Abundance Patterns of the S Stars in ω Centauri

Vanture, Andrew D.; Wallerstein, George; Suntzeff, Nicholas B.

doi:10.1086/339427

Cited by 30 publications

(43 citation statements)

References 40 publications

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“…For example, according to the abundance analysis by Vanture et al (2002), ROA 300 (an RGB-a member) shows a substantially higher abundance of sprocess elements with respect to star ROA 201 (which is conversely an MInt member). If this kind of discontinuous behavior is confirmed, it will further support the hypothesis that the RGB-a population had a very different evolutionary and chemical history with respect to the other stars of q Cen.…”

Section: Discussionmentioning

confidence: 99%

Discovery of an Accreted Stellar System within the Globular Cluster ω Centauri

Ferraro

Bellazzini

Pancino

2002

The Astrophysical Journal

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Recent wide-field photometric surveys (Lee et al.; Pancino et al.) have shown the existence of a previously unknown metal-rich ( ) stellar population in the galactic globular cluster q Centauri. The discovery [Fe/H] Ӎ Ϫ0.6 of this new component, which comprises only a small percentage (∼5%) of the entire cluster population, has added a new piece to the already puzzling picture of the star formation and chemical evolution of this stellar system. In this Letter, we show that stars belonging to the newly discovered metal-rich population have a coherent bulk motion with respect to the other cluster stars, thus demonstrating that they formed in an independent selfgravitating stellar system. This is the first clear-cut evidence that extreme metal-rich stars were part of a small stellar system (a satellite of q Centauri?) that has been accreted by the main body of the cluster. In this case, we are witnessing an in vivo example of hierarchical merging on the subgalactic scale.

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Section: Discussionmentioning

confidence: 99%

Discovery of an Accreted Stellar System within the Globular Cluster ω Centauri

Ferraro

Bellazzini

Pancino

2002

The Astrophysical Journal

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“…We adopted ½/Fe ¼ þ0:3 for both the rMS and the bMS samples, according to the most recent high-resolution spectroscopic results (Norris & Da Costa 1995;Smith et al 2000;Vanture et al 2002). For the two MS components we computed a set of models with canonical helium abundance (Y ¼ 0:246; Salaris et al 2004) and various helium enhancement levels.…”

Section: Comparison With Theoretical Isochronesmentioning

confidence: 99%

Deep FORS1 Observations of the Double Main Sequence of ω Centauri

Sollima

Ferraro

Bellazzini

et al. 2007

ApJ

129

140

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We present the results of a deep photometric survey performed with the VLT FORS1 aimed at investigating the complex main-sequence structure of the stellar system ! Centauri. We confirm the presence of a double main sequence and identify its blue component (bMS) over a large field of view up to 26 0 from the cluster center. We found that bMS stars are significantly more concentrated toward the cluster center than the other ''normal'' MS stars. The bMS morphology and its position in the CMD have been used to constrain the helium overabundance required to explain the observed MS morphology.

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“…4) are wider than those of 47 Tuc and even that of ! Cen, which is well established to have a metal spread from [Fe/H] % À2.2 to [Fe/H] % À0.7 (Vanture, Wallerstein, & Suntzeff 2002). The latter result is somewhat surprising, given the fact that the metal-rich RGB of 47 Tuc provides a poor approximation of the metal-poor RGB of !…”

Section: No 4 2003mentioning

confidence: 99%

2MASS Studies of Differential Reddening across Three Massive Globular Clusters

et al. 2003

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J-, H-, and K s -band data from the Two Micron All Sky Survey (2MASS) are used to study the effects of differential reddening across the three massive Galactic globular clusters ! Centauri, NGC 6388, and NGC 6441. Evidence is found that variable extinction may produce false detections of tidal tails around ! Centauri.We also investigate what appears to be relatively strong differential reddening toward NGC 6388 and NGC 6441 and find that differential extinction may be exaggerating the need for a metallicity spread to explain the width of the red giant branches for these two clusters. Finally, we consider the implications of these results for the connection between unusual, multipopulation globular clusters and the cores of dwarf spheroidal galaxies (dSph).

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Abundance Patterns of the S Stars in ω Centauri

Cited by 30 publications

References 40 publications

Discovery of an Accreted Stellar System within the Globular Cluster ω Centauri

Discovery of an Accreted Stellar System within the Globular Cluster ω Centauri

Deep FORS1 Observations of the Double Main Sequence of ω Centauri

2MASS Studies of Differential Reddening across Three Massive Globular Clusters

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