Forming clusters within clusters: How 30 Doradus recollapsed and gave birth again

Abstract

The 30 Doradus Nebula in the Large Magellanic Cloud (LMC) contains the massive starburst cluster NGC 2070 with a massive and probably younger stellar sub clump at its center: R136. It is not clear how such a massive inner cluster could form several million years after the older stars in NGC 2070, given that stellar feedback is usually thought to expel gas and inhibit further star formation. Using the recently developed 1D feedback scheme WARPFIELD to scan a large range of cloud and cluster properties, we show that an age offset of several million years between the stellar populations is in fact to be expected given the interplay between feedback and gravity in a giant molecular cloud (GMC) with a density $\gtrsim 500$ cm${}^{-3}$ due to re-accretion of gas onto the older stellar population. Neither capture of field stars nor gas retention inside the cluster have to be invoked in order to explain the observed age offset in NGC 2070 as well as the structure of the interstellar medium (ISM) around it.

5 pages, 3 figures, accepted to MNRAS

References in corpus (9)

• Fast rotating massive stars and the origin of the abundance patterns in galactic globular clusters
• Formation and Dynamical Evolution of Multiple Stellar Generations in Globular Clusters
• The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 Msun stellar mass limit
• The Effects of Stellar Rotation. II. A Comprehensive Set of Starburst99 Models
• The SILCC project --- IV. Impact of dissociating and ionising radiation on the interstellar medium and Halpha emission as a tracer of the star formation rate
• Feedback in Clouds II: UV Photoionisation and the first supernova in a massive cloud
• A Tale of Three Cities: OmegaCAM discovers multiple sequences in the color-magnitude diagram of the Orion Nebula Cluster
• Gas expulsion vs gas retention: what process dominates in young massive clusters?
• Hydrodynamic simulations of mechanical stellar feedback in a molecular cloud formed by thermal instability

Cited by in corpus (18)

• Mapping metallicity variations across nearby galaxy disks
• The molecular cloud lifecycle
• The R136 star cluster dissected with Hubble Space Telescope/STIS. III. The most massive stars and their clumped winds
• Simulations of the star-forming molecular gas in an interacting M51-like galaxy
• Metallicity, ionization parameter, and pressure variations of HII regions in the TYPHOON spiral galaxies
• The 30 Doradus Molecular Cloud at 0.4 pc Resolution with the Atacama Large Millimeter/submillimeter Array: Physical Properties and the Boundedness of CO-emitting Structures
• The Global Star-Formation Law by Supernova Feedback
• Stellar associations powering HII regions $\unicode{x2013}$ I. Defining an evolutionary sequence
• Early-Forming Massive Stars Suppress Star Formation and Hierarchical Cluster Assembly
• Structural and Dynamical Analysis of 0.1pc Cores and Filaments in the 30~Doradus-10 Giant Molecular Cloud
• Emission-line diagnostics of HII regions using conditional Invertible Neural Networks
• TODDLERS: A new UV-mm emission library for star-forming regions. 1. Integration with SKIRT and public release
• Noise-Net: Determining physical properties of HII regions reflecting observational uncertainties
• The density gradient inside molecular-gas clumps as a booster of their star formation activity
• Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud
• Simulations of pre-supernova feedback in spherical clouds
• The Star Formation Factory revisited I. The impact of metallicity on collapsing star-forming clouds
• The fragmentation properties of massive star-forming regions in 30Dor-10 at 2000 au resolution