How to Find Young Massive Cluster Progenitors

Abstract

We propose that bound, young massive stellar clusters form from dense clouds that have escape speeds greater than the sound speed in photo-ionized gas. In these clumps, radiative feedback in the form of gas ionization is bottled up, enabling star formation to proceed to sufficiently high efficiency so that the resulting star cluster remains bound even after gas removal. We estimate the observable properties of the massive proto-clusters (MPCs) for existing Galactic plane surveys and suggest how they may be sought in recent and upcoming extragalactic observations. These surveys will potentially provide a significant sample of MPC candidates that will allow us to better understand extreme star-formation and massive cluster formation in the Local Universe.

5 pages, 1 figure, 1 table, accepted for publication in ApJL

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Cited by in corpus (61)

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• Comparing Young Massive Clusters and their Progenitor Clouds in the Milky Way
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• A Census of Star Formation in the Outer Galaxy II: The GLIMPSE360 Field
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• Unveiling the physical conditions in NGC 6910
• Formation of Massive Star Clusters by Fast HI Gas Collision
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• A Census of Star Formation in the Outer Galaxy: the SMOG field
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