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

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

Nov 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.300..857e&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 300, Issue 3, pp. 857-862.

Astronomy and Astrophysics

Astronomy

56

Binaries: General, Globular Clusters: Individual: Ngc 1818, Magellanic Clouds, Galaxies: Star Clusters

Scientific paper

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 M_primary~2-5.5M_solar 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.

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