Absolute proper motions to B approximately 22.5: Evidence for kimematical substructure in halo field stars

Details Absolute proper motions to B approximately 22.5: Evidence for kimematical substructure in halo field stars Absolute proper motions to B approximately 22.5: Evidence for kimematical substructure in halo field stars

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...427l..37m&link_type=abstract

Astrophysical Journal, Part 2 - Letters, vol. 427, no. 1, p. L37-L41

Astronomy and Astrophysics

Astrophysics

67

Astronomical Models, Astrophysics, Galactic Evolution, Galactic Halos, Galactic Structure, Kinematics, Radial Velocity, Star Formation, Stellar Motions, Astronomical Observatories, Data Reduction, Spectroscopic Telescopes, Stellar Parallax

Scientific paper

Radial velocities have been obtained for six of nine stars identified on the basis of similar distances and common, extreme transverse velocities in the proper motion survey of Majewski (1992) as a candidate halo moving group at the north Galactic pole. These radial velocities correspond to velocities perpendicular to the Galactic plane which span the range -48 +/- 21 to -128 +/- 9 km/sec (but a smaller range, -48 +/- 21 to -86 +/- 19 km/sec, when only our own measurements are considered), significantly different than the expected distribution, with mean 0 km/sec, for a random sample of either halo or thick disk stars. The probability of picking such a set of radial velocities at random is less than 1%. Thus the radial velocity data support the hypothesis that these stars constitute part of a halo moving group or star stream at a distance of approximately 4-5 kpc above the Galactic plane. If real, this moving group is evidence for halo phase space substructure which may be the fossil remains of a destroyed globular cluster, Galactic satellite, or Searle & Zinn (1978) 'fragment.'

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