The Chemical Evolution of the Globular Cluster ω Centauri (NGC 5139)

By V. Smith, N. Suntzeff, K. Cunha, Roberto Gallino, M. Busso, D. Lambert, O. Straniero. 2000

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In Astronomy and Astrophysics

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Abundance Variations within Globular Clusters (2004, background): “An extensive study was presented by Smith et al. (2000), who considered 22 chemical elements in 10 red giants plus published literature values, spanning the range from [Fe/H] ∼ −1.8 to −0.8.”
Nucleosynthesis and Mixing on the Asymptotic Giant Branch. III. Predicted and Observed s-Process Abundances (2001, background): “This is e.g. the case of the s enrichment in red giants belonging to the globular cluster ω Cen (Smith et al. 2000).”
“Sculptor-ing” the Galaxy? The Chemical Compositions of Red Giants in the Sculptor Dwarf Spheroidal Galaxy (2004, methodology): “Cen (e.g., Vanture et al. 1994; Norris & Da Costa 1995; Smith et al. 2000).”
The two metallicity groups of the globular cluster M 22: a chemical perspective (2011, background): “In the latter, the s-process abundance ratios rise seemingly monotonically with [Fe/H] before reaching a plateau at constant [s-process/Fe] (Norris & Da Costa 1995, Smith et al. 2000, Marino et al. 2011, Stanford et al. 2010, Johnson & Pilachowski 2010).”
The 85Kr s-Process Branching and the Mass of Carbon Stars (2001, background): “…& Lambert 1999) and in AGB stars of di†erent spectral types : Ba stars (Tomkin & Lambert 1983 ; Malaney & Lambert 1988), MS and S giants (Lambert et al. 1995), yellow symbiotics (Smith et al. 1997), and some s-processÈ rich stars in u Cen (Vanture, Wallerstein, & Brown 1994 ; Smith et al. 2000).”
The Multiplicity of the Subgiant Branch of ω Centauri: Evidence for Prolonged Star Formation (2007, background): “In this case, our results agree well: Smith et al. (2000) found a Ca and Ti enhancement between 0.2 and 0.4 dex, as we do; but, more inter- esting, the Ba abundance also agrees, with the bulk of stars in their paper having [Ba/Fe] between 0.5 and 1.0 dex.”
Metallicities on the Double Main Sequence of ω Centauri Imply Large Helium Enhancement (2004, background): “The Ba abundance for stars on the bMS is compatible with (albeit somewhat smaller than) that observed in metal-rich red giants of ω Cen (cf. Smith et al. 2000).”
Abundances of Cu and Zn in metal-poor stars: Clues for Galaxy evolution (2002, background): “Recently, also some data for ω Centauri have become available (see e.g. Smith et al. 2000; Cunha et al. 2002; Pancino et al. 2002), together with abundances in single very low-metallicity galactic stars (Westin et al. 2000; Cowan et al. 2002; Hill et al. 2002).”
Formation of ω Centauri from an Ancient Nucleated Dwarf Galaxy (2003, background): “…(e.g., Freeman & Rodgers 1975; Norris et al. 1996), strong variations of nearly all element abundances among its stars (e.g., Norris & Da Costa 1995; Smith et al. 2000), kinematical difference between its metal-rich and metal-poor stellar populations (e.g., Norris et al. 1997), multiple stellar…”
The s process: Nuclear physics, stellar models, and observations (2010, background): “Studies of neutroncapture elements for a significant sample of cluster stars by Norris and Da Costa (1995) and Smith et al. (2000) have shown that the [Ba/Fe] and [La/Fe] ratios increase with increasing metallicity.”
Abundance Patterns in the Draco, Sextans, and Ursa Minor Dwarf Spheroidal Galaxies (2000, background): “Such a situation would not be entirely surprising given the relative luminosities of the dSph galaxies and ω Cen: i.e., the latter has roughly the same luminosity as the three dSph galaxies combined.”
ω Centauri: The Population Puzzle Goes Deeper (2004, background): “The dramatic increase ofs-process heavy-element abundances with metallicity found by Smith et al. (2000) inq Cen RGB stars further supports the hypothesis that Mint stars could have formed from material polluted by ejecta from AGB stars.”
An Abundance Analysis of Bright Giants in the Globular Cluster NGC 1851 (2007, background): “…a large metallicity spread and are the two most massive Galactic globular clusters. q Centauri is widely regarded as the nucleus of an accreted dwarf galaxy (e.g., Smith et al. 2000), and M54 is suspected to be the nucleus of the Sagittarius dwarf spheroidal galaxy (e.g., Layden & Sarajedini 2000).”
Origin of multiple stellar populations in globular clusters and their helium enrichment (2008, background): “In ω Cen star-to-star variations of CNO elements exist as well, but their overall [C + N + O/Fe] abundance ratio appear to be constant within a factor of ∼2, as typical of all GCs (e.g. Norris & Da Costa 1995; Smith et al. 2000, 2005).”
CHEMICAL ABUNDANCES FOR 855 GIANTS IN THE GLOBULAR CLUSTER OMEGA CENTAURI (NGC 5139) (2010, methodology): “Previous high resolution spectroscopic work has targeted more than 200 RGB stars (Cohen 1981; Brown & Wallerstein 1993; Norris & Da Costa 1995; Zucker et al. 1996; Smith et al. 2000; Johnson et al. 2008; Johnson et al. 2009) and shown: (1) ∆[Al/Fe]>0.5 at all metallicities and exceeds more than a fa”
New Analyses of Star-to-Star Abundance Variations among Bright Giants in the Mildly Metal-poor Globular Cluster M5 (2001, background): “Even more striking is the Eu deÐciency found among u Cen giants of intermediate metallicity (Smith et al. 2000).”
The formation of ultracompact dwarf galaxies (2001, result): “Such a scenario may also be consistent with the unusual metallicity distribution in ω Cen (e.g. Smith et al. 2000), which is being taken as evidence that this unusual cluster may in fact be a compact dwarf galaxy.”
The Helium Abundances of ω Centauri (2004, background): “Values in the range 0–5 Gyr have been claimed (Norris & Da Costa 1995; Lee et al. 1999; Smith et al. 2000; Hilker & Richtler 2000; Stanford et al. 2004; Ferraro et al. 2004; Hughes et al. 2004; Rey et al. 2004).”