Kinematic Structure of the Galactic Center S-cluster
  We present a detailed analysis of the kinematics of 112 stars that mostly
comprise the high velocity S-cluster and orbit the super massive black hole
SgrA* at the center of the Milky Way. For 39 of them orbital elements are
known, for the remainder we know proper motions. The distribution of
inclinations, and proper motion flight directions deviate significantly from a
uniform distribution which one expects if the orientation of the orbits are
random. Across the central arcseconds the S-cluster stars are arranged in two
almost edge on disks that are located at a position angle approximately +-45 o
with respect to the Galactic plane. The angular momentum vectors for stars in
each disk point in both directions, i.e. the stars in a given disk rotate in
opposite ways. The poles of this structure are located only about 25 o from the
line of sight. This structure may be the result of a resonance process that
started with the formation of the young B-dwarf stars in the cluster about 6
Myr ago. Alternatively, it indicated the presence of a disturber at a distance
from the center comparable to the distance of the compact stellar association
IRS13.
