  Using a sample of 248 metal-poor stars (RR Lyraes, red giants and RHB stars)
which is remarkable for the accuracy of its 6-D kinematical data, we find a new
component for the local halo which has an axial ratio c/a ~ 0.2, a similar
flattening to the thick disk. It has a small prograde rotation but is supported
by velocity anisotropy, and contains more intermediate-metallicity stars (with
-1.5 < [Fe/H] < -1.0) than the rest of our sample. We suggest that this
component was formed quite late, during or after the formation of the disk. It
formed either from the gas that was accreted by the last major mergers
experienced by the Galaxy, or by dynamical friction of massive infalling
satellite(s) with the halo and possibly the stellar disk or thick disk. The
remainder of the stars in our sample exhibit a clumpy distribution in energy
and angular momentum, suggesting that the early, chaotic conditions under which
the inner halo formed were not violent enough to erase the record of their
origins. The clumpy structure suggests that a relatively small number of
progenitors were responsible for building up the inner halo, in line with
theoretical expectations. We find a difference in mean binding energy between
the RR Lyrae variables and the red giants in our sample, suggesting that more
of the RR Lyraes in the sample belong to the outer halo, and that the outer
halo may be somewhat younger, as first suggested by Searle and Zinn (1978). We
also find that the RR Lyrae mean rotation is more negative than the red giants,
which is consistent with the recent result of Carollo et al.(2007) that the
outer halo has a retrograde rotation and with the difference in kinematics seen
between RR Lyraes and BHB stars by Kinman et al.(2007).
