Publication

Evidence for metallicity spreads in three massive M31 globular clusters

Pascale Jablonka, Georges Meylan
2008
Journal Articles

Abstract

Aims. We quantify the intrinsic width of the red giant branches of three massive globular clusters in M31 in a search for metallicity spreads within these objects.

Official source

https://infoscience.epfl.ch/entities/publication/526d6e62-e2b5-4156-8101-cc80e99fceea

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Pascale Jablonka, Georges Meylan
2008
Journal Articles

Abstract

Aims. We quantify the intrinsic width of the red giant branches of three massive globular clusters in M31 in a search for metallicity spreads within these objects.

Official source

https://infoscience.epfl.ch/entities/publication/526d6e62-e2b5-4156-8101-cc80e99fceea

About this result

Ontological neighbourhood

Astronomy

Astrophysics: Stellar astronomy

Related concepts (16)

Globular cluster

A globular cluster is a spheroidal conglomeration of stars. Globular clusters are bound together by gravity, with a higher concentration of stars towards their centers. They can contain anywhere from tens of thousands to many millions of member stars. Their name is derived from Latin globulus (small sphere). Globular clusters are occasionally known simply as "globulars". Although one globular cluster, Omega Centauri, was observed in antiquity and long thought to be a star, recognition of the clusters' true nature came with the advent of telescopes in the 17th century.

Star cluster

Star clusters are large groups of stars held together by self-gravitation. Two main types of star clusters can be distinguished: globular clusters are tight groups of ten thousand to millions of old stars which are gravitationally bound, while open clusters are more loosely clustered groups of stars, generally containing fewer than a few hundred members, and are often very young.

Red clump

The red clump is a clustering of red giants in the Hertzsprung–Russell diagram at around 5,000 K and absolute magnitude (MV) +0.5, slightly hotter than most red-giant-branch stars of the same luminosity. It is visible as a denser region of the red-giant branch or a bulge towards hotter temperatures. It is prominent in many galactic open clusters, and it is also noticeable in many intermediate-age globular clusters and in nearby field stars (e.g. the Hipparcos stars).

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