The binary star population of the young cluster NGC 1818 in the Large Magellanic Cloud

Rebecca A.W. Elson; Steinn Sigurdsson; Melvyn Davies; Jarrod Hurley; Gerard Gilmore

doi:10.1111/j.1365-8711.1998.t01-1-01948.x

The binary star population of the young cluster NGC 1818 in the Large Magellanic Cloud

Rebecca A.W. Elson
, Steinn Sigurdsson
, Melvyn Davies
, Jarrod Hurley
, Gerard Gilmore

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

66 Scopus citations

Abstract

We determine the binary star fraction as a function of radius in NGC 1818, a young rich cluster in the Large Magellanic Cloud, using Hubble Space Telescope images in bands F336W (∼U) and F555W (∼V). Our sample includes binaries with A/_primary ∼2-5.5 M⊙ and M_secondary ≳ 0.7M_primary. The binary fraction increases towards the cluster centre, from ∼20 ± 5 per cent in the outer parts, to ∼35 ± 5 per cent inside the core. This increase is consistent with dynamical mass segregation and need not be primordial. We compare our results with expectations from N-body models, and discuss the implications for the formation and early evolution of such clusters.

Original language	English (US)
Pages (from-to)	857-862
Number of pages	6
Journal	Monthly Notices of the Royal Astronomical Society
Volume	300
Issue number	3
DOIs	https://doi.org/10.1111/j.1365-8711.1998.t01-1-01948.x
State	Published - Nov 1 1998

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.1111/j.1365-8711.1998.t01-1-01948.x

Cite this

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title = "The binary star population of the young cluster NGC 1818 in the Large Magellanic Cloud",

abstract = "We determine the binary star fraction as a function of radius in NGC 1818, a young rich cluster in the Large Magellanic Cloud, using Hubble Space Telescope images in bands F336W (∼U) and F555W (∼V). Our sample includes binaries with A/primary ∼2-5.5 M⊙ and Msecondary ≳ 0.7Mprimary. The binary fraction increases towards the cluster centre, from ∼20 ± 5 per cent in the outer parts, to ∼35 ± 5 per cent inside the core. This increase is consistent with dynamical mass segregation and need not be primordial. We compare our results with expectations from N-body models, and discuss the implications for the formation and early evolution of such clusters.",

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T1 - The binary star population of the young cluster NGC 1818 in the Large Magellanic Cloud

AU - Elson, Rebecca A.W.

AU - Sigurdsson, Steinn

AU - Davies, Melvyn

AU - Hurley, Jarrod

AU - Gilmore, Gerard

PY - 1998/11/1

Y1 - 1998/11/1

N2 - We determine the binary star fraction as a function of radius in NGC 1818, a young rich cluster in the Large Magellanic Cloud, using Hubble Space Telescope images in bands F336W (∼U) and F555W (∼V). Our sample includes binaries with A/primary ∼2-5.5 M⊙ and Msecondary ≳ 0.7Mprimary. The binary fraction increases towards the cluster centre, from ∼20 ± 5 per cent in the outer parts, to ∼35 ± 5 per cent inside the core. This increase is consistent with dynamical mass segregation and need not be primordial. We compare our results with expectations from N-body models, and discuss the implications for the formation and early evolution of such clusters.

AB - We determine the binary star fraction as a function of radius in NGC 1818, a young rich cluster in the Large Magellanic Cloud, using Hubble Space Telescope images in bands F336W (∼U) and F555W (∼V). Our sample includes binaries with A/primary ∼2-5.5 M⊙ and Msecondary ≳ 0.7Mprimary. The binary fraction increases towards the cluster centre, from ∼20 ± 5 per cent in the outer parts, to ∼35 ± 5 per cent inside the core. This increase is consistent with dynamical mass segregation and need not be primordial. We compare our results with expectations from N-body models, and discuss the implications for the formation and early evolution of such clusters.

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The binary star population of the young cluster NGC 1818 in the Large Magellanic Cloud

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