Kinematics of metal-poor giants in an inner-halo field, with implications for disk formation

Details Kinematics of metal-poor giants in an inner-halo field, with implications for disk formation Kinematics of metal-poor giants in an inner-halo field, with implications for disk formation

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aj....105..539m&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 105, no. 2, p. 539-556.

Astronomy and Astrophysics

Astronomy

32

Galactic Nuclei, Giant Stars, Kinematics, Metallicity, Stellar Structure, Milky Way Galaxy, Sky Surveys (Astronomy), Star Formation

Scientific paper

A sample of approximately 100 predominantly metal-weak giants, identified in a high-latitude field towards the galactic center using an automated objective-prism survey technique, is presented. Abundances and radial velocities have been measured for these giants, whose distances from the Sun range from 1 to 18 kpc. While the extremely metal-weak stars in the field have halo kinematics, the majority of the stars with intermediate abundance have thick disk kinematics, despite the fact that their average distance from the galactic plane is 3 kpc. The most satisfactory explanation for this effect is that the inner halo is moderately flattened, and the metal-weak stars of the thick disk have a scale height of about 2 kpc. It is suggested that the thick disk may have formed in a dissipational collapse, rather than in a separate event such as the accretion of a small satellite galaxy.

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