Mapping the tilt of the Milky Way bulge velocity ellipsoids with ARGOS
  and $Gaia$ DR2
  Until the recent advent of $Gaia$ Data Release 2 (DR2) and deep multi-object
spectroscopy, it has been difficult to obtain 6-D phase space information for
large numbers of stars beyond 4 kpc, in particular towards the Galactic centre,
where dust and crowding effects are significant. In this study we combine
line-of-sight velocities from the Abundances and Radial velocity Galactic
Origins Survey (ARGOS) spectroscopic survey with proper motions from $Gaia$
DR2, to obtain a sample of $\sim$ 7,000 red clump stars with 3-D velocities. We
perform a large scale stellar kinematics study of the Milky Way (MW) bulge to
characterize the bulge velocity ellipsoids. We measure the tilt $l_{v}$ of the
major-axis of the velocity ellipsoid in the radial-longitudinal velocity plane
in 20 fields across the bulge. The tilt or vertex deviation, is characteristic
of non-axisymmetric systems and a significant tilt is a robust indicator of
non-axisymmetry or bar presence. We compare the observations to the predicted
kinematics of an N-body boxy-bulge model formed from dynamical instabilities.
In the model, the $l_{v}$ values are strongly correlated with the angle
($\alpha$) between the bulge major-axis and the Sun-Galactic centre
line-of-sight. We use a maximum likelihood method to obtain an independent
measurement of $\alpha$, from bulge stellar kinematics alone. The most likely
value of $\alpha$ given our model is $\alpha = (29 \pm 3)^{\circ}$. In the
Baade's window, the metal-rich stars display a larger vertex deviation ($l_{v}
= -40^{\circ}$) than the metal-poor stars ($l_{v} = 10^{\circ}$) but we do not
detect significant $l_{v}-$metallicity trends in the other fields.
