scholarly journals Four new planetary nebulae towards the Small Magellanic Cloud

2015 ◽  
Vol 452 (2) ◽  
pp. 1402-1411 ◽  
Author(s):  
Danica Drašković ◽  
Quentin A. Parker ◽  
Warren A. Reid ◽  
Milorad Stupar
Keyword(s):  
Planetary Nebulae ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud

scholarly journals Radio planetary nebulae in the Small Magellanic Cloud

2016 ◽  
Vol 361 (3) ◽  
Author(s):  
Howard Leverenz ◽  
Miroslav D. Filipović ◽  
I. S. Bojičić ◽  
E. J. Crawford ◽  
J. D. Collier ◽  
...  
Keyword(s):  
Planetary Nebulae ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud

scholarly journals Discovery of new planetary nebulae in the Small Magellanic Cloud

2016 ◽  
Vol 728 ◽  
pp. 072008
Author(s):  
D. Drašković ◽  
Q. A. Parker ◽  
W. A. Reid ◽  
M. Stupar
Keyword(s):  
Planetary Nebulae ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud

Coravel Radial Velocities of Supergiants in the Small Magellanic Cloud

1984 ◽  
Vol 88 ◽  
pp. 265-268
Author(s):  
E. Maurice ◽  
N. Martin ◽  
L. Prévot ◽  
E. Rebeirot
Keyword(s):  
South Africa ◽  
Velocity Field ◽  
Planetary Nebulae ◽  
Hii Regions ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
Radial Velocities ◽  
Small Magellanic Cloud ◽  
Objective Prism

Kinematical studies of the Magellanic Clouds began more than half a century ago, when Wilson, in 1918, first interpreted the gradient of the 17 radial velocities of gazeous nebulae in the Large Cloud in terms of rotation. In the case of the Small Magellanic Cloud, the first real attempt to understand the velocity field of this galaxy was performed by the Radcliffe astronomers (Feast et al., 1960, 1961). Their study was based on radial velocities of 40 stars and 13 HII regions.With the installation by ESO of an objective-prisme astrograph in South Africa, in 1961, and then of several larger telescopes in Chile in 1968, the number of measurements significantly increased for Magellanic objects, in particular in the SMC. In this galaxy, the objective-prism observations resulted in about 100 stellar radial velocities (Florsch, 1972a) of probable members. A compilation by Maurice (1979) of all then known slit-spectrograph radial velocities gave velocities for 80 supergiants, 35 HII regions and 12 planetary nebulae.

The UKST Survey of Planetary Nebulae in the Small Magellanic Cloud

1995 ◽  
Vol 148 ◽  
pp. 415-418
Author(s):  
D. H. Morgan
Keyword(s):  
Spatial Distribution ◽  
Planetary Nebulae ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Schmidt Telescope ◽  
Objective Prism ◽  
The Uk

AbstractThis paper describes the results of searches for planetary nebulae on seven objective prism plates which were taken with the UK 1.2m Schmidt Telescope and cover the entire Small Magellanic Cloud. A total of 62 objects were detected; their spatial distribution is discussed.

scholarly journals Chemical evolution of the Small Magellanic Cloud based on planetary nebulae

2007 ◽  
Vol 472 (1) ◽  
pp. 101-110 ◽  
Author(s):  
T. P. Idiart ◽  
W. J. Maciel ◽  
R. D. D. Costa
Keyword(s):  
Chemical Evolution ◽  
Planetary Nebulae ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud

The kinematics and internal dynamics of planetary nebulae in the small Magellanic Cloud

1985 ◽  
Vol 296 ◽  
pp. 390 ◽  
Author(s):  
M. A. Dopita ◽  
C. J. Lawrence ◽  
H. C. Ford ◽  
B. L. Webster
Keyword(s):  
Planetary Nebulae ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Internal Dynamics

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.

Sign in / Sign up

Export Citation Format

Share Document