Structure in the motions of the fastest halo stars

Details Structure in the motions of the fastest halo stars Structure in the motions of the fastest halo stars

Aug 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005a%26a...439..551r&link_type=abstract

Astronomy and Astrophysics, Volume 439, Issue 2, August IV 2005, pp.551-558

Astronomy and Astrophysics

Astrophysics

12

Galaxy: Formation, Galaxy: Halo, Galaxy: Kinematics And Dynamics

Scientific paper

We analyzed the catalog published by Beers et al. (2000, ApJ, 119, 2866) of 2106 non-kinematically selected metal poor stars in the solar neighborhood, with the goal of quantifying the amount of substructure in the motions of the fastest halo stars. We computed the two-point velocity correlation function for a subsample of halo stars within 1-2 kpc of the Sun, and found statistical evidence of substructure with a similar amplitude to that predicted by high resolution CDM simulations. The signal is due to a small kinematic group whose dynamical properties are compared to the stellar "stream" previously discovered by Helmi et al. (1999). If real, this high velocity moving group would provide further support for the idea that substructures remain as fossils from the formation of the Galaxy as expected in the CDM scenario.

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