Detection of a radial velocity gradient in the extended local disc with RAVE

TL;DR

This study detects a radial velocity gradient in the local Galactic disc using RAVE survey data, indicating non-axisymmetric features like the bar or spiral arms influence stellar motions.

Contribution

It presents a new method to identify the velocity gradient in the Galactic disc independent of proper motions and Galactic parameters.

Findings

Detected a velocity gradient |K+C| < 3 km/s/kpc in the Galactic disc.

Reconstructed 2D velocity maps using different proper motions and distances.

Results suggest non-axisymmetric structures affect stellar velocities.

Abstract

Using a sample of 213,713 stars from the Radial Velocity Experiment (RAVE) survey, limited to a distance of 2 kpc from the Sun and to |z|<1 kpc, we report the detection of a velocity gradient of disc stars in the fourth quadrant, directed radially from the Galactic centre. In the direction of the Galactic centre, we apply a simple method independent of stellar proper motions and of Galactic parameters to assess the existence of this gradient in the RAVE data. This velocity gradient corresponds to |K+C| < 3 km/s/kpc, where K and C are the Oort constants measuring the local divergence and radial shear of the velocity field, respectively. In order to illustrate the effect, assuming a zero radial velocity of the Local Standard of Rest we then reconstruct the two-dimensional Galactocentric velocity maps using two different sets of proper motions and photometric distances based either on isochrone fitting or on K-band magnitudes, and considering two sets of values for the Galactocentric radius of the Sun and local circular speed. Further observational confirmation of our finding with line-of-sight velocities of stars at low latitudes, together with further modelling, should help constrain the non-axisymmetric components of the Galactic potential, including the bar, the spiral arms and possibly the ellipticity of the dark halo.