Kinematics of the old open cluster system

Details Kinematics of the old open cluster system Kinematics of the old open cluster system

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aj....109.1706s&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 109, no. 4, p. 1706-1715

Astronomy and Astrophysics

Astronomy

50

Disk Galaxies, Galactic Rotation, Giant Stars, Kinematics, Late Stars, Milky Way Galaxy, Open Clusters, Radial Velocity, Astronomical Observatories, Astronomical Spectroscopy, Cross Correlation, Spectrographs

Scientific paper

Radial velocities accurate to 15 km/s or better were determined for 11 open clusters older than approximately 1 GYR and distributed over a range of positions in the galaxy. Moderate resolution spectra of an average of 30 stars in each cluster of varying spectral types were obtained using the 4.0 m telescope at Kitt Peak National Observatory (KPNO) and the Hydra multi-object spectrograph. The radial velocities were calculated for the late type giants in each cluster using cross correlation techniques; and mean velocity values were obtained for five clusters with no previous radial velocity measurements: Be 17, Be 31, Be 32, King 5, and King 11. Using these data, along with published velocities for an additional 24 clusters, the mean difference between the velocities of the open clusters and those predicted by a standared rotation curve is 1 +/- 29 km/s. Also, assuming that the old open cluster system rotates about the Galactic center with a constant rotation velocity, this velocity is found to be 21 +/- 7 km/s with a line-of-sight dispersion of 28 km/s. Both of these results imply that the old open clusters are predominantly a thin disk population. Be 17, the oldest cluster in this sample, also exhibits peculiar kinematics, and is discussed in particular.

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