## The very bright and compact massive young cluster, NGC 3603, has been cited as an example of a starburst in the Milky Way and compared with the much-studied R136/30 Doradus region in the Large Magellanic Cloud.

The O star hinterland of the Galactic starburst, NGC 3603

## 5If* star RFS8 ($\sim$70 $M_{\odot}$), found within $\approx$ 53 and 58 pc respectively from the Galactic massive young cluster NGC 3603, using Gaia data.

On the origin of very massive stars around NGC 3603

## Multiwavelength observations show that Abell 1367 (A1367) is a dynamically young cluster, with at least two subclusters merging along the SE–NW direction.

A merger shock in Abell 1367

## Multiwavelength observations show that Abell 1367 (A1367) is a dynamically young cluster, with at least two subclusters merging along the SE–NW direction.

A merger shock in Abell 1367.

## 0 to several open clusters with different properties and environments to show the capabilities of the tool: an area of five degrees around NGC 2682 (M 67), an old, well known cluster; a young cluster NGC 2516 with a striking elongate structure extended up to four degrees; NGC 1750 & NGC 1758, a pair of partly overlapping clusters; in the area of NGC 1817 we confirm a little-known cluster, Juchert 23; and in an area with many clusters we disentangle the existence of two overlapping clusters where only one was previously known: Ruprecht 26 and the new, Clusterix 1.

Clusterix 2.0. A Virtual Observatory tool to estimate cluster membership probability

## We examine the mass-dependence of the velocity dispersion of stars in the young cluster NGC 6530 to better understand how it formed.

Kinematic signatures of cluster formation from cool collapse in the Lagoon Nebula cluster NGC 6530

10.1051/0004-6361/201936579

## In particular, we use proper motions to detect co-moving groups of stars which can trace low mass or partially dissolved young clusters in the GC that can hardly be discovered by any other means.

First results from a large-scale proper motion study of the Galactic Centre

10.1093/mnras/stz3610

## 0 to several open clusters with different properties and environments to show the capabilities of the tool: an area of five degrees around NGC 2682 (M 67), an old, well known cluster; a young cluster NGC 2516 with a striking elongate structure extended up to four degrees; NGC 1750 & NGC 1758, a pair of partly overlapping clusters; in the area of NGC 1817 we confirm a little-known cluster, Juchert 23; and in an area with many clusters we disentangle the existence of two overlapping clusters where only one was previously known: Ruprecht 26 and the new, Clusterix 1.

Clusterix 2.0. A Virtual Observatory tool to estimate cluster membership probability

10.3847/1538-4357/aaf6ea

## This is the predicted cutoff from dynamical models in which old globular clusters and young clusters observed today formed by similar processes with similar initial mass functions.

Constraints on Upper Cutoffs in the Mass Functions of Young Star Clusters

10.1093/mnras/stz1897

## Traditionally, expanding young clusters have been pictured as entities that became unbound due to the lack of gravitational binding once the gas from the parental cloud that formed the cluster has been expelled by the stellar radiation of the massive stars in the cluster.

Flipping-up the field: gravitational feedback as a mechanism for young clusters dispersal

## Chemical enrichment is a dynamic process happening as the young cluster assembles, so that the original (1P) and enriched (2P) subpopulations of stars form almost simultaneously.

On the origin of multiple populations during massive star cluster formation

10.1093/mnras/stz2303

## We examine the mass-dependence of the velocity dispersion of stars in the young cluster NGC 6530 to better understand how it formed.

Kinematic signatures of cluster formation from cool collapse in the Lagoon Nebula cluster NGC 6530

## The very bright and compact massive young cluster, NGC 3603, has been cited as an example of a starburst in the Milky Way and compared with the much-studied R136/30 Doradus region in the Large Magellanic Cloud.

The O star hinterland of the Galactic starburst, NGC 3603

10.1134/S1063772919060039

## At the time of its discovery, it was the first multi-planet system in a young cluster.

Activity of Five Young Dwarfs with Planetary Systems

10.1038/s41550-019-0865-1

## The distribution of size as a function of age observed for star clusters in the Large Magellanic Cloud (LMC) is very puzzling: young clusters are all compact, while the oldest systems show both small and large sizes.

Size diversity of old Large Magellanic Cloud clusters as determined by internal dynamical evolution

10.3847/1538-4357/ab3e06

## The low surface brightness of the streams (typically >30 mag/arcsec$^2$), however, will make them difficult to detect, unless the streams originate from very young clusters.

Detecting Thin Stellar Streams in External Galaxies: Resolved Stars & Integrated Light

## A grid of 20 millions 3-1100$\mu$m SED models is presented for synthetic young clusters embedded in dense clumps.

Evolution of young protoclusters embedded in dense massive clumps. A new grid of population synthesis SED models and a new set of L/M evolutionary tracks

10.3847/1538-3881/aafbe6

## We make stellar surface density and minimum spanning tree maps to identify young clusters, and use {\it Spitzer} images to identify irradiated structures, such as elephant trunk-like structures (ETLSs) and pillars in the region.

Understanding Formation of Young, Distributed Low-mass Stars and Clusters in the W4 Cloud Complex

10.1051/0004-6361/201935051

## Grids of stellar models are useful tools to derive the properties of stellar clusters, in particular young clusters hosting massive stars, and to provide information on the star formation process in various mass ranges.

Stellar models and isochrones from low-mass to massive stars including pre-main sequence phase with accretion

10.1093/mnras/sty3424

## However, the clustering strength of the most massive GMCs, supposedly the progenitors of the young clusters for a star formation efficiency of a few percent, is comparable (alpha = -0.

The spatial relation between young star clusters and molecular clouds in M51 with LEGUS

10.1093/mnras/sty3473

## Likewise, we found young clusters, at present located in the inner regions of both MCs, formed out of gas that has remained unmixed since several Gyr ago.

Metallicity estimates of young clusters in the Magellanic Clouds from Strömgren photometry of supergiant stars

10.1093/mnras/stz2820

## We study ∼700 young clusters (≤10 Myr) in three nearby spiral galaxies (NGC 7793, NGC 4395, and NGC 1313) using Hubble Space Telescope (HST) imaging from LEGUS (Legacy ExtraGalactic Ultraviolet Survey).

H α morphologies of star clusters: a LEGUS study of H ii region evolution time-scales and stochasticity in low-mass clusters

10.1051/0004-6361/201936409

## Our study not only reinforces the notion that some young clusters like NGC 1866 harbor multiple populations, but gives also hints that the first population, the older, may inherit the angular momentum from the parent cloud while stars of the second one, the younger, do not.

Multiple stellar populations in NGC 1866. New clues from Cepheids and colour-magnitude diagram

10.1051/0004-6361/201936549

## Extended main-sequence turn-offs (eMSTO) are a commonly observed property of young clusters.

Isochrone-cloud fitting of the extended Main-Sequence Turn-Off of young clusters

10.5303/JKAS.2019.52.5.145

## All of the 655 cluster candidates have a well defined main-sequence except for two candidates if we consider that the main sequence of very young clusters is somewhat broad due to differential extinction.

207 New Open Star Clusters within 1 kpc from Gaia Data Release 2.

10.1051/0004-6361/201834693

## We derive parameters such as age, distance modulus and extinction for a sample of 269 open clusters, selecting only low reddening objects and discarding very young clusters, for which techniques other than isochrone-fitting are more suitable for estimating ages.

Age determination for 269 $Gaia$ DR2 Open Clusters

10.25518/0037-9565.8723

## Here we provide an overview of optical photometric observations of the young clusters, identification of variable nature from their light curves, characterization of their circumstellar disk.

Rotation rates of pre-main sequence stars: role of circumstellar disk

10.3847/1538-4357/ab3df9

## These observations shed light on the frequency of the ejection events in young clusters.

Runaway Young Stars in the Orion Nebula

10.3847/1538-4357/ab4ae3

## Young clusters and associations hold clues to the origin and properties of multiple star systems.

A Search for Intermediate Separation Low Mass Binaries in the Orion Nebula Cluster

10.1093/mnrasl/slz135

## This finding is important for understanding the physics of the MP phenomenon, as these young clusters can provide much stronger constraints (e.

An extragalactic chromosome map: the intermediate-age SMC cluster Lindsay 1

## Multiwavelength observations show that Abell 1367 (A1367) is a dynamically young cluster, with at least two subclusters merging along the SE–NW direction.

A merger shock in Abell 1367

10.3847/1538-4357/ab15d2

## We suggest that variable stars, binary interactions, and stellar rotation affect the eMSTO morphology of these very young clusters.

Extended main-sequence turnoffs in the double cluster $h$ and $\chi$ Persei: The complex role of stellar rotation

10.1051/0004-6361/201936283

## The Scutum complex in the inner disk of the Galaxy hosts a number of young clusters and associations of red supergiant stars that are heavily obscured by dust extinction.

Stellar population astrophysics (SPA) with the TNG. GIANO-B spectroscopy of red supergiants in Alicante 7 and Alicante 10.

10.1051/0004-6361/201936921

## We have undertaken a similar analysis for 61 B-type similar targets, towards the young cluster, NGC 346 in the Small Magellanic Cloud (SMC).

The NGC 346 massive star census. Nitrogen abundances for apparently single, narrow lined, hydrogen core burning B-type stars

10.3847/1538-4357/ab5303

## 1 Msun not associated with a young cluster.

WISE2150-7520AB: A very low mass, wide co-moving brown dwarf system discovered through the citizen science project Backyard Worlds: Planet 9.

## It is shown that the shallow, power-law density profiles characteristic of young clusters is predicted by the hierarchical star formation scenario.

The Role of Stellar Feedback in Star Cluster Formation

10.1051/0004-6361/201935415

## Spectroscopy for 247 stars towards the young cluster NGC 346 in the Small Magellanic Cloud has been combined with that for 116 targets from the VLT-FLAMES Survey of Massive Stars.

A census of massive stars in NGC 346. Stellar parameters and rotational velocities

10.1051/0004-6361/201935107

## 5If* star RFS8 ($\sim$70 $M_{\odot}$), found within $\approx$ 53 and 58 pc respectively from the Galactic massive young cluster NGC 3603, using Gaia data.

On the origin of very massive stars around NGC 3603

10.1093/mnras/sty2898

## In this work we report the discovery of a young cluster of asteroids that originated by the breakup of an asteroid member of the (221)Eos family.

Discovery of a young subfamily of the (221) Eos asteroid family

10.1051/0004-6361/201833877

## (abridged) NGC6530 is a young cluster with a complex morphology and star-formation history.

Wide-area photometric and astrometric (Gaia DR2) study of the young cluster NGC 6530

## W40 is a blistered Hii region, and Serpens South is an infrared dark cloud accompanied by a young cluster.

Cluster formation in the W 40 and Serpens South complex triggered by the expanding H ii region

10.1093/MNRASL/SLZ049

## Multiwavelength observations show that Abell 1367 (A1367) is a dynamically young cluster, with at least two subclusters merging along the SE–NW direction.

A merger shock in Abell 1367.