The stellar dynamics of omega centauri.
نویسندگان
چکیده
منابع مشابه
The Stellar Dynamics of ω Centauri
The stellar dynamics of ω Centauri are inferred from the radial velocities of 469 stars measured with CORAVEL (Mayor et al. 1997). Rather than fit the data to a family of models, we generate estimates of all dynamical functions nonparametrically, by direct operation on the data. The cluster is assumed to be oblate and edge-on but mass is not assumed to follow light. The mean motions are consist...
متن کاملThe Luminosity Function of Omega Centauri
Deep HST–WFPC2 observations of the stellar population in the globular cluster ωCen (NGC5139) have been used to measure the luminosity function of main sequence stars at the low-mass end. Two fields have been investigated, located respectively ∼ 4 . 6 and ∼ 7 away from the cluster center, or near the half-light radius of this cluster (rhl ≃ 4 ′ . 8). The color-magnitude diagrams derived from the...
متن کاملThe Chemical Evolution of Omega Centauri
The globular cluster ωCen is an outstanding object in terms of both its chemical and kinematic properties. Its large mass, spread in element abundances, chemical and kinematical segregations, as well as its peculiar orbit, all suggest that it is the surviving remnant of a larger system. In this contribution we deal with the chemical evolution of ωCen in the framework of a model where it is the ...
متن کاملOmega Centauri: the Population Puzzle Goes Deeper
We present HST observations that show a bifurcation of colors in the middle main sequence of the globular cluster ω Centauri. We see this in three different fields, observed with different cameras and filters. We also present high precision photometry of a central ACS field which shows a number of main-sequence turnoffs and subgiant branches. The double main sequence, the multiple turnoffs and ...
متن کاملON omega CENTAURI AND ITS RRc STARS
Masses, temperatures, and absolute luminosities are proposed for a large sample of RRc stars in the globular cluster w Centauri. Our technique uses three observed quantities: period, relative luminosity, and Fourier phase CP31' interpreting them in the light of linear and hydrodynamic pulsation models. The masses we obtain agree with those of the RRd stars in other clusters, and our derived par...
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ژورنال
عنوان ژورنال: The Astronomical Journal
سال: 1997
ISSN: 0004-6256
DOI: 10.1086/118538