Star cluster formation and evolution in nearby starburst galaxies -- II. Initial conditions

AbstractWe present a model for hydrodynamic + N-body simulations of star cluster formation and evolution using AMUSE. Our model includes gas dynamics, star formation in regions of dense gas, stellar evolution and a galactic tidal spiral potential, thus incorporating most of the processes that play a role in the evolution of star clusters.We test our model on initial conditions of two colliding molecular clouds as well as a section of a spiral arm from a previous galaxy simulation.

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Star cluster formation and evolution in nearby starburst galaxies -- I. Systematic uncertainties

Monthly Notices of the Royal Astronomical Society ◽

10.1046/j.1365-8711.2003.06536.x ◽

2003 ◽

Vol 342 (1) ◽

pp. 259-273 ◽

Cited By ~ 69

Author(s):

R. de Grijs ◽

U. Fritze-v. Alvensleben ◽

P. Anders ◽

J. S. Gallagher ◽

N. Bastian ◽

...

Keyword(s):

Cluster Formation ◽

Starburst Galaxies ◽

Star Cluster ◽

Systematic Uncertainties ◽

Formation And Evolution

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Star Cluster Encounters in the Magellanic Clouds

Symposium - International Astronomical Union ◽

10.1017/s0074180900118509 ◽

1999 ◽

Vol 190 ◽

pp. 443-444

Author(s):

M.R. de Oliveria ◽

H. Dottori ◽

E. Bica

Keyword(s):

Initial Conditions ◽

Past History ◽

Cluster Formation ◽

Star Cluster ◽

Magellanic Clouds ◽

The Past ◽

Sky Survey ◽

History Of ◽

Fundamental Insight ◽

Selection Of

The study of star cluster pairs in the Magellanic Clouds (MCs) has been explored extensively in the past years (Bhatia & Hatzidimitriou 1988; Rodrigues et al. 1994; de Oliveira et al. 1998). The evolution of these pairs can provide fundamental insight into the past history of cluster formation in the MCs.We have selected MC clusters (Bica & Schmitt 1995; Bica et al. 1998) with morphologies resembling those of the present models. The images in this selection of pairs were obtained from the Digital Sky Survey (DSS). We have also performed N-body simulations of star cluster encounters under different initial conditions, with the total number of particles per simulation ranging from 1024 to 20480.

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3 things they don’t tell you about star clusters

Proceedings of the International Astronomical Union ◽

10.1017/s1743921319007312 ◽

2019 ◽

Vol 14 (S351) ◽

pp. 40-46 ◽

Cited By ~ 1

Author(s):

Florent Renaud

Keyword(s):

Dark Matter ◽

Galaxy Formation ◽

Cluster Formation ◽

Star Clusters ◽

Matter Content ◽

Star Cluster ◽

Stellar Systems ◽

Holistic View ◽

Cosmological Context ◽

Formation And Evolution

AbstractDense stellar systems in general and star clusters in particular have recently regained the interest of the extragalactic and even cosmology communities, due to the role they could play as actors and probes of re-ionization, galactic archeology and the dark matter content of galaxies, among many others. In the era of the exploitation and the preparation of large stellar surveys (Gaia, APOGEE, 4MOST, WEAVE), of the detection of gravitational waves mostly originating from dense regions like the cores of clusters (Ligo, LISA), and in an always more holistic view of galaxy formation (HARMONI, Euclid, LSST†), a complete theory on the formation and evolution of clusters is needed to interpret the on-going and forthcoming data avalanche. In this context, the community carries an effort to model the aspects of star cluster formation and evolution in galactic and even cosmological context. However, it is not always easy to understand the caveats and the shortcuts taken in theories and simulations, and their implications on the conclusions drawn. I take the opportunity of this document to highlight three of these topics and discuss why some shortcuts taken by the community are or could be misleading.

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Young massive clusters in the interacting LIRG Arp 299: evidence for the dependence of star cluster formation and evolution on environment

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/sty2837 ◽

2018 ◽

Vol 482 (2) ◽

pp. 2530-2554 ◽

Cited By ~ 4

Author(s):

Z Randriamanakoto ◽

P Väisänen ◽

S D Ryder ◽

P Ranaivomanana

Keyword(s):

Cluster Formation ◽

Star Cluster ◽

Formation And Evolution ◽

Massive Clusters

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Young massive clusters in Arp 299

Proceedings of the International Astronomical Union ◽

10.1017/s1743921319007701 ◽

2019 ◽

Vol 14 (S351) ◽

pp. 143-146

Author(s):

Zara Randriamanakoto ◽

Petri Väisänen

Keyword(s):

Star Formation ◽

Globular Clusters ◽

Cluster Formation ◽

Age Distribution ◽

Star Cluster ◽

Luminous Infrared Galaxies ◽

Star Formation Activity ◽

Formation And Evolution ◽

Using Data ◽

Formation Efficiency

AbstractBecause of their young ages and compact densities, young massive star clusters (YMCs) are widely considered as potential proto-globular clusters. They are ubiquitous in environments with ongoing star formation activity such as interacting luminous infrared galaxies. To determine the galactic environmental effects on the star cluster formation and evolution, we study the YMC population of Arp 299 (NGC 3690E/NGC 3690W) using data taken with the HST WFC3/UVIS camera. By fitting the multiband photometry with the Yggdrasil models, we derive the star cluster masses, ages and extinction. While the cluster mass-galactocentric radius relation of NGC 3690E indicates that there could be an influence of the gas density distribution on the cluster formation, the age distribution of the western component suggests that YMCs in that galaxy endure stronger disruption mechanisms. With a cluster formation efficiency of 19 percent, star formation happening in bound clusters in Arp 299 is 3–5 times higher than that of a typical normal spiral.

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Star cluster formation and evolution in Mrk 930: properties of a metal-poor starburst★

Monthly Notices of the Royal Astronomical Society ◽

10.1111/j.1365-2966.2011.18867.x ◽

2011 ◽

Vol 415 (3) ◽

pp. 2388-2406 ◽

Cited By ~ 21

Author(s):

A. Adamo ◽

G. Östlin ◽

E. Zackrisson ◽

P. Papaderos ◽

N. Bergvall ◽

...

Keyword(s):

Cluster Formation ◽

Star Cluster ◽

Formation And Evolution

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The star cluster age function in the Galactic disc with Gaia DR2

Astronomy and Astrophysics ◽

10.1051/0004-6361/202038532 ◽

2020 ◽

Vol 645 ◽

pp. L2

Author(s):

Friedrich Anders ◽

Tristan Cantat-Gaudin ◽

Irene Quadrino-Lodoso ◽

Mark Gieles ◽

Carme Jordi ◽

...

Keyword(s):

Open Cluster ◽

Cluster Formation ◽

Formation Rate ◽

Age Distribution ◽

Star Cluster ◽

Open Clusters ◽

Open Star Clusters ◽

Open Star ◽

Formation And Evolution ◽

Cluster Age

We perform a systematic reanalysis of the age distribution of Galactic open star clusters. Using a catalogue of homogeneously determined ages for 834 open clusters contained in a 2 kpc cylinder around the Sun and characterised with astrometric and photometric data from the Gaia satellite, we find that it is necessary to revise earlier works that relied on data from the Milky Way Star Cluster survey. After establishing age-dependent completeness limits for our sample, we find that the cluster age function in the range 6.5 < log t < 10 is compatible with Schechter-type or broken power-law functions. Our best-fit values indicate an earlier drop of the age function (by a factor of 2−3) with respect to the results obtained in the last five years, and are instead more compatible with results obtained in the early 2000s along with radio observations of inner-disc clusters. Furthermore, we find a typical destruction timescale of ∼1.5 Gyr for a 104 M⊙ cluster and a present-day cluster formation rate of 0.55−0.15+0.19 Myr−1 kpc−2, suggesting that only 16−8+11% of all stars born in the solar neighbourhood form in bound clusters. Accurate cluster-mass measurements are now needed to place more precise constraints on open-cluster formation and evolution models.

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Multiple stellar populations in massive LMC star clusters

Proceedings of the International Astronomical Union ◽

10.1017/s1743921308028627 ◽

2008 ◽

Vol 4 (S256) ◽

pp. 305-310

Author(s):

A. D. Mackey ◽

P. Broby Nielsen ◽

A. M. N. Ferguson ◽

J. C. Richardson

Keyword(s):

Globular Clusters ◽

Main Sequence ◽

Cluster Formation ◽

Star Clusters ◽

Stellar Populations ◽

Star Cluster ◽

Magellanic Clouds ◽

Formation And Evolution ◽

Galactic Globular Clusters

AbstractThe recent discovery of multiple stellar populations in massive Galactic globular clusters poses a serious challenge for models of star cluster formation and evolution. A new angle on this problem is being provided by rich intermediate-age clusters in the Magellanic Clouds. In this contribution we describe the discovery of three such LMC clusters with peculiar main-sequence turn-off morphologies. The simplest interpretation of our observations is that each of these three clusters is comprised of two or more stellar populations spanning an age interval of ~300 Myr. Surprisingly, such features may not be unusual in this type of cluster.

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