An H I Mosaic of the Small Magellanic Cloud

1995 ◽  
Vol 12 (1) ◽  
pp. 13-19 ◽  
Author(s):  
L. Staveley-Smith ◽  
R. J. Sault ◽  
D. McConnell ◽  
M. J. Kesteven ◽  
D. Hatzidimitriou ◽  
...  
Keyword(s):  
Star Formation ◽  
Neutral Hydrogen ◽  
Optical Emission ◽  
Magellanic Cloud ◽  
Molecular Gas ◽  
Small Magellanic Cloud ◽  
High Brightness ◽  
First Results ◽  
Low Metallicity ◽  
High Column

AbstractThis paper describes the first results from a 20 deg2 mosaic of the Small Magellanic Cloud (SMC) in the λ21-cm line of neutral hydrogen. The mosaic consists of 320 separate pointings with the 375-m array of the Australia Telescope Compact Array. The angular resolution is 1′· 5 (26 pc, for a distance of 60 kpc) and the velocity resolution is l·6kms−1. The images reveal a structure of remarkable complexity, with much of the spatial power contained in high-brightness temperature compact knots and filaments. Numerous wind-blown ‘bubbles’ and ‘supershells’ are evident in the data, both inside and outside the stellar confines of the SMC. Some high-density H I regions are seen to correlate with Hα regions, indicating sites of current star formation. However, many high-column-density H I regions are devoid of optical emission and may represent regions of future star formation. These regions may be under-abundant in diffuse molecular gas due to the high radiation field and low metallicity of the SMC.

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 STATE OF THE GAS AND THE RELATION BETWEEN GAS AND STAR FORMATION AT LOW METALLICITY: THE SMALL MAGELLANIC CLOUD

2011 ◽  
Vol 741 (1) ◽  
pp. 12 ◽  
Author(s):  
Alberto D. Bolatto ◽  
Adam K. Leroy ◽  
Katherine Jameson ◽  
Eve Ostriker ◽  
Karl Gordon ◽  
...  
Keyword(s):  
Star Formation ◽  
Magellanic Cloud ◽  
The State ◽  
Small Magellanic Cloud ◽  
Low Metallicity

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 The VMC survey – XIV. First results on the look-back time star formation rate tomography of the Small Magellanic Cloud★

2015 ◽  
Vol 449 (1) ◽  
pp. 639-661 ◽  
Author(s):  
Stefano Rubele ◽  
Léo Girardi ◽  
Leandro Kerber ◽  
Maria-Rosa L. Cioni ◽  
Andrés E. Piatti ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Look Back ◽  
First Results ◽  
The Look

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 ISO Observations of Compact HII Regions in the Large Magellanic Cloud

1999 ◽  
Vol 190 ◽  
pp. 377-378
Author(s):  
A. Moneti ◽  
R. J. Laureijs ◽  
J.M. van der Hulst ◽  
F. Israel ◽  
P.P. van der Werf
Keyword(s):  
Star Formation ◽  
Hii Regions ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
First Results ◽  
Reflection Nebulae ◽  
Compact Hii Regions

With the detection of strong PAH features and H2 emission in selected knots of the N159, N11A, and 30 Dor regions in the LMC, we present the first results of a study that is part of a coordinated Guaranteed Time ISO programme to investigate star formation in the Magellanic Clouds. The PAH features have different ratios than the ones in Galactic reflection nebulae.

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