An extremely carbon-poor planetary nebula in the Small Magellanic Cloud

1990 ◽  
Vol 361 ◽  
pp. 101 ◽  
Author(s):  
Stephen J. Meatheringham ◽  
Stephen P. Maran ◽  
Theodore P. Stecher ◽  
Andrew G. Michalitsianos ◽  
Theodore R. Gull ◽  
...  
Keyword(s):  
Planetary Nebula ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud

scholarly journals ISO Observations of the Planetary Nebula Lindsay 305 in the Small Magellanic Cloud

2000 ◽  
Vol 52 (4) ◽  
pp. 619-622 ◽  
Author(s):  
Arūnas Kučinskas ◽  
Vladas Vansevičius ◽  
Marc Sauvage ◽  
Toshihiko Tanabé
Keyword(s):  
Planetary Nebula ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud

scholarly journals XSHOOTER spectroscopy of the enigmatic planetary nebula Lin49 in the Small Magellanic Cloud

2016 ◽  
Vol 462 (1) ◽  
pp. 12-34 ◽  
Author(s):  
Masaaki Otsuka ◽  
F. Kemper ◽  
M. L. Leal-Ferreira ◽  
I. Aleman ◽  
J. Bernard-Salas ◽  
...  
Keyword(s):  
Planetary Nebula ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud

scholarly journals Binary interactions on the RGB: Dusty post-RGB stars

2016 ◽  
Vol 12 (S323) ◽  
pp. 223-226
Author(s):  
Devika Kamath ◽  
Hans Van Winckel ◽  
Peter Wood
Keyword(s):  
Radial Velocity ◽  
Planetary Nebula ◽  
Planetary Nebulae ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
Binary Interaction ◽  
Small Magellanic Cloud ◽  
Preliminary Results ◽  
Low Metallicity ◽  
Binary Evolution

AbstractIt is widely accepted that binary interactions are responsible for the shaping of planetary nebula. However, these binary interactions and evolutionary channels are poorly understood. Our recent study revealed a newly discovered population of low-luminosity, low-metallicity, likely binaries in the Magellanic Clouds: dusty post-RGB stars. They are likely to have evolved off the RGB via binary interaction. In this paper we present preliminary results of the first radial velocity monitoring of the post-RGB stars in the Small Magellanic Cloud (SMC) and the implications on stellar (binary) evolution. We also investigate their link, if any, to the planetary nebulae systems.

scholarly journals Planetary nebulae and Wolf-Rayet stars in the Magellanic Clouds

1964 ◽  
Vol 20 ◽  
pp. 316-321 ◽  
Author(s):  
B. E. Westerlund
Keyword(s):  
Planetary Nebula ◽  
Large Scale ◽  
Planetary Nebulae ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
Small Magellanic Cloud ◽  
Solar Mass ◽  
The Masses

Objects in the Small Magellanic Cloud classified by Lindsay (1961) as planetary nebulae or probable planetary nebulae have been studied in detail on large-scale photographs (Henize and Westerlund 1963). Of Lindsay's 50 objects, 11 are clearly resolved, 2 are probably resolved, 12 show stellar images, 13 are below the limit of the plates, 11 (fairly faint) are outside the photographed regions, and 1 is of uncertain identification. The masses of the resolved nebulae lie between 2 and 33 solar masses. They are therefore classified as small diffuse nebulae; it appears unlikely that the mass of a planetary nebula can exceed a few tenths of a solar mass.

scholarly journals SMC SMP 24: A newly radio-detected planetary nebula in the small Magellanic cloud

2010 ◽  
pp. 63-68 ◽  
Author(s):  
I.S. Bojicic ◽  
M.D. Filipovic ◽  
E.J. Crawford
Keyword(s):  
Planetary Nebula ◽  
Magellanic Cloud ◽  
Radio Continuum ◽  
Small Magellanic Cloud ◽  
Radio Observations ◽  
Radio Data ◽  
Continuum Image ◽  
New Radio ◽  
Multi Wavelength

In this paper we report a new radio-continuum detection of an extragalactic planetary nebula (PN): SMC SMP 24. We show the radio-continuum image of this PN and present the measured radio data. The newly reduced radio observations are consistent with the multi-wavelength data and derived parameters found in the literature. SMC SMP 24 appears to be a young and compact PN, optically thick at frequencies below 2 GHz.

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
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