A large C+N+O abundance spread in giant stars of the globular cluster NGC 1851

David Yong; Frank Grundahl; Francesca D'Antona; Amanda I. Karakas; John C. Lattanzio; John E. Norris

doi:10.1088/0004-637X/695/1/L62

A large C+N+O abundance spread in giant stars of the globular cluster NGC 1851

David Yong^*, Frank Grundahl, Francesca D'Antona, Amanda I. Karakas, John C. Lattanzio, John E. Norris

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

103 Citations (Scopus)

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. 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 asymptotic giant branch stars are responsible for the globular cluster light element abundance variations.

Original language	English
Pages (from-to)	L62-L66
Journal	Astrophysical Journal
Volume	695
Issue number	1 PART 2
DOIs	https://doi.org/10.1088/0004-637X/695/1/L62
Publication status	Published - 2009

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title = "A large C+N+O abundance spread in giant stars of the globular cluster NGC 1851",

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. 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 asymptotic giant branch stars are responsible for the globular cluster light element abundance variations.",

keywords = "Galaxy: abundances, Globular clusters: individual (NGC 1851), Stars: abundances",

author = "David Yong and Frank Grundahl and Francesca D'Antona and Karakas, {Amanda I.} and Lattanzio, {John C.} and Norris, {John E.}",

year = "2009",

doi = "10.1088/0004-637X/695/1/L62",

language = "English",

volume = "695",

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TY - JOUR

T1 - A large C+N+O abundance spread in giant stars of the globular cluster NGC 1851

AU - Yong, David

AU - Grundahl, Frank

AU - D'Antona, Francesca

AU - Karakas, Amanda I.

AU - Lattanzio, John C.

AU - Norris, John E.

PY - 2009

Y1 - 2009

N2 - 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. 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 asymptotic giant branch stars are responsible for the globular cluster light element abundance variations.

AB - 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. 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 asymptotic giant branch stars are responsible for the globular cluster light element abundance variations.

KW - Galaxy: abundances

KW - Globular clusters: individual (NGC 1851)

KW - Stars: abundances

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U2 - 10.1088/0004-637X/695/1/L62

DO - 10.1088/0004-637X/695/1/L62

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VL - 695

SP - L62-L66

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 PART 2

ER -

A large C+N+O abundance spread in giant stars of the globular cluster NGC 1851

Abstract

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