Astronomical and Imaging Data

Useful Informations

NGC 4372 is a globular cluster located in the southern constellation of Musca, near the Coalsack Nebula and the Dark Doodad Nebula, whose obscuring dust lanes make the cluster appear unusually faint. It is a relatively low-luminosity and sparsely concentrated cluster that is notable for its chemical and kinematic properties.

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Physical Characteristics

• Distance: Approximately 18,900 light-years (5.8 kiloparsecs) from Earth.
• Apparent Magnitude: The cluster has an apparent magnitude of 9.85, making it a faint but observable target for small telescopes.
• Concentration: On the Shapley–Sawyer Concentration Scale, NGC 4372 is a Class XII cluster, indicating an extremely low concentration of stars toward its core.
• Mass and Age: It has a mass of about 3.29×105 solar masses and an estimated age of 12.5 billion years, similar to many other old globular clusters.

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Unique Properties

• Abnormal Chemistry: Despite being an ancient, metal-poor globular cluster with a metallicity of approximately -2.33 dex, spectroscopic studies have found that it has unusually high abundances of alpha elements like magnesium and titanium relative to iron. This “peculiar” chemistry sets it apart from other clusters of a similar age and metallicity.
• Internal Rotation: Contrary to the traditional view of globular clusters as non-rotating, spherically symmetric systems, NGC 4372 has been shown to exhibit a significant degree of internal rotation. This finding, along with similar observations in other clusters, suggests that rotation may be a more common feature of globular cluster dynamics than previously thought. The internal rotation is believed to be responsible for the cluster’s slight flattening.
• Tidal Interaction: The cluster’s location and faint, stretched-out appearance suggest it is undergoing tidal disruption from the Milky Way’s gravity. Its orbit and morphology are consistent with the tidal forces exerted on it, which contribute to its low stellar density.

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