Proper-Motion Anisotropy, Rotation, and the Shape of the Galactic Bulge

Details Proper-Motion Anisotropy, Rotation, and the Shape of the Galactic Bulge Proper-Motion Anisotropy, Rotation, and the Shape of the Galactic Bulge

Oct 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...470..506z&link_type=abstract

Astrophysical Journal v.470, p.506

Astronomy and Astrophysics

Astronomy

15

Galaxy: Kinematics And Dynamics, Galaxy: Structure, Stars: Late-Type

Scientific paper

We explain the apparent proper-motion anisotropy σl/σb = 1.15±0.06 at Baade's window (l, b) = (1°, -4°) observed by Spaenhauer, Jones, & Whitford by rotation broadening in the longitude direction. We find that the observed solid-body rotation rate of the bulge can account for the observed proper-motion anisotropy.
We find also that the sample is not homogeneous in kinematics. The M giants and the late-type and/or metal-rich K giants in the sample have a bigger apparent anisotropy σl/σb and smaller intrinsic dispersion σb than the whole sample. Also, σr > σb for the metal-rich stars. We show that these anisotropies are consistent with a rapidly rotating and intrinsically anisotropical bar in the center.

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