Core velocity dispersions for 25 Galactic and 10 old Magellanic globular clusters.

Details Core velocity dispersions for 25 Galactic and 10 old Magellanic globular clusters. Core velocity dispersions for 25 Galactic and 10 old Magellanic globular clusters.

Aug 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...324..505d&link_type=abstract

Astronomy and Astrophysics, v.324, p.505-522

Astronomy and Astrophysics

Astrophysics

49

(Galaxy:) Globular Clusters: General, Stars: Kinematics, Techniques: Radial Velocities, Galaxies: Star Clusters, Magellanic Clouds

Scientific paper

We present, for 25 Galactic and 10 old Magellanic globular clusters, projected velocity dispersion (σ_p_) measurements obtained by applying a cross-correlation technique to integrated-light spectra. In order to understand and estimate the statistical errors of these measurements due to small numbers of bright stars dominating the integrated light, we provide an extensive discussion based on detailed numerical simulations. These errors are smaller if the integration area is larger and/or the cluster concentration higher. The simulations show that measurements are reliable when the integrated light within the integration area is brighter than a given magnitude. The statistical errors on the σ_p_ measurements of Magellanic globular clusters are small because of a physically large integration area, whereas they can be important for measurements carried out over small central areas in Galactic clusters. The present observational results are used to outline a few characteristics of the globular cluster fundamental plane. In this respect, the old Magellanic globular clusters appear similar to the Galactic clusters.

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