scholarly journals Infrared Emission from Interstellar Dust. III. The Small Magellanic Cloud

2002 ◽  
Vol 576 (2) ◽  
pp. 762-772 ◽  
Author(s):  
Aigen Li ◽  
B. T. Draine
Keyword(s):  
Interstellar Dust ◽  
Infrared Emission ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud

scholarly journals Small Magellanic Cloud–Type Interstellar Dust in the Milky Way

2003 ◽  
Vol 598 (1) ◽  
pp. 369-374 ◽  
Author(s):  
Lynne A. Valencic ◽  
Geoffrey C. Clayton ◽  
Karl D. Gordon ◽  
Tracy L. Smith
Keyword(s):  
Interstellar Dust ◽  
Milky Way ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Cloud Type

scholarly journals TheSpitzerSurvey of the Small Magellanic Cloud: Far‐Infrared Emission and Cold Gas in the Small Magellanic Cloud

2007 ◽  
Vol 658 (2) ◽  
pp. 1027-1046 ◽  
Author(s):  
Adam Leroy ◽  
Alberto Bolatto ◽  
Snezana Stanimirovic ◽  
Norikazu Mizuno ◽  
Frank Israel ◽  
...  
Keyword(s):  
Far Infrared ◽  
Infrared Emission ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Cold Gas

scholarly journals Interstellar Polarization in the Small Magellanic Cloud

1992 ◽  
Vol 150 ◽  
pp. 109-110
Author(s):  
C. Rodrigues ◽  
A.M. Magalhãtes ◽  
G. Coyne ◽  
V. Piirola
Keyword(s):  
Interstellar Dust ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Polarization Data ◽  
Maximum Polarization

Data of our on-going program on the interstellar polarization in the Small Magellanic Cloud (SMC) seem to show a correlation between the UV extinction and the parameters of the Serkowski law which describe the polarization. Fits of popular interstellar dust models to the polarization data are not always satisfactory, being better for stars with small wavelength of maximum polarization, λmax.

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

scholarly journals Infrared extinction in the Small Magellanic Cloud

1984 ◽  
Vol 211 (4) ◽  
pp. 895-900 ◽  
Author(s):  
K. Nandy ◽  
D. H. Morgan ◽  
L. Houziaux
Keyword(s):  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Infrared Extinction

scholarly journals A new study of N66 in the Small Magellanic Cloud

1991 ◽  
Vol 249 (4) ◽  
pp. 722-728 ◽  
Author(s):  
T. Ye ◽  
A. J. Turtle ◽  
R. C. Kennicutt
Keyword(s):  
Magellanic Cloud ◽  
Small Magellanic Cloud
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