  The velocity distribution of stars in the Solar neighbourhood is
inhomogeneous and rich with stellar streams and kinematic structures. These may
retain important clues of the formation and dynamical history of the Milky Way.
However, the nature and origin of many of the streams and structures is
unclear, hindering our understanding of how the Milky Way formed and evolved.
We aim to study the velocity distribution of stars of the Solar neighbourhood
and investigate the properties of individual kinematic structures in order to
improve our understanding of their origins.
  Using the astrometric data provided by Gaia DR1/TGAS and radial velocities
from RAVE DR5 we perform a wavelet analysis with the `a trous algorithm to
55831 stars that have U and V velocity uncertainties less than 4 km/s. An
auto-convolution histogram method is used to filter the output data, and we
then run Monte Carlo simulations to verify that the detected structures are
real due to velocity uncertainties. Additionally we analysed our stellar sample
by splitting all stars into a nearby sample (<300 pc) and a distant sample
(>300 pc), and two chemically defined samples that to a first degree represent
the thin and the thick disks.
  With the much enlarged stellar sample and much increased precision in
distances, proper motions, provided by Gaia DR1 TGAS we have shown that the
velocity distribution of stars in the Solar neighbourhood contains more
structures than previously known. A new feature is discovered and three
recently detected groups are confirmed at high confidence level. Dividing the
sample based on distance and/or metallicity shows that there are variety of
structures which are as large-scale and small-scale groups, some of them have
clear trends on metallicities, others are a mixture of both disk stars and
based on that we discuss possible origin of each group.
