A large C+N+O abundance spread in giant stars of the globular cluster NGC 1851
David Yong (1), Frank Grundahl (2), Francesca D'Antona (3), Amanda I., Karakas (1), John C. Lattanzio (4), and John E. Norris (1) ((1) RSAA, Mt, Stromlo Observatory, (2) Univ. of Aarhus, (3) INAF Osservatorio di Roma, (4), CSPA, Monash University)
TL;DR
This study reveals a significant C+N+O abundance spread in giant stars of NGC 1851, supporting the idea that AGB stars influence light element variations and the cluster's multiple populations.
Contribution
It provides the first strong evidence linking C+N+O variations to AGB star pollution in a globular cluster.
Findings
C+N+O abundance varies by 0.6 dex among giants
Correlations found between C+N+O and light element abundances
Supports AGB star pollution scenario in globular clusters
Abstract
Abundances of C, N, and O are determined in four bright red giants that span the known abundance range for light (Na and Al) and s-process (Zr and La) elements in the globular cluster NGC 1851. The abundance sum C+N+O exhibits a range of 0.6 dex, a factor of 4, in contrast to other clusters in which no significant C+N+O spread is found. Such an abundance range offers support for the Cassisi et al. (2008) scenario in which the double subgiant branch populations are coeval but with different mixtures of C+N+O abundances. Further, the Na, Al, Zr, and La abundances are correlated with C+N+O, and therefore, NGC 1851 is the first cluster to provide strong support for the scenario in which AGB stars are responsible for the globular cluster light element abundance variations.
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