  Circa 10 billion years ago the Milky Way merged with a massive satellite,
Gaia-Enceladus. To gain insight into the properties of its debris we analyse in
detail the suite of simulations from Villalobos & Helmi (2008), which includes
an experiment that produces a good match to the kinematics of nearby halo stars
inferred from Gaia data. We compare the kinematic distributions of stellar
particles in the simulations and study the distribution of debris in orbital
angular momentum, eccentricity and energy, and its relation to the mass-loss
history of the simulated satellite. We confirm that Gaia-Enceladus probably
fell in on a retrograde, 30$^\circ$ inclination orbit. We find that while 75%
of the debris in our preferred simulation has large eccentricity ($> 0.8$),
roughly 9% has eccentricity smaller than 0.6. Star particles lost early have
large retrograde motions, and a subset of these have low eccentricity. Such
stars would be expected to have lower metallicities as they stem from the
outskirts of the satellite, and hence naively they could be confused with
debris associated with a separate system. These considerations seem to apply to
some of the stars from the postulated Sequoia galaxy. When a massive discy
galaxy merges, it leaves behind debris with a complex phase-space structure, a
large range of orbital properties, and a range of chemical abundances.
Observationally, this results in substructures with very different properties,
which can be misinterpreted as implying independent progeny. Detailed chemical
abundances of large samples of stars and tailored hydrodynamical simulations
are critical to resolving such conundrums.
