Young Massive Star Clusters

By S. P. Portegies Zwart, S. McMillan, M. Gieles. 2010

905 citations recorded by the source corpus.

Young massive clusters (YMCs) are dense aggregates of young stars that form the fundamental building blocks of galaxies. Several examples exist in the Milky Way Galaxy and the Local Group, but they are particularly abundant in starburst and interacting galaxies. The few YMCs that are close enough to resolve are of prime interest for studying the stellar mass function and the ecological interplay between stellar evolution and stellar dynamics. The distant unresolved clusters may be effectively used to study the star-cluster mass function, and they provide excellent constraints on the formation mechanisms of young cluster populations. YMCs are expected to be the nurseries for many unusual objects, including a wide range of exotic stars and binaries. So far only a few such objects have been found in YMCs, although their older cousins, the globular clusters, are unusually rich in stellar exotica. In this review, we focus on star clusters younger than ∼100 Myr, more than a few current crossing times old, and m...

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3808053c1f4238c77d7d2a0a22d29992872aae91

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Citations in the corpus

Feedback from winds and supernovae in massive stellar clusters – I. Hydrodynamics (2012, background): “The removal of molecular material is also crucial to the question of cluster dissolution (Portegies Zwart et al. 2010; Pfalzner 2011; Pelupessy & Portegies Zwart 2012).”
Merging black holes in young star clusters (2019, background): “Star formation (and especially massive star formation) is expected to occur mostly in young SCs and associations (Lada & Lada 2003; Portegies Zwart et al. 2010).”
On the fraction of star formation occurring in bound stellar clusters (2012, background): “P. 137 Kruijssen J. M. D., Cooper A. P., 2012, MNRAS, 420, 340 Kruijssen J. M. D., Pelupessy F. I., Lamers H. J. G. L. M., Portegies Zwart S. F., Icke V., 2011, MNRAS, 414, 1339 Kruijssen J. M. D., Maschberger T., Moeckel N., Clarke C. J., Bastian N., Bonnell I. A., 2012a, MNRAS, 419, 841 Kruijssen ”
Kinematics in Young Star Clusters and Associations with Gaia DR2 (2018, background): “Much attention has been focused on the role of gas expulsion, which will cause a cluster to expand and can cause bound embedded clusters to become unbound (Mathieu 1983; Elmegreen 1983; Adams 2000; Kroupa et al. 2001; Goodwin & Bastian 2006; Pelupessy & Portegies Zwart 2012; Brinkmann et al. 2017).”
Evidence of Environmental Dependencies of Type Ia Supernovae from the Nearby Supernova Factory indicated by Local H$\alpha$ (2013, background): “This cohort is likely to have been an open cluster or OB association; open clusters remain bound on the relevant timescale, while OB associations have very low velocities dispersions (∼ 3 km s−1 de Zeeuw et al. 1999; Portegies Zwart et al. 2010; Röser et al. 2010).”
Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo (2018, background): “For example, BBHs might form from isolated massive binaries in the galactic field through common-envelope evolution(Bethe & Brown 1998; Portegies Zwart & Yungelson 1998; Belczynski et al. 2002, 2007, 2008, 2014; Voss & Tauris 2003; Dewi et al. 2006; Dominik et al. 2013; Mennekens & Vanbeveren 2014; ”
ATLASGAL - properties of a complete sample of Galactic clumps (2017, background): “These can be broadly defined as being younger than 100 Myr and having stellar masses &10,000 M (Portegies Zwart et al. 2010).”
A Gaia DR2 view of the open cluster population in the Milky Way (2018, background): “…in isolation, it is believed that most (possibly all) stars form in clustered environments and spend at least a short amount of time gravitationally bound with their siblings (see e.g. Clarke et al. 2000; Lada & Lada 2003; Portegies Zwart et al. 2010), embedded in their progenitor molecular cloud.”
Physical Processes in the Interstellar Medium (2014, background): “They seem inconsistent with the observed stellar densities of most Galactic star clusters (e.g. Portegies Zwart et al., 2010, and references therein), but could be reached in the central regions of the most extreme and massive clusters in the Local Group (such as 30 Doradus in the LMC as shown in Fi”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “Portegies Zwart et al. (2010) have cataloged massive (M⋆ ≥ 10 4 M⊙), young (age ≤ 100 Myr) clusters (12) and associations (13), but none of these are more distant than the Galactic Center, so they are clearly undercounted.”
The R136 star cluster dissected with Hubble Space Telescope/STIS. I. Far-ultraviolet spectroscopic census and the origin of He II λ1640 in young star clusters (2016, background): “However, the 0.1 pc core radius of R136a (Portegies Zwart et al. 2010; Selman & Melnick 2013) subtends only 0.41 arcsec at the 50 kpc distance to the LMC (Pietrzyński et al. 2013), which led to the cluster at one time being mistaken for a ≥1000 M star (Cassinelli, Mathis & Savage 1981; Feitzinger,…”
Modeling Dense Star Clusters in the Milky Way and Beyond with the CMC Cluster Catalog (2019, background): “Such objects may have important implications for the formation of intermediate-mass BHs (IMBHs; e.g., Ebisuzaki et al. 2001; Portegies Zwart & McMillan 2002; Gürkan et al. 2004; Freitag et al. 2006; Portegies Zwart et al. 2010; Goswami et al. 2012).”
Observational Signatures of Particle Acceleration in Supernova Remnants (2012, background): “Its age is just 1-2 Myr and its central density reaches 105 M pc −3 (Portegies Zwart et al., 2010).”
CO-EVOLUTION OF GALACTIC NUCLEI AND GLOBULAR CLUSTER SYSTEMS (2013, background): “2010, ApJ, 718, 739 Miller, M. C. & Davies, M. B. 2012, ApJ, 755, 81 Misgeld, I. & Hilker, M. 2011, MNRAS, 414, 3699 Morscher, M., Umbreit, S., Farr, W. M., & Rasio, F. A. 2013, ApJ, 763, L15 Muratov, A. L. & Gnedin, O. Y. 2010, ApJ, 718, 1266 Naab, T., Johansson, P. H., & Ostriker, J. P. 2009, ApJ,”