# The Chemical Composition of Globular Clusters of Different Nature in our Galaxy

## TL;DR

This study compiles a comprehensive catalog of 157 Galactic globular clusters, analyzing their chemical and kinematic properties to understand their origins and classifications within the Galaxy.

## Contribution

It provides an extensive dataset combining chemical abundances, kinematic data, and morphological indices, and discusses the relationships and discrepancies among cluster properties and Galactic subsystems.

## Key findings

- Metal-rich clusters are located near the Galaxy center and plane.
- Accreted clusters show distinct chemical and kinematic properties.
- Distant, metal-poor clusters are prevalent in various Galactic subsystems.

## Abstract

A catalog of Galactic globular clusters has been compiled and used to analyze relations between the chemical and kinematic parameters of the clusters. The catalog contains positions, distances, luminosities, metallicites, and horizontal-branch morphology indices for 157~globular clusters, as well as space velocities for 72~globular clusters. For 69~globular clusters, these data are suppleented with the relative abundances of 28~chemical elements produced in various nuclear-synthesis processes, taken from 101~papers published between 1986 and 2018. The tendency for redder horizontal branches in low-metallicity accreted globular clusters is discussed. The discrepancy between the criteria for cluster membership in the thick-disk and halo subsystems based on chemical and kinematic properties is considered. This is manifest through the fact that all metal-rich ($\rm{[Fe/H]} > -1.0$) clusters are located close to the center and plane of the Galaxy, regardless of their kinematic membership in particular Galaxy subsystems. An exception is three accreted clusters lost by a dwarf galaxy in Sagittarius. At the same time, the fraction of more distant clusters is high among metal-poorer clusters in any kinematically selected Galactic subsystem.