Kinematic Evidence for an Old Stellar Halo in the Large Magellanic Cloud

Details Kinematic Evidence for an Old Stellar Halo in the Large Magellanic Cloud Kinematic Evidence for an Old Stellar Halo in the Large Magellanic Cloud

2003-09-12

arxiv.org/abs/astro-ph/0309351v1

Astronomy and Astrophysics

Astrophysics

8 pages, 2 figures; to be published in Science on Sept. 12, 2003

Scientific paper

10.1126/science.1088529

The oldest and most metal-poor Milky Way stars form a kinematically hot halo, which motivates the two major formation scenarios for our galaxy: extended hierarchical accretion and rapid collapse. RR Lyrae stars are excellent tracers of old and metal-poor populations. We measure the kinematics of 43 RR Lyrae stars in the inner regions of the nearby Large Magellanic Cloud (LMC) galaxy. The velocity dispersion, \sigma_{true}=53\pm10 km/s, indicates that a kinematically hot metal-poor old halo also exists in the LMC. This suggests that our galaxy and smaller late-type galaxies like the LMC have similar early formation histories.

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