The Complete Far Ultraviolet Spectroscopic Explorer Spectrum of the Small Magellanic Cloud Star Sk 108

2003 ◽  
Vol 147 (2) ◽  
pp. 265-303 ◽  
Author(s):  
Christoforos Mallouris
Keyword(s):  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Far Ultraviolet

scholarly journals Far‐Ultraviolet and Hα Spectroscopy of SNR 0057−7226 in the Small Magellanic Cloud HiiRegion N66

2003 ◽  
Vol 586 (2) ◽  
pp. 1179-1190 ◽  
Author(s):  
Charles W. Danforth ◽  
Ravi Sankrit ◽  
William P. Blair ◽  
J. Christopher Howk ◽  
You‐Hua Chu
Keyword(s):  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Far Ultraviolet

scholarly journals Far‐Ultraviolet and X‐Ray Observations of the Reverse Shock in the Small Magellanic Cloud Supernova Remnant 1E 0102.2−7219

2006 ◽  
Vol 642 (1) ◽  
pp. 260-269 ◽  
Author(s):  
Manami Sasaki ◽  
Terrance J. Gaetz ◽  
William P. Blair ◽  
Richard J. Edgar ◽  
Jon A. Morse ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Reverse Shock ◽  
X Ray ◽  
Far Ultraviolet

scholarly journals OBSERVATIONS OF FAR-ULTRAVIOLET DIFFUSE EMISSION FROM THE SMALL MAGELLANIC CLOUD

2011 ◽  
Vol 743 (1) ◽  
pp. 80 ◽  
Author(s):  
Ananta C. Pradhan ◽  
Jayant Murthy ◽  
Amit Pathak
Keyword(s):  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Diffuse Emission ◽  
Far Ultraviolet

Far Ultraviolet Spectroscopic ExplorerObservations of Interstellar Gas toward the Small Magellanic Cloud Star Sk 108

2001 ◽  
Vol 558 (1) ◽  
pp. 133-144 ◽  
Author(s):  
C. Mallouris ◽  
D. E. Welty ◽  
D. G. York ◽  
H. W. Moos ◽  
K. R. Sembach ◽  
...  
Keyword(s):  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Interstellar Gas ◽  
Far Ultraviolet

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 A new super-soft X-ray source in the Small Magellanic Cloud: Discovery of the first Be/white dwarf system in the SMC?

2012 ◽  
Vol 537 ◽  
pp. A76 ◽  
Author(s):  
R. Sturm ◽  
F. Haberl ◽  
W. Pietsch ◽  
M. J. Coe ◽  
S. Mereghetti ◽  
...  
Keyword(s):  
White Dwarf ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
X Ray

scholarly journals UVIT-HST-Gaia-VISTA study of KRON 3 in the Small Magellanic Cloud: A cluster with an extended red clump in UV

2021 ◽  
Author(s):  
P K Nayak ◽  
A Subramaniam ◽  
S Subramanian ◽  
S Sahu ◽  
C Mondal ◽  
...  
Keyword(s):  
Near Infrared ◽  
Spectral Energy Distribution ◽  
Variable Mass ◽  
Intrinsic Property ◽  
Small Variation ◽  
Magellanic Cloud ◽  
Spectral Energy ◽  
Small Range ◽  
Small Magellanic Cloud ◽  
Red Clump

Abstract We have demonstrated the advantage of combining multi-wavelength observations, from the ultraviolet (UV) to near-infrared, to study Kron 3, a massive star cluster in the Small Magellanic Cloud. We have estimated the radius of the cluster Kron 3 to be 2${_{.}^{\prime}}$0 and for the first time, we report the identification of NUV-bright red clump (RC) stars and the extension of the RC in colour and magnitude in the NUV versus (NUV−optical) colour-magnitude diagram (CMD). We found that extension of the RC is an intrinsic property of the cluster and it is not due to contamination of field stars or differential reddening across the field. We studied the spectral energy distribution of the RC stars, and estimated a small range in temperature ∼5000–5500 K, luminosity ∼60–90 L⊙ and radius ∼8.0–11.0 R⊙ supporting their RC nature. The range of UV magnitudes amongst the RC stars (∼23.3 to 24.8 mag) is likely caused by the combined effects of variable mass loss, variation in initial helium abundance (Yini = 0.23 to 0.28), and a small variation in age (6.5-7.5 Gyr) and metallicity ([Fe/H] = −1.5 to −1.3). Spectroscopic follow-up observations of RC stars in Kron 3 are necessary to confirm the cause of the extended RC.

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

FUSEMeasurements of Far‐Ultraviolet Extinction. II. Magellanic Cloud Sight Lines

2005 ◽  
Vol 630 (1) ◽  
pp. 355-367 ◽  
Author(s):  
Stefan I. B. Cartledge ◽  
Geoffrey C. Clayton ◽  
Karl D. Gordon ◽  
Brian L. Rachford ◽  
B. T. Draine ◽  
...  
Keyword(s):  
Magellanic Cloud ◽  
Ultraviolet Extinction ◽  
Far Ultraviolet
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