Help Privacy Policy Disclaimer
  Advanced SearchBrowse




Journal Article

Structure and rotation of young massive star clusters in a simulated dwarf starburst


Naab,  Thorsten
Computational Structure Formation, MPI for Astrophysics, Max Planck Society;

External Resource
No external resources are shared
Fulltext (restricted access)
There are currently no full texts shared for your IP range.
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available

Lahén, N., Naab, T., Johansson, P. H., Elmegreen, B., Hu, C.-Y., & Walch, S. (2020). Structure and rotation of young massive star clusters in a simulated dwarf starburst. The Astrophysical Journal, 904(1): 71. doi:10.3847/1538-4357/abc001.

Cite as: https://hdl.handle.net/21.11116/0000-0007-E1FB-0
We analyze the three-dimensional shapes and kinematics of the young star cluster population forming in a high-resolution GRIFFIN project simulation of a metal-poor dwarf galaxy starburst. The star clusters, which follow a power-law mass distribution, form from the cold ISM phase with an IMF sampled with individual stars down to 4 solar masses at sub-parsec spatial resolution. Massive stars and their important feedback mechanisms are modelled in detail. The simulated clusters follow a surprisingly tight relation between the specific angular momentum and mass with indications of two sub-populations. Massive clusters (M cl ≳ 3 × 104 M ) have the highes specific angular momenta at low ellipticities (ϵ∼0.2) and show alignment between their shapes and rotation. Lower mass clusters have lower specific angular momenta with larger scatter, show a broader range of elongations, and are typically misaligned indicating that they are not shaped by rotation. The most massive clusters (M≳105M) accrete gas and proto-clusters from a ≲100pc scale local galactic environment on a t≲10Myr timescale, inheriting the ambient angular momentum properties. Their two-dimensional kinematic maps show ordered rotation at formation, up to v∼8.5kms−1, consistent with observed young massive clusters and old globular clusters, which they might evolve into. The massive clusters have angular momentum parameters λR≲0.5 and show Gauss-Hermite coefficients h3 that are anti-correlated with the velocity, indicating asymmetric line-of-sight velocity distributions as a signature of a dissipative formation process.