The stellar population of the Small Magellanic Cloud near NGC 121. I - The mean metallicity, metallicity spread, and radial velocity of SMC halo giants

1986 ◽  
Vol 91 ◽  
pp. 275 ◽  
Author(s):  
N. B. Suntzeff ◽  
E. Friel ◽  
A. Klemola ◽  
R. P. Kraft ◽  
J. A. Graham
Keyword(s):  
Radial Velocity ◽  
Stellar Population ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
The Mean

scholarly journals Wolf-Rayet binaries: old friends and new acquaintances

1999 ◽  
Vol 193 ◽  
pp. 26-37 ◽  
Author(s):  
Virpi S. Niemela ◽  
Roberto Gamen ◽  
Nidia I. Morrell ◽  
Sixto Giménez Benítez
Keyword(s):  
Radial Velocity ◽  
Binary Systems ◽  
Magellanic Cloud ◽  
Elliptic Orbit ◽  
Spectral Lines ◽  
Small Magellanic Cloud ◽  
Orbital Elements ◽  
Spectroscopic Observations ◽  
Short Period ◽  
Old Friends

Observations of WR stars in binary systems are discussed, emphasizing constraints on our knowledge of the binary frequency of WR stars, and of WR stars as a distinctive class of objects. Radial velocity orbits of newly discovered binaries, e.g., WR 29, a short period WN7+OB binary in our Galaxy, and SMC/AB 7, a massive WN+O7 binary in the Small Magellanic Cloud, are presented. New spectroscopic observations of binary systems with previously known orbits are also reported, showing in the case of WR 21 evidence of change of the orbital elements as derived from different spectral lines. An elliptic orbit for CV Ser is also illustrated.

HI in the Small Magellanic Cloud Re-examined

1981 ◽  
Vol 4 (2) ◽  
pp. 189-195 ◽  
Author(s):  
R. X. McGee ◽  
Lynette M. Newton
Keyword(s):  
Radial Velocity ◽  
Neutral Hydrogen ◽  
Total Content ◽  
Hii Regions ◽  
Magellanic Cloud ◽  
Hydrogen Gas ◽  
Radial Velocities ◽  
Line Of Sight ◽  
Small Magellanic Cloud

Our re-examination of the neutral hydrogen gas in the Small Magellan Cloud has led to four important results. Firstly, we find that Hindman’s (1967) total content HI map is a satisfactory representation of the gas in the line of sight. Secondly, we find that the HI gas in the SMC exists in four distinct large masses separated from one another in radial velocity by 20 to 30 km s−1. Thirdly, having made this division of the gas we show that there is good correlation between the radial velocities of HII regions, supergiant stars and HI. Finally, we believe that our observations reveal that the SMC is associated with an extremely large trailing halo of HI gas which forms the major component of the inter-cloud bridge region.

scholarly journals The Relation Between Field Massive Stars and Clusters

2007 ◽  
Vol 3 (S246) ◽  
pp. 65-66
Author(s):  
M. S. Oey ◽  
N. L. King ◽  
J. Wm. Parker ◽  
J. B. Lamb
Keyword(s):  
Small Groups ◽  
Stellar Population ◽  
Massive Stars ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Multiple Origins ◽  
External Galaxies ◽  
Runaway Stars ◽  
Massive Field

AbstractMassive “field” stars are those that appear in apparent isolation, in contrast to those in clusters. Whereas cluster stars are formed together in large aggregates, simultaneously, field stars have multiple origins. Some massive field stars may be the “tip of the iceberg” on small groups of physically associated stars, while others appear to be “runaway” stars that are dynamically ejected from clusters. What is the intrinsic relation between clusters and field stars, and what is the faction of runaway stars? Since massive stars are the most luminous stellar population, their demographics are accessible in the nearest external galaxies. We present our current efforts to understand these issues for the Small Magellanic Cloud.

scholarly journals Age and metallicity of star clusters in the Small Magellanic Cloud from integrated spectroscopy

2009 ◽  
Vol 5 (S262) ◽  
pp. 329-330
Author(s):  
Bruno Dias ◽  
Paula Coelho ◽  
Leandro Kerber ◽  
Beatriz Barbuy ◽  
Thais Idiart
Keyword(s):  
Chemical Evolution ◽  
Stellar Population ◽  
Star Clusters ◽  
Population Models ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
Small Magellanic Cloud ◽  
Full Spectrum ◽  
Young Clusters ◽  
Spectrum Fitting

AbstractAnalysis of integrated spectra of star clusters in the Magellanic Clouds can bring important information for studies on the chemical evolution of the Clouds. The aim of the present work is to derive ages and metallicities from integrated spectra of 15 star clusters in the Small Magellanic Cloud (SMC), some of them not studied so far. Making use of a full spectrum fitting technique, we compared the integrated spectra of the sample clusters to three different sets of single stellar population models available in the literature. We derived ages and metallicities for the sample clusters employing the codes STARLIGHT and ULySS. Out of the 15 clusters in our sample, 9 are old/intermediate age clusters and 6 are young clusters. We point out the results for the newly identified as old/intermediate age clusters HW1, NGC 152, Lindsay 3 and 11. We also confirm old ages for NGC 361, NGC 419 and Kron 3, and the oldest well-known SMC cluster NGC 121.

scholarly journals Observational Aspects of Slow Variables in Globular Clusters

1973 ◽  
Vol 21 ◽  
pp. 131-144
Author(s):  
M. W. Feast
Keyword(s):  
Radial Velocity ◽  
Compact Group ◽  
Globular Cluster ◽  
Globular Clusters ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Mira Variables ◽  
Period Effects ◽  
Slow Variables ◽  
Red Giant

AbstractThere are up to 14 known Mira variables in seven globular clusters, though several have not yet been confirmed as radial velocity members. The periods of only 5 are known, all near 200 days. The clusters seem to form a compact group of relatively metal rich clusters. In 3 or 4 cases spectroscopy shows that the giant branches of these clusters penetrate into the M types. The Mira-containing clusters also contain red variables of shorter period and smaller amplitude which are generally also M type stars. Stars apparently evolve to the red of the giant tip as variables of increasing amplitude and period. Effects of TiO blanketing on the (B — V) colours may be anticipated in these clusters.Besides variables at the red giant tip the metal poor globular cluster ω Cen contains variables with strong TiO bands. Photometry, including recent J, H, K, L photometry by Glass shows that these stars are very cool objects. They indicate an extension of the giant branch considerably cooler than previously considered for metal poor clusters.V1, NGC 121 in the Small Magellanic Cloud has a spectrum indicative of an SRd variable. It is not yet clear whether galactic stars similar to this star exist or not.

scholarly journals The VMC survey – XXIII. Model fitting of light and radial velocity curves of Small Magellanic Cloud classical Cepheids

2016 ◽  
Vol 466 (3) ◽  
pp. 3206-3216 ◽  
Author(s):  
M. Marconi ◽  
R. Molinaro ◽  
V. Ripepi ◽  
M.-R. L. Cioni ◽  
G. Clementini ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Model Fitting ◽  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Classical Cepheids

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 Gaia view of a stellar sub-structure in front of the Small Magellanic Cloud

2020 ◽  
Vol 500 (3) ◽  
pp. 2757-2776
Author(s):  
Abinaya O Omkumar ◽  
Smitha Subramanian ◽  
Florian Niederhofer ◽  
Jonathan Diaz ◽  
Maria-Rosa L Cioni ◽  
...  
Keyword(s):  
Stellar Population ◽  
Tangential Velocity ◽  
Magellanic Cloud ◽  
Stellar Structure ◽  
Main Body ◽  
Small Magellanic Cloud ◽  
North West ◽  
The North ◽  
Spatial Coverage ◽  
Red Clump

ABSTRACT Recent observational studies identified a foreground stellar sub-structure traced by red clump (RC) stars (∼12 kpc in front of the main body) in the eastern regions of the Small Magellanic Cloud (SMC) and suggested that it formed during the formation of the Magellanic Bridge (MB), due to the tidal interaction of the Magellanic Clouds. Previous studies investigated this feature only up to 4${_{.}^{\circ}}$0 from the centre of the SMC due to the limited spatial coverage of the data and hence could not find a physical connection with the MB. To determine the spatial extent and properties of this foreground population, we analysed data from the Gaia Data Release 2 (DR2) of a ∼314 deg2 region centred on the SMC, which cover the entire SMC and a significant portion of the MB. We find that the foreground population is present only between 2${_{.}^{\circ}}$5 to ∼5°–6° from the centre of the SMC in the eastern regions, towards the MB and hence does not fully overlap with the MB in the plane of the sky. The foreground stellar population is found to be kinematically distinct from the stellar population of the main body with ∼35 km s−1 slower tangential velocity and moving to the north-west relative to the main body. Though the observed properties are not fully consistent with the simulations, a comparison indicates that the foreground stellar structure is most likely a tidally stripped counterpart of the gaseous MB and might have formed from the inner disc (dominated by stars) of the SMC. A chemical and 3D kinematic study of the RC stars along with improved simulations, including both tidal and hydro-dynamical effects, are required to understand the offset between the foreground structure and MB.

Sign in / Sign up

Export Citation Format

Share Document