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NGC1818 unveils the origin of the extended main-sequence turn-off in young Magellanic Clouds clusters

The nature of young star clusters in the Magellanic Clouds is debated. Here, the authors show an alternative approach that exploits data to exclude the presence of age differences greater than a few million years among cluster stars in a very young cluster.

Giacomo Cordoni
Antonino P. Milone
Maria V. Legnardi
ResearchOpen Access26 Jul 2022
Nature Communications

Volume: 13, P: 1-9
Author Correction: Fast-moving stars around an intermediate-mass black hole in ω Centauri

Maximilian Häberle
Nadine Neumayer
Glenn van de Ven
Amendments and CorrectionsOpen Access17 Sept 2024
Nature

Volume: 634, P: E1
Fast-moving stars around an intermediate-mass black hole in ω Centauri

Observations of seven fast-moving stars in the central 3 arcsec (0.08 pc) of ω Centauri indicate an intermediate-mass black hole in ω Centauri.

Maximilian Häberle
Nadine Neumayer
Glenn van de Ven
ResearchOpen Access10 Jul 2024
Nature

Volume: 631, P: 285-288
Stellar mergers as the origin of the blue main-sequence band in young star clusters

The distribution of the slowly rotating, blue fraction of main-sequence stars in the colour–magnitude diagram of young star clusters, and their peculiar mass function, imply that they may originate from binary star mergers.

Chen Wang
Norbert Langer
Selma E. de Mink
Research10 Feb 2022
Nature Astronomy

Volume: 6, P: 480-487
Stars caught in the braking stage in young Magellanic Cloud clusters

Some star clusters in the Large Magellanic Cloud have extended main-sequence turnoffs, suggesting that the component stars have different ages. However, if the blue main-sequence stars were initially spinning rapidly, and experienced braking, the apparent age difference disappears.

Francesca D’Antona
Antonino P. Milone
Marcella Di Criscienzo
Research24 Jul 2017
Nature Astronomy

Volume: 1, P: 1-5
Rapidly rotating second-generation progenitors for the ‘blue hook’ stars of ω Centauri

The observed range of luminosities of the extremely hot ‘blue hook’ stars of the globular cluster ω Centauri is successfully explained by a model in which the progenitors of these stars are second-generation helium-rich stars characterized by a range of rotation rates arising during the cluster’s very early evolution.

Marco Tailo
Francesca D’Antona
Roberto Capuzzo-Dolcetta
Research22 Jun 2015
Nature

Volume: 523, P: 318-321

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NGC1818 unveils the origin of the extended main-sequence turn-off in young Magellanic Clouds clusters

Author Correction: Fast-moving stars around an intermediate-mass black hole in ω Centauri

Fast-moving stars around an intermediate-mass black hole in ω Centauri

Stellar mergers as the origin of the blue main-sequence band in young star clusters

Stars caught in the braking stage in young Magellanic Cloud clusters

Rapidly rotating second-generation progenitors for the ‘blue hook’ stars of ω Centauri

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