Globular Clusters of the Galaxy: Chemical Composition vs Kinematics
  A comprehensive statistical analysis of the relationship between the chemical
and spatially kinematic parameters of the globular clusters of the Galaxy has
been performed. The data of the author's compilation catalog contain
astrophysical parameters for 157 clusters and the relative abundances of
{\alpha}-elements for 69 clusters. For 121 clusters, the data are supplemented
by spatially kinematic parameters taken from the literature. The phenomenon of
reddening of horizontal branches of low-metal accreted globular clusters is
discussed. We consider the contradiction between the criteria for clusters to
belong to the subsystems of the thick disk and the halo in terms of chemical
and kinematic properties. It consists in the fact that, regardless of belonging
to the galactic subsystems by kinematics, almost all metallic ([Fe/H] >-1.0)
clusters are located close to the center and plane of the Galaxy, while among
the less metallic of both subsystems there are many distant ones. Differences
in the abundances of {\alpha}-elements in the stellar objects of the Galaxy and
the surrounding low-mass dwarf satellite galaxies confirm the well-known
conclusion that all globular clusters and field stars of the accreted halo are
remnants of galaxies of higher mass than the current environment of the Galaxy.
A possible exception is a distant low-metal cluster with low relative abundance
of {\alpha}-elements Rup 106.
