scholarly journals Star Cluster Evolution: From Young Massive Star Clusters to Old Globulars

2009 ◽  
pp. 353-356
Author(s):  
Richard de Grijs
Keyword(s):  
Massive Star ◽  
Star Clusters ◽  
Star Cluster ◽  
Cluster Evolution

scholarly journals Massive star clusters in galaxies

2010 ◽  
Vol 368 (1913) ◽  
pp. 889-906 ◽  
Author(s):  
William E. Harris
Keyword(s):  
Recent Work ◽  
Globular Clusters ◽  
Evolutionary History ◽  
Massive Star ◽  
Star Clusters ◽  
Star Cluster ◽  
Cluster System ◽  
History Of ◽  
Review Current

The ensemble of all star clusters in a galaxy constitutes its star cluster system . In this review, the focus of the discussion is on the ability of star clusters, particularly the systems of old massive globular clusters (GCs), to mark the early evolutionary history of galaxies. I review current themes and key findings in GC research, and highlight some of the outstanding questions that are emerging from recent work.

scholarly journals Massive star cluster formation and evolution in tidal dwarf galaxies

2019 ◽  
Vol 628 ◽  
pp. A60 ◽  
Author(s):  
Jérémy Fensch ◽  
Pierre-Alain Duc ◽  
Médéric Boquien ◽  
Debra M. Elmegreen ◽  
Bruce G. Elmegreen ◽  
...  
Keyword(s):  
Globular Clusters ◽  
Massive Star ◽  
Dwarf Galaxies ◽  
Cluster Formation ◽  
Spectral Energy Distribution ◽  
Star Clusters ◽  
Star Cluster ◽  
Spectral Energy ◽  
Physical Parameters ◽  
Near Ultraviolet

Context. The formation of globular clusters remains an open debate. Dwarf starburst galaxies are efficient at forming young massive clusters with similar masses as globular clusters and may hold the key to understanding their formation. Aims. We study star cluster formation in a tidal debris, including the vicinity of three tidal dwarf galaxies, in a massive gas-dominated collisional ring around NGC 5291. These dwarfs have physical parameters that differ significantly from local starbursting dwarfs. They are gas rich, highly turbulent, their gas metallicity is already enriched up to half solar values, and they are expected to be free of dark matter. The aim is to study massive star cluster formation in this as yet unexplored type of environment. Methods. We used imaging from the Hubble Space Telescope using broadband filters that cover the wavelength range from the near-ultraviolet to the near-infrared. We determined the masses and ages of the cluster candidates by using the spectral energy distribution-fitting code CIGALE. We considered age-extinction degeneracy effects on the estimation of the physical parameters. Results. We find that the tidal dwarf galaxies in the ring of NGC 5291 are forming star clusters with an average efficiency of ∼40%, which is similar to blue compact dwarf galaxies. We also find massive star clusters for which the photometry suggests that they were formed at the very birth of the tidal dwarf galaxies. These clusters have survived for several hundred million years. Therefore our study shows that extended tidal dwarf galaxies and compact clusters may be formed simultaneously. In the specific case observed here, the young star clusters are not massive enough to survive for a Hubble time. However, it may be speculated that similar objects at higher redshift, with a higher star formation rate, might form some of the long-lived globular clusters.

scholarly journals Ages and Masses of Star Clusters in M33: a Multiwavelength Study

2021 ◽  
Vol 163 (1) ◽  
pp. 16
Author(s):  
Caitlin Moeller ◽  
Daniela Calzetti
Keyword(s):  
Spectral Energy Distribution ◽  
Star Clusters ◽  
Young Star ◽  
Star Cluster ◽  
Spectral Energy ◽  
Physical Parameters ◽  
Nearby Galaxy ◽  
Population Synthesis ◽  
Cluster Evolution ◽  
The Masses

Abstract We combine archival images for the nearby galaxy M33 (Triangulum Galaxy) from the ultraviolet (UV) to the infrared to derive ages, masses, and extinctions for the young star cluster population, and compare our physical parameters with published ones. Our goal is to test the robustness of clusters ages and masses, and possibly improve on existing ones both by expanding the wavelength range of the spectral-energy distribution (SED) fits and by using more recent population synthesis models. The rationale for this experiment is to verify the sensitivity of the clusters physical parameters to observational setups and model choices that span those commonly found in the literature. We derive the physical parameters of 137 clusters, using SEDs measured in eight UV-to-I bands, including Hα, from GALEX and ground-based images. We also add the 24 μm image from the Spitzer Space Telescope to help break some age degeneracies. We find that our derived cluster ages show significant differences with earlier determinations, while the masses remain relatively insensitive to the fitting approach adopted. We also highlight an already known difficulty in recovering old, low-extinction clusters, as SED-fitting codes tend to prefer younger, higher extinction solutions when the extinction is a free parameter. We publish updated ages, masses, and extinctions, with uncertainties for all sample star clusters, together with their photometry. Given the proximity of M33, this represents an important population to secure for the study of star formation and cluster evolution in spirals.

scholarly journals Effects of Stellar Collisions on Star Cluster Evolution and Core Collapse

2007 ◽  
Vol 3 (S246) ◽  
pp. 151-155 ◽  
Author(s):  
Sourav Chatterjee ◽  
John M. Fregeau ◽  
Frederic A. Rasio
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Simulations ◽  
Massive Stars ◽  
Relaxation Times ◽  
Star Clusters ◽  
Dynamical Evolution ◽  
Star Cluster ◽  
Core Collapse ◽  
Cluster Evolution ◽  
Stellar Collisions

AbstractWe systematically study the effects of collisions on the overall dynamical evolution of dense star clusters using Monte Carlo simulations over many relaxation times. We derive many observable properties of these clusters, including their core radii and the radial distribution of collision products. We also study different aspects of collisions in a cluster taking into account the shorter lifetimes of more massive stars, which has not been studied in detail before. Depending on the lifetimes of the significantly more massive collision products, observable properties of the cluster can be modified qualitatively; for example, even without binaries, core collapse can sometimes be avoided simply because of stellar collisions.

scholarly journals Super star clusters in Hii galaxies

2009 ◽  
Vol 5 (S266) ◽  
pp. 447-450
Author(s):  
Patricio Lagos ◽  
Eduardo Telles ◽  
E. R. Carrasco
Keyword(s):  
Spatial Distribution ◽  
Star Formation ◽  
Massive Star ◽  
Star Clusters ◽  
Dominant Mode ◽  
Star Cluster ◽  
The Galaxy ◽  
Super Star Clusters ◽  
Field Unit ◽  
The Masses

AbstractWe summarize our results based on observations with the NIRI camera on the Gemini North telescope of three Hii galaxies (Mrk 36, UM 408 and UM 461), obtained to identify and determine the ages and masses of the elementary components (the star cluster population) of the starburst regions in compact Hii galaxies. Our preliminary results indicate that the masses of the stellar clusters in these galaxies range from ~104 to ~106 M⊙, with associated ages of a few Myr. The most massive star clusters fall in the so-called super star cluster category. The identification of these clusters suggests that the formation and evolution of massive star clusters is the dominant mode of star formation in these galaxies. Their spatial distribution and ages seem to indicate that star formation is simultaneous over these timescales in some of our objects. We also review our recent description of the spatial distribution of physical conditions in the Hii galaxy UM 408 using the GMOS integral-field unit on Gemini South. The spatial distribution of the oxygen abundance does not show any significant variation or gradient across the galaxy on scales of hundreds of parsecs, within our observational uncertainties, confirming that this compact Hii galaxy, like other previously studied dwarf irregular galaxies, is chemically homogeneous.

scholarly journals Effects of Stellar-Mass Black Holes on Massive Star Cluster Evolution

2015 ◽  
Vol 12 (S316) ◽  
pp. 234-239
Author(s):  
Sourav Chatterjee ◽  
Meagan Morscher ◽  
Carl L. Rodriguez ◽  
Bharat Pattabiraman ◽  
Frederic A. Rasio
Keyword(s):  
Globular Clusters ◽  
Massive Star ◽  
Star Clusters ◽  
Mass Function ◽  
Stellar Mass ◽  
Cluster Center ◽  
Cluster Evolution ◽  
Large Populations ◽  
Direct Contrast ◽  
Mass Segregation

AbstractRecent observations have revealed the existence of stellar mass black hole (BH) candidates in some globular clusters (GC) in the Milky Way and in other galaxies. Given that the detection of BHs is challenging, these detections likely indicate the existence of large populations of BHs in these clusters. This is in direct contrast to the past understanding that at most a handful of BHs may remain in old GCs due to quick mass segregation and rapid mutual dynamical ejection. Modern realistic star-by-star numerical simulations suggest that the retention fraction of BHs is typically much higher than what was previously thought. The BH dynamics near the cluster center leads to dynamical formation of new binaries and dynamical ejections, and acts as a persistent and significant energy source for these clusters. We have started exploring effects of BHs on the global evolution and survival of star clusters. We find that the evolution as well as survival of massive star clusters can critically depend on the details of the initial assumptions related to BH formation physics, such as natal kick distribution, and the initial stellar mass function (IMF). In this article we will present our latest results.

scholarly journals Super massive star clusters: from superwinds to a cooling catastrophe and the re-processing of the injected gas

2006 ◽  
Vol 2 (S237) ◽  
pp. 242-245
Author(s):  
S. Silich ◽  
G. Tenorio-Tagle ◽  
C. Muñoz-Tuñón ◽  
J. Palouš
Keyword(s):  
Positive Feedback ◽  
Massive Star ◽  
Threshold Energy ◽  
Star Clusters ◽  
Star Cluster ◽  
Stellar Winds ◽  
Star Forming ◽  
Radiative Regime

AbstractDifferent hydrodynamic regimes for the gaseous outflows generated by multiple supernovae explosions and stellar winds occurring within compact and massive star clusters are discussed. It is shown that there exists the threshold energy that separates clusters whose outflows evolve in the quasi-adiabatic or radiative regime from those within which catastrophic cooling and a positive feedback star-forming mode sets in. The role of the surrounding ISM and the observational appearance of the star cluster winds evolving in different hydrodynamic regimes are also discussed.

scholarly journals Super Star Clusters in NGC 7673 and Mrk 8

2002 ◽  
Vol 207 ◽  
pp. 464-467
Author(s):  
N. Homeier ◽  
J.S. Gallagher
Keyword(s):  
Star Formation ◽  
Emission Line ◽  
Massive Star ◽  
Hubble Space Telescope ◽  
Star Clusters ◽  
Star Cluster ◽  
Population Synthesis ◽  
Massive Star Formation ◽  
Super Star Clusters ◽  
Intense Star Formation

We present an analysis of super star cluster populations using WFPC 2 on theHubble Space Telescopefor two starburst galaxies: NGC 7673 and Markarian 8. Both galaxies are luminious and have signatures of massive star formation, such as emission-line dominated optical spectra. Their optical appearances are highly disturbed, featuring prominent knots of intense star formation. Using HST F255W, F555W, and F814W images, we perform aperture photometry for a select sample of star clusters in different regions of each galaxy, and compare the results with evolutionary population synthesis models.

scholarly journals Simulations of Massive Star Cluster Formation and Feedback in Turbulent Giant Molecular Clouds

2010 ◽  
Vol 6 (S270) ◽  
pp. 235-238 ◽  
Author(s):  
Elizabeth Harper-Clark ◽  
Norman Murray
Keyword(s):  
Star Formation ◽  
Molecular Clouds ◽  
Massive Star ◽  
Cluster Formation ◽  
Star Clusters ◽  
Star Cluster ◽  
Giant Molecular Clouds

AbstractUsing the AMR code ENZO we are simulating the formation of massive star clusters within turbulent Giant Molecular Clouds (GMCs). Here we discuss the simulations from the first stages of building realistic turbulent GMCs, to accurate star formation, and ultimately comprehensive feedback. These simulations aim to build a better understanding of how stars affect GMCs, helping to answer the questions of how long GMCs live and why only a small fraction of the GMC gas becomes stars.

scholarly journals On the Origin of Complex Stellar Populations in Star Clusters

2007 ◽  
Vol 3 (S246) ◽  
pp. 71-72
Author(s):  
J. Pflamm-Altenburg ◽  
P. Kroupa
Keyword(s):  
Star Formation ◽  
Globular Clusters ◽  
Massive Star ◽  
Cluster Formation ◽  
Star Clusters ◽  
Stellar Populations ◽  
Star Cluster ◽  
Young Stars

AbstractThe existence of complex stellar populations in some star clusters challenges the understanding of star formation. E.g. the ONC or the sigma Orionis cluster host much older stars than the main bulk of the young stars. Massive star clusters (ω Cen, G1, M54) show metallicity spreads corresponding to different stellar populations with large age gaps. We show that (i) during star cluster formation field stars can be captured and (ii) very massive globular clusters can accrete gas from a long-term embedding inter stellar medium and restart star formation.

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