We use Fabry-Pérot absorption line imaging spectroscopy to measure radial velocities using the Ca ii \lambda 8542 line in 3360 stars towards three lines of sight in the Milky Way ’ s bar : Baade ’ s Window and offset position at ( l,b ) \simeq ( \pm 5.0 , -3.5 ) \arcdeg .
This sample includes 2488 bar red clump giants , 339 bar M/K-giants , and 318 disk main sequence stars .
We measure the first four moments of the stellar velocity distribution of the red clump giants , and find it to be symmetric and flat-topped .
We also measure the line-of-sight average velocity and dispersion of the red clump giants as a function of distance in the bar .
We detect stellar streams at the near and far side of the bar with velocity difference \gtrsim 30 km s ^ { -1 } at l = \pm 5 ° , but we do not detect two separate streams in Baade ’ s Window .
Our M-giants kinematics agree well with previous studies , but have dispersions systematically lower than those of the red clump giants by \sim 10 km s ^ { -1 } .
For the disk main sequence stars we measure a velocity dispersion of \sim 45 km s ^ { -1 } for all three lines-of-sight , placing a majority of them in the thin disk within 3.5 kpc of the Sun , associated with the Sagittarius spiral arm .
We measure the equivalent widths of the Ca ii \lambda 8542 line that can be used to infer metallicities .
We find indications of a metallicity gradient with Galactic longitude , with greater metallicity in Baade ’ s Window .
We find the bulge to be metal-rich , consistent with some previous studies .