Kinematics of the Late M Giants in Baade's Window

Details Kinematics of the Late M Giants in Baade's Window Kinematics of the Late M Giants in Baade's Window

Sep 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.246...54s&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 246, NO. 1/SEP1, P. 54, 1990

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74

Scientific paper

Radial velocities have been measured for an unbiased sample of 239 late-type M giants in the b = -4° Galactic Bulge window (Baade's Window). The velocity dispersion for the 225 stars with I ≥ -11.8 is 113+6-5 km s-1, similar to other bulge populations. Subdividing this group of stars in various ways does not alter this dispersion within the errors, and demonstrates that the late-M stars form a kinematically homogeneous group. The 14 stars with I < 11.8 have a significantly smaller velocity dispersion of 71+20-11 km s-1. Together with other evidence, this result is consistent with these bright stars being foreground objects in the outer bulge or disc. Kinematical evidence suggests that the bulge must have an appreciable flattening. Comparison of those stars having infrared photometry with model atmospheres for cool stars indicates that the late-M giants have a mean metallicity 0.5 dex greater than solar; a significant fraction have masses in the range 1.5-2.0 Msun.

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