Volume 549, January 2013
|Number of page(s)||16|
|Section||Galactic structure, stellar clusters and populations|
|Published online||14 January 2013|
Local-density-driven clustered star formation
Astronomisches Rechen-Institut, Zentrum für Astronomie, Heidelberg
2 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
3 Argelander-Institut für Astronomie, Bonn Universität, Auf dem Hügel 71, 53121 Bonn, Germany
Accepted: 23 October 2012
Context. A positive power-law trend between the local surface densities of molecular gas, Σgas, and young stellar objects, Σ ⋆ , in molecular clouds of the solar neighbourhood has recently been identified. How it relates to the properties of embedded clusters, in particular to the recently established radius-density relation, has so far not been investigated.
Aims. We model the development of the stellar component of molecular clumps as a function of time and initial local volume density. Our study provides a coherent framework able to explain both the molecular-cloud and embedded-cluster relations quoted above.
Methods. We associate the observed volume density gradient of molecular clumps to a density-dependent free-fall time. The molecular clump star formation history is obtained by applying a constant star formation efficiency per free-fall time, ϵff.
Results. For the volume density profiles typical of observed molecular clumps (i.e. power-law slope ≃ −1.7), our model gives a star-gas surface-density relation of the form Σ⋆ ∝ Σgas2, which agrees very well with the observations. Taking the case of a molecular clump of mass M0 ≃ 104 M⊙ and radius R ≃ 6 pc experiencing star formation during 2 Myr, we derive what star formation efficiency per free-fall time matches the normalizations of the observed and predicted (Σ ⋆ , Σgas) relations best. We find ϵff ≃ 0.1. We show that the observed growth of embedded clusters, embodied by their radius-density relation, corresponds to a surface density threshold being applied to developing star-forming regions. The consequences of our model in terms of cluster survivability after residual star-forming gas expulsion are that, owing to the locally high star formation efficiency in the inner part of star-forming regions, global star formation efficiency as low as 10% can lead to the formation of bound gas-free star clusters.
Key words: stars: formation / galaxies: star clusters: general / ISM: clouds / stars: kinematics and dynamics
© ESO, 2013
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