Mapping the tilt of the Milky Way bulge velocity ellipsoids with ARGOS and $Gaia$ DR2

Abstract

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 ($\hat{I}\pm$) 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 $\hat{I}\pm$, from bulge stellar kinematics alone. The most likely value of $\hat{I}\pm$ given our model is $\hat{I}\pm =(29\pm 3{)}^{\circ }$. 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.

13 pages, 11 figures