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 ( [ 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 . In addition , all metal-rich clusters whose origins are related to the same protogalactic cloud are located in the [ Fe/H ] – [ \alpha /Fe ] diagram considerably higher than the strip populated with field stars . All metal-poor clusters ( most of them accreted ) populate the entire width of the strip formed by high-velocity ( i. e. , presumably accreted ) field stars . Stars of dwarf satellite galaxies ( all of them being metal-poor ) are located in this diagram much lower than accreted field stars . These facts suggest that all stellar objects in the accreted halo are remnants of galaxies with higher masses than those in the current environment of the Galaxy . Differences in the relative abundances of \alpha -process elements among stellar objects of the Galaxy and surrounding dwarf satellite galaxies confirm that the latter have left no appreciable stellar traces in the Galaxy , with the possible exception of the low-metallicity cluster Rup 106 , which has low relative abundances of \alpha -process elements .