scholarly journals Clustered Star Formation in the Small Magellanic Cloud. ASpitzer/IRAC View of the Star‐Forming Region NGC 602/N 90

2007 ◽  
Vol 665 (1) ◽  
pp. 306-314 ◽  
Author(s):  
Dimitrios A. Gouliermis ◽  
Sascha P. Quanz ◽  
Thomas Henning
Keyword(s):  
Star Formation ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Star Forming

scholarly journals Resolving the Transition from Molecular to Atomic at 1/5 Solar Metallicity in the Small Magellanic Cloud

2015 ◽  
Vol 11 (S315) ◽  
pp. 13-16
Author(s):  
Katherine E. Jameson ◽  
Alberto D. Bolatto ◽  
Mark Wolfire ◽  
Monica Rubio ◽  
Rodrigo Herrera Camus ◽  
...  
Keyword(s):  
Star Formation ◽  
High Resolution ◽  
Preliminary Evidence ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Star Forming ◽  
Solar Metallicity ◽  
Low Metallicity ◽  
Photodissociation Regions ◽  
First Time

AbstractAt a distance of 61 kpc, the Small Magellanic Cloud (SMC) affords an absolutely unique view of the low metallicity star-forming interstellar medium, providing the nearest laboratory to study processes relevant to star formation at high redshifts. We present new ALMA 7m-array maps of CO and 12CO (2-1) for one of the four observed regions in the Southwest Bar of the SMC. These maps are the first high-resolution (~6″ ~ 1.7 pc) images of CO in a molecular cloud at 1/5 Solar metallicity. We show the structure of photodissociation regions for the first time at 1/5 Solar metallicity by combining the new ALMA data with Herschel maps of [C ii] and [O i]. We present preliminary evidence that there is extended, faint 12CO (2-1) emission near where we expect the Hi-to-H2 transition. We also compare our data to the low metallicity 3D simulations by Glover & Mac Low (2011) and Shetty et al. (2011).

scholarly journals THE CLUSTERED NATURE OF STAR FORMATION. PRE-MAIN-SEQUENCE CLUSTERS IN THE STAR-FORMING REGION NGC 602/N90 IN THE SMALL MAGELLANIC CLOUD

2012 ◽  
Vol 748 (1) ◽  
pp. 64 ◽  
Author(s):  
Dimitrios A. Gouliermis ◽  
Stefan Schmeja ◽  
Andrew E. Dolphin ◽  
Mario Gennaro ◽  
Emanuele Tognelli ◽  
...  
Keyword(s):  
Star Formation ◽  
Main Sequence ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Star Forming

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 The Star‐forming Region NGC 346 in the Small Magellanic Cloud withHubble Space TelescopeACS Observations. II. Photometric Study of the Intermediate‐Age Star Cluster BS 90

2007 ◽  
Vol 664 (1) ◽  
pp. 322-331 ◽  
Author(s):  
Boyke Rochau ◽  
Dimitrios A. Gouliermis ◽  
Wolfgang Brandner ◽  
Andrew E. Dolphin ◽  
Thomas Henning
Keyword(s):  
Magellanic Cloud ◽  
Star Cluster ◽  
Photometric Study ◽  
Small Magellanic Cloud ◽  
Star Forming

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).

Formation History of Binary Clusters in the Large Magellanic Cloud

2018 ◽  
Vol 14 (S344) ◽  
pp. 118-121
Author(s):  
Rhorom Priyatikanto ◽  
Mochamad Ikbal Arifyanto ◽  
Rendy Darma ◽  
Aprilia ◽  
Muhamad Irfan Hakim
Keyword(s):  
Binary Star ◽  
Cluster Formation ◽  
Formation Rate ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Star Forming ◽  
Binary Clusters ◽  
Formation History ◽  
History Of

AbstractGlobal history of star or cluster formation in the Large Magellanic Cloud (LMC) has been the center of interest in several studies as it is thought to be influenced by tidal interaction with the Small Magellanic Cloud and even the Milky Way. This study focus on the formation history of the LMC in relation with the context of binary star clusters population, the apparent binary fraction (e.g., percentage of cluster pairs) in different epoch were calculated and analyzed. From the established distributions, it can be deduced that the binary clusters tend to be young (∽ 100 Myr) while their locations coincide with the locations of star forming complexes. There is an indication that the binary fraction increases as the rise of star formation rate in the last millions years. In the LMC, the increase of binary fraction at age ∽ 100 Myr can be associated to the last episode of close encounter with the Small Magellanic Cloud at ∽ 150 Myr ago. This observational evidence supports the theory of binary cluster formation through the fission of molecular cloud where the encounter between galaxies enhanced the clouds velocity dispersion which in turn increased the probability of cloud-cloud collisions that produce binary clusters.

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