Spatial Distribution of Globular Clusters in the Galaxy
  The Milky Way's satellite galaxies and Globular Clusters (GCs) are known to
exhibit an anisotropic spatial distribution. We examine in detail this
anisotropy by the means of the inertia tensor. We estimate the statistical
significance of the results by repeating this analysis for random catalogues
which use the radial distribution of the real sample. Our method reproduces the
well-known planar structure in the distribution of the satellite galaxies. We
show that for GCs several anisotropic structures are observed. The GCs at small
distances, $2<R<10$ kpc, show a structure coplanar with the Galactic plane. At
smaller and larger distances the whole sample of GCs shows quite weak
anisotropy. Nevertheless, at largest distances the orientation of the structure
is close to that of the satellite galaxies, i.e. perpendicular to the Galactic
plane. We estimate the probability of random realization for this structure of
1.7%. The Bulge-Disk GCs show a clear disk-like structure lying within the
galactic disk. The Old Halo GCs show two structures: a well pronounced polar
elongated structure at $R<3$ kpc which is perpendicular to the galactic plane,
and a less pronounced disk-like structure coplanar with the galactic disk at
$6<R<20$ kpc. The Young Halo GCs do not show significant anisotropy.
