scholarly journals ALMA Reveals a Cloud–Cloud Collision that Triggers Star Formation in the Small Magellanic Cloud

2021 ◽  
Vol 908 (2) ◽  
pp. L43
Author(s):  
Naslim Neelamkodan ◽  
Kazuki Tokuda ◽  
Susmita Barman ◽  
Hiroshi Kondo ◽  
Hidetoshi Sano ◽  
...  
Keyword(s):  
Star Formation ◽  
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 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 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 STAR FORMATION HISTORY IN TWO FIELDS OF THE SMALL MAGELLANIC CLOUD BAR

2012 ◽  
Vol 754 (2) ◽  
pp. 130 ◽  
Author(s):  
M. Cignoni ◽  
A. A. Cole ◽  
M. Tosi ◽  
J. S. Gallagher ◽  
E. Sabbi ◽  
...  
Keyword(s):  
Star Formation ◽  
Magellanic Cloud ◽  
Star Formation History ◽  
Small Magellanic Cloud ◽  
Formation History

scholarly journals MEAN AGE GRADIENT AND ASYMMETRY IN THE STAR FORMATION HISTORY OF THE SMALL MAGELLANIC CLOUD

2013 ◽  
Vol 775 (2) ◽  
pp. 83 ◽  
Author(s):  
M. Cignoni ◽  
A. A. Cole ◽  
M. Tosi ◽  
J. S. Gallagher ◽  
E. Sabbi ◽  
...  
Keyword(s):  
Star Formation ◽  
Magellanic Cloud ◽  
Star Formation History ◽  
Small Magellanic Cloud ◽  
Formation History ◽  
History Of

scholarly journals N-Body Simulations of the Magellanic System Including Gas Dynamics and Star Formation

1999 ◽  
Vol 186 ◽  
pp. 60-60
Author(s):  
A.M. Yoshizawa ◽  
M. Noguchi
Keyword(s):  
Star Formation ◽  
Gas Dynamics ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
Small Magellanic Cloud ◽  
Tidal Distortion ◽  
Formation And Evolution ◽  
Magellanic Stream ◽  
Magellanic System

The system of the Magellanic Clouds is considered to be dynamically interacting among themselves and with our Galaxy. This interaction is thought to be the cause of many complicated features seen in the Magellanic Clouds and the Magellanic Stream (see Westerlund 1990, A&AR, 2, 27). In order to better understand the formation and evolution of the Magellanic System, we carry out realistic N-body simulations of the tidal distortion of the Small Magellanic Cloud (SMC) due to our Galaxy and the Large Magellanic Cloud (LMC).

Intermediate-age and Old Populations in the Small Magellanic Cloud

1999 ◽  
Vol 190 ◽  
pp. 299-305 ◽  
Author(s):  
D. Hatzidimitriou
Keyword(s):  
Star Formation ◽  
Magellanic Cloud ◽  
Star Formation History ◽  
Small Magellanic Cloud ◽  
Formation History ◽  
History Of ◽  
The Subject

The star formation history and kinematics of intermediate-age and old populations in the Small Magellanic Cloud are the subject of this brief review. New results confirm the occurrence of a period of enhanced SF about 8–10 Gyr ago in the SMC. Younger populations are confirmed to be more centrally concentrated than older ones. The SMC, at least in the areas studied (which do not include the Bar) seems to have had a different history of star formation from the LMC. Although the kinematics of the SMC have been extensively studied, it is still unclear if there are distinct Bar, disk and halo components, or if all populations share the same kinematics.

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