Gclusters :: Bibliographic item "gc397"

Release 11.12 ("Hergest Ridge")

Gclusters :: Bibliographic item "gc397"

Article ID: gc397

Author Simmerer, J.; Feltzing, S.; Primas, F.

Title A study of the metal-rich, thick disk globular cluster NGC 5927. A stellar inventory
Journal Astronomy & Astrophysics, Volume 556, id.A58, 13 pp.
Year of publication 2013 (on gclusters from 2013-10-22 10:41:01 )

Abstract We present a list of 72 radial velocity member stars in the metal-rich globular cluster NGC 5927. The radial velocities are based on multiepoch, multifibre spectra. We identify 46 RGB/HB stars and 26 turn-off stars that are radial velocity members in the cluster. This cluster is situated quite close to the disk and hence fore- and/or background contamination, especially in the outskirts of the cluster, can be quite severe. Fortunately, the cluster has a radial velocity (we determine it to vr = -104.03 ± 5.03 km s-1) that sets it clearly apart from the bulk velocities of the surrounding, background, and foreground stellar populations. Hence, our identification of members is clean and we can quantify a 50% contamination when stars in the outer part of the cluster are selected solely based on position in the color-magnitude diagram as opposed to selections based on radial velocities.

Tags NGC 5927
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Article ID: gc397
Author	Simmerer, J.; Feltzing, S.; Primas, F.
Title	A study of the metal-rich, thick disk globular cluster NGC 5927. A stellar inventory
Journal	Astronomy & Astrophysics, Volume 556, id.A58, 13 pp.
Year of publication	2013 (on gclusters from 2013-10-22 10:41:01 )
Abstract	We present a list of 72 radial velocity member stars in the metal-rich globular cluster NGC 5927. The radial velocities are based on multiepoch, multifibre spectra. We identify 46 RGB/HB stars and 26 turn-off stars that are radial velocity members in the cluster. This cluster is situated quite close to the disk and hence fore- and/or background contamination, especially in the outskirts of the cluster, can be quite severe. Fortunately, the cluster has a radial velocity (we determine it to vr = -104.03 ± 5.03 km s-1) that sets it clearly apart from the bulk velocities of the surrounding, background, and foreground stellar populations. Hence, our identification of members is clean and we can quantify a 50% contamination when stars in the outer part of the cluster are selected solely based on position in the color-magnitude diagram as opposed to selections based on radial velocities.
Tags	NGC 5927