The Ultraviolet and Optical Spectra of Luminous B‐Type Stars in the Small Magellanic Cloud

2004 ◽  
Vol 116 (824) ◽  
pp. 909-919 ◽  
Author(s):  
C. J. Evans ◽  
D. J. Lennon ◽  
N. R. Walborn ◽  
C. Trundle ◽  
S. A. Rix
Keyword(s):  
Optical Spectra ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud

scholarly journals The Mass Loss Rate of SK 80 (07Iaf) in the Small Magellanic Cloud

1986 ◽  
Vol 116 ◽  
pp. 269-270
Author(s):  
A J Willis ◽  
I D Howarth ◽  
K Nandy ◽  
D H Morgan
Keyword(s):  
Mass Loss ◽  
Loss Rate ◽  
Mass Loss Rate ◽  
Optical Spectra ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
Small Magellanic Cloud ◽  
Ob Stars

The star SK 80 in the SMC is classified as 07Iaf by Walborn (1976) who notes that it is the only confirmed Of star in that Galaxy known to date. A knowledge of the mass loss properties of OB stars in the Magellanic Clouds is of interest because of the recent evidence that such stars show reduced mass loss properties than their galactic counterparts (Hutchings 1980) and for Of stars because of the possible link between such stars and Pop I transition WNL stars (Conti 1976).We have secured HIRES IUE and optical spectra of SK 80 and have attempted to derive the mass loss rate from these data.

scholarly journals Optical spectra of radio planetary nebulae in the small Magellanic cloud

2008 ◽  
pp. 65-70 ◽  
Author(s):  
J.L. Payne ◽  
M.D. Filipovic ◽  
E.J. Crawford ◽  
Horta de ◽  
G.L. White ◽  
...  
Keyword(s):  
South Africa ◽  
High Resolution ◽  
Planetary Nebulae ◽  
Optical Spectra ◽  
Magellanic Cloud ◽  
Radio Sources ◽  
Small Magellanic Cloud ◽  
Preliminary Results ◽  
Central Stars ◽  
Compact Array

We present preliminary results from spectral observations of four (4) candidate radio sources co-identified with known planetary nebulae (PNe) in the Small Magellanic Cloud (SMC). These were made using the Radcliffe 1.9-meter telescope in Sutherland, South Africa. These radio PNe were originally found in Australia Telescope Compact Array (ATCA) surveys of the SMC at 1.42 and 2.37 GHz, and were further confirmed by new high resolution ATCA images at 6 and 3 cm (400 /200 ). Optical PNe and radio candidates are within 200 and may represent a sub- population of selected radio bright objects. Nebular ionized masses of these objects may be 2.6 Mo or greater, supporting the existence of PNe progenitor central stars with masses up to 8 Mo.

scholarly journals The Oxygen-Rich Supernova Remnant in the Small Magellanic Cloud

1988 ◽  
Vol 101 ◽  
pp. 187-190
Author(s):  
William P. Blair ◽  
John C. Raymond ◽  
John Danziger ◽  
Francesca Matteucci
Keyword(s):  
Supernova Remnant ◽  
Optical Spectra ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Shock Excitation ◽  
X Ray ◽  
Line Intensities ◽  
Relative Line

AbstractWe report ultraviolet and optical spectra of IE 0102-7219, the oxygen-rich supernova remnant in the Small Magellanic Cloud. The UV data contain strong lines of oxygen, carbon, neon, and magnesium. OI recombination lines in the optical and UV permit the relative line intensities to be determined from 1200Å to 1 micron. Models assuming shock excitation and X-ray photoionization have been calculated and compared with the observations.

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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