scholarly journals Astrophysical properties of binary star clusters in the Small Magellanic Cloud

2009 ◽  
Vol 5 (S266) ◽  
pp. 533-536
Author(s):  
João F. C. Santos ◽  
Alex A. Schmidt ◽  
Eduardo Bica
Keyword(s):  
Star Formation ◽  
Age Differences ◽  
Binary Star ◽  
Star Clusters ◽  
Magellanic Cloud ◽  
Age Difference ◽  
Small Magellanic Cloud ◽  
Density Profiles ◽  
Physical Connection ◽  
Stellar Density

AbstractTo study the evolution of binary star clusters, we have imaged seven systems in the Small Magellanic Cloud with the SOAR 4m telescope using B and V filters. The sample contains pairs with well-separated components (d < 30 pc) as well as systems that apparently have merged, as evidenced by their unusual structures. By employing isochrone fitting to their color–magnitude diagrams, we have determined reddening values, ages and metallicities, and by fitting King models to their radial stellar-density profiles we estimated core radii. Disturbances of the density profiles are interpreted as evidence of interactions. Properties such as the distances between their components and their age differences are addressed in terms of the timescales involved, to assess the physical connection of the system. In two cases, the age difference is more than 50 Myr, which suggests a chance alignment, capture or sequential star formation.

scholarly journals Disruption of giant molecular clouds and formation of bound star clusters under the influence of momentum stellar feedback

2019 ◽  
Vol 487 (1) ◽  
pp. 364-380 ◽  
Author(s):  
Hui Li ◽  
Mark Vogelsberger ◽  
Federico Marinacci ◽  
Oleg Y Gnedin
Keyword(s):  
Star Formation ◽  
Molecular Clouds ◽  
Star Clusters ◽  
Giant Molecular Clouds ◽  
Density Profiles ◽  
Stellar Feedback ◽  
Wide Range ◽  
Gas Removal ◽  
Formation Efficiency ◽  
Stellar Density

Abstract Energetic feedback from star clusters plays a pivotal role in shaping the dynamical evolution of giant molecular clouds (GMCs). To study the effects of stellar feedback on the star formation efficiency of the clouds and the dynamical response of embedded star clusters, we perform a suite of isolated GMC simulations with star formation and momentum feedback subgrid models using the moving-mesh hydrodynamics code Arepo. The properties of our simulated GMCs span a wide range of initial mass, radius, and velocity configurations. We find that the ratio of the final stellar mass to the total cloud mass, ϵint, scales strongly with the initial cloud surface density and momentum feedback strength. This correlation is explained by an analytic model that considers force balancing between gravity and momentum feedback. For all simulated GMCs, the stellar density profiles are systematically steeper than that of the gas at the epochs of the peaks of star formation, suggesting a centrally concentrated stellar distribution. We also find that star clusters are always in a sub-virial state with a virial parameter ∼0.6 prior to gas expulsion. Both the sub-virial dynamical state and steeper stellar density profiles prevent clusters from dispersal during the gas removal phase of their evolution. The final cluster bound fraction is a continuously increasing function of ϵint. GMCs with star formation efficiency smaller than 0.5 are still able to form clusters with large bound fractions.

scholarly journals The Oldest Star Clusters in the Small Magellanic Cloud

1999 ◽  
Vol 190 ◽  
pp. 445-445 ◽  
Author(s):  
Kenneth J. Mighell ◽  
Ata Sarajedini ◽  
Rica S. French
Keyword(s):  
Star Formation ◽  
Theoretical Model ◽  
Observational Data ◽  
Hubble Space Telescope ◽  
Star Clusters ◽  
Magellanic Cloud ◽  
Wide Field ◽  
Small Magellanic Cloud ◽  
Formation Model ◽  
Age Sequence

We present our analysis of archival Hubble Space Telescope Wide Field Planetary Camera 2 (WFPC2) observations in F450W (~B) and F555W (~V) of the intermediate-age populous star clusters NGC 121, NGC 339, NGC 361, NGC 416, and Kron 3 in the Small Magellanic Cloud. We use published photometry of two other SMC populous star clusters, Lindsay 1 and Lindsay 113, to investigate the age sequence of these seven star clusters in order to improve our understanding of the formation chronology of the SMC. We analyzed the V vs B–V and MV vs (B–V)o color-magnitude diagrams of these populous Small Magellanic Cloud star clusters using a variety of techniques and determined their ages, metallicities, and reddenings. These new data enable us to improve the age-metallicity relation of star clusters in the Small Magellanic Cloud. In particular, we find that a closed-box continuous star-formation model does not reproduce the age-metallicity relation adequately. However, a theoretical model punctuated by bursts of star formation is in better agreement with the observational data. The full details of this analysis are reported in Mighell, Sarajedini, & French (1998, AJ, 116, 2395).

scholarly journals Ages and Metallicities of Five Intermediate-Age Star Clusters Projected Towards the Small Magellanic Cloud

2002 ◽  
Vol 207 ◽  
pp. 196-198
Author(s):  
Juan J. Clariá ◽  
Andrés E. Piatti ◽  
João F. C. Santos ◽  
Eduardo Bica ◽  
Ata Sarajedini ◽  
...  
Keyword(s):  
Star Formation ◽  
Chemical Evolution ◽  
Central Body ◽  
Age Distribution ◽  
Star Clusters ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Ccd Photometry ◽  
Cluster Age

Washington CCD photometry of intermediate-age clusters in the Small Magellanic Cloud (SMC) is presented. The cluster age distribution in the SMC suggests formation epochs at 3 and 6 Gyr, respectively. Recent star formation is confined to the central body of the SMC. The chemical evolution of the SMC appears to be best represented by bursty models.

scholarly journals Star formation in the Small Magellanic Cloud: the youngest star clusters

2006 ◽  
Vol 2 (S237) ◽  
pp. 199-203
Author(s):  
E. Sabbi ◽  
A. Nota ◽  
M. Sirianni ◽  
L. R. Carlson ◽  
M. Tosi ◽  
...  
Keyword(s):  
Star Formation ◽  
Milky Way ◽  
Cluster Formation ◽  
Star Clusters ◽  
Magellanic Cloud ◽  
Dust Content ◽  
Small Magellanic Cloud ◽  
Preliminary Results ◽  
Low Metallicity ◽  
Cluster Program

AbstractWe recently launched a comprehensive ground based (ESO/VLT/NTT) and space (HST & SST) study of the present and past star formation in the Small Magellanic Cloud (SMC), in clusters and in the field, with the goal of understanding how star and cluster formation occur and propagate in an environment of low metallicity, with a gas and dust content that is significantly lower than in the Milky Way. In this paper, we present some preliminary results of the “young cluster” program, where we acquired deep F555W (~V), and F814W (~I) HST/ACS images of the four young and massive SMC star clusters: NGC 346, NGC 602, NGC 299, and NGC 376.

scholarly journals Star formation in the Small Magellanic Cloud: the youngest star clusters

2009 ◽  
Vol 324 (2-4) ◽  
pp. 101-107
Author(s):  
E. Sabbi ◽  
A. Nota ◽  
J. S. Gallagher ◽  
M. Tosi ◽  
L. R. Carlson ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Clusters ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud

scholarly journals An overview of the structure and kinematics of the Magellanic Clouds

1991 ◽  
Vol 148 ◽  
pp. 15-23 ◽  
Author(s):  
B. E. Westerlund
Keyword(s):  
Star Formation ◽  
Observational Data ◽  
Spiral Structure ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
Line Of Sight ◽  
Small Magellanic Cloud ◽  
Complex Velocity ◽  
The Past

A vast amount of observational data concerning the structure and kinematics of the Magellanic Clouds is now available. Many basic quantities (e.g. distances and geometry) are, however, not yet sufficiently well determined. Interactions between the Small Magellanic Cloud (SMC), the Large Magellanic Cloud (LMC) and our Galaxy have dominated the evolution of the Clouds, causing bursts of star formation which, together with stochastic self-propagating star formation, produced the observed structures. In the youngest generation in the LMC it is seen as an intricate pattern imitating a fragmented spiral structure. In the SMC much of the fragmentation is along the line of sight complicating the reconstruction of its history. The violent events in the past are also recognizable in complex velocity patterns which make the analysis of the kinematics of the Clouds difficult.

scholarly journals Age and metallicity of star clusters in the Small Magellanic Cloud from integrated spectroscopy

2010 ◽  
Vol 520 ◽  
pp. A85 ◽  
Author(s):  
B. Dias ◽  
P. Coelho ◽  
B. Barbuy ◽  
L. Kerber ◽  
T. Idiart
Keyword(s):  
Star Clusters ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud

scholarly journals Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud

2005 ◽  
Vol 440 (1) ◽  
pp. 111-120 ◽  
Author(s):  
A. E. Piatti ◽  
J. F. C. Santos ◽  
J. J. Clariá ◽  
E. Bica ◽  
A. V. Ahumada ◽  
...  
Keyword(s):  
Spectral Analysis ◽  
Star Clusters ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud
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