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  The GRIFFIN project -- Formation of star clusters with individual massive stars in a simulated dwarf galaxy starburst

Lahén, N., Naab, T., Johansson, P. H., Elmegreen, B., Hu, C.-Y., Walch, S., et al. (2020). The GRIFFIN project -- Formation of star clusters with individual massive stars in a simulated dwarf galaxy starburst. The Astrophysical Journal, 891(1): 2. doi:10.3847/1538-4357/ab7190.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0006-C0EC-7 Version Permalink: http://hdl.handle.net/21.11116/0000-0006-C0EF-4
Genre: Journal Article

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Lahén, Natalia, Author
Naab, Thorsten1, Author              
Johansson, Peter H., Author
Elmegreen, Bruce, Author
Hu, Chia-Yu, Author
Walch, Stefanie, Author
Steinwandel, Ulrich P.2, Author              
Moster, Benjamin P.1, Author              
Affiliations:
1Computational Structure Formation, MPI for Astrophysics, Max Planck Society, ou_2205642              
2Cosmology, MPI for Astrophysics, Max Planck Society, ou_159876              

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 Abstract: We describe a population of young star clusters (SCs) formed in a hydrodynamical simulation of a gas-rich dwarf galaxy merger resolved with individual massive stars at sub-parsec spatial resolution. The simulation is part of the GRIFFIN (Galaxy Realizations Including Feedback From INdividual massive stars) project. The star formation environment during the simulation spans seven orders of magnitude in gas surface density and thermal pressure, and the global star formation rate surface density (ΣSFR) varies by more than three orders of magnitude during the simulation. Young SCs more massive than M∗,cl∼102.5M form along a mass function with a power-law index α∼−1.7 (α∼−2 for M∗,cl ≳103M) at all merger phases, while the normalization and the highest SC masses (up to ∼106M) correlate with ΣSFR. The cluster formation efficiency varies from Γ∼20% in early merger phases to Γ∼80% at the peak of the starburst and is compared to observations and model predictions. The massive SCs (≳104M) have sizes and mean surface densities similar to observed young massive SCs. Simulated lower mass clusters appear slightly more concentrated than observed. All SCs form on timescales of a few Myr and lose their gas rapidly resulting in typical stellar age spreads between σ∼0.1−2 Myr (1σ), consistent with observations. The age spreads increase with cluster mass, with the most massive cluster (∼106M) reaching a spread of 5Myr once its hierarchical formation finishes. Our study shows that it is now feasible to investigate the SC population of entire galaxies with novel high-resolution numerical simulations.

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 Dates: 2020-02-27
 Publication Status: Published online
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 Identifiers: DOI: 10.3847/1538-4357/ab7190
Other: LOCALID: 3245065
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Title: The Astrophysical Journal
Source Genre: Journal
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Publ. Info: Bristol; Vienna : IOP Publishing; IAEA
Pages: - Volume / Issue: 891 (1) Sequence Number: 2 Start / End Page: - Identifier: ISSN: 0004-637X
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215_3