Astrophys. J., 904, 71-71 (2020/November-3)
Structure and rotation of young massive star clusters in a simulated dwarf starburst.
LAHEN N., NAAB T., JOHANSSON P.H., ELMEGREEN B., HU C.-Y. and WALCH S.
Abstract (from CDS):
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 phase interstellar medium with an initial mass function sampled with individual stars down to four solar masses at sub-parsec spatial resolution. Massive stars and their important feedback mechanisms are modeled 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 (Mcl >= 3 x 104 M☉) have the highest 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 >= 105 M☉) accrete gas and protoclusters from a <=100 pc scale local galactic environment on a t <= 10 Myr timescale, inheriting the ambient angular momentum properties. Their two-dimensional kinematic maps show ordered rotation at formation, up to v ∼ 8.5 km s–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.
© 2020. The American Astronomical Society. All rights reserved.
Young star clusters - Computational astronomy - Stellar kinematics - Star formation
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