Kinematics of subclusters in star cluster complexes: imprint of their parental molecular clouds

摘要: Star cluster complexes such as the Carina Nebula can have formed in turbulent giant molecular clouds. We perform a series of $N$-body simulations starting from subclustering initial conditions based on hydrodynamic These finally result formation star consisting several subclusters (clumps). obtain inter-clump velocity distribution, size region, and mass most massive our simulated complex compare results with observed ones (the NGC 2264). The one-dimensional dispersion obtained is $2.9\pm0.3$ $1.4\pm0.4$ km s$^{-1}$ for Carina- 2264-like models, respectively, which are consistent those Gaia Data Release 2: 2.35 0.99 2264, respectively. estimate that masses parental clouds 2264 $4\times 10^5$ 10^4M_{\odot}$,