Z(X,Y)$ maps. The previous work by Alfaro et al. (1991) showed that Kriging can provide reliable results even with small data samples ($N \sim 100$). We approach the 3D spatial and vertical velocity field structure of the Galactic disk defined by YOCs and analyze the hierarchy of the stellar cluster formation, which shows a rich hierarchical structure, displaying complexes embedded within each other. We discuss the fundamental characteristics of the methodology used to perform the mapping and point out the main results obtained in phenomenological terms. Both the 3D spatial distribution and the vertical velocity field reveal a complex disk structure with a high degree of substructures. Their analysis provides clues about the main physical mechanisms that shape the phase space of the clustered star formation in this Galactic area. Warp, corrugations, and high local deviations in $Z$ and $V_Z$, appear intimately connected in a single but intricate scenario.