Central velocity dispersion in the globular cluster ω Centauri.

Details Central velocity dispersion in the globular cluster ω Centauri. Central velocity dispersion in the globular cluster ω Centauri.

Nov 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...303..761m&link_type=abstract

Astronomy and Astrophysics, v.303, p.761

Astronomy and Astrophysics

Astrophysics

89

Clusters: Globular, {Omega} Cen, Stars: Kinematics, Stellar Dynamics

Scientific paper

The mean radial velocities obtained with CORAVEL for 151 individual stars located in the center of the galactic globular cluster ω Centauri = NGC 5139 are combined with the previous measurements of 318 other stars to derive the velocity dispersion profile. It increases significantly from the outer parts inwards: the 16 outermost stars, located between 19.2' and 22.4' from the center, have a velocity dispersion σ_p_=5.1+/-1.6km/s, while the 16 innermost stars, located within 1' from the center, have a velocity dispersion σ_p_=21.9+/-3.9km/s. This inner value of about σ_p_(0)=22km/s is the largest velocity dispersion value obtained in the core of any galactic globular cluster and is significantly larger than the previous estimate, viz. σ_p_=16.7+/-1.9km/s (Meylan & Mayor 1986). A simultaneous fit of these radial velocities and of the surface brightness profile to a multi-mass King-Michie dynamical model provides mean estimates of the total mass equal to M_tot_=5.1x10^6^Msun_, with a corresponding mean mass-to-light ratio M/L_V_=4.1. The present results emphasize the fact that ω Centauri is not only the brightest but also, by far, the most massive galactic globular cluster.

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