Studies of the Large Magellanic Cloud. II. The Globular Cluster NGC 1846.

1960 ◽  
Vol 132 ◽  
pp. 341 ◽  
Author(s):  
Paul W. Hodge
Keyword(s):  
Globular Cluster ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

scholarly journals THE EXTENDED MAIN-SEQUENCE TURNOFF CLUSTERS OF THE LARGE MAGELLANIC CLOUD—MISSING LINKS IN GLOBULAR CLUSTER EVOLUTION

2011 ◽  
Vol 731 (1) ◽  
pp. 22 ◽  
Author(s):  
Stefan C. Keller ◽  
A. Dougal Mackey ◽  
Gary S. Da Costa
Keyword(s):  
Globular Cluster ◽  
Main Sequence ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Cluster Evolution

Studies of the Large Magellanic Cloud. III the Globular Cluster NGC 1978.

1960 ◽  
Vol 132 ◽  
pp. 346 ◽  
Author(s):  
Paul W. Hodge
Keyword(s):  
Globular Cluster ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

scholarly journals Spectroscopy of Overluminous Cepheids in the Magellanic Clouds

1984 ◽  
Vol 108 ◽  
pp. 223-224
Author(s):  
Horace A. Smith ◽  
Leo Connolly
Keyword(s):  
Globular Cluster ◽  
Large Magellanic Cloud ◽  
Variable Stars ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
Small Magellanic Cloud ◽  
Single Star ◽  
Rr Lyrae ◽  
Short Period ◽  
The Galaxy

The Small Magellanic Cloud is known to contain types of short period Cepheid variable stars not yet discovered in either the Large Magellanic Cloud or, with the exception of a single star, in the Galaxy. These variables can be divided into two categories: anomalous Cepheids and Wesselink-Shuttleworth (WS) stars. The former, which have also been found in dwarf spheroidal systems and in the globular cluster NGC 5466, have periods of 0.4–3 days, but average 0.7–1.0 mag. brighter than RR Lyrae and BL Her stars of equal period. The stars we call WS stars have periods less than about 1.1 day and, at MV = −1 to −2, are brighter than anomalous Cepheids of equal period.

scholarly journals Kinematics of the LMC CH-stars

1991 ◽  
Vol 148 ◽  
pp. 77-80 ◽  
Author(s):  
F.D.A. Hartwick ◽  
A. P. Cowley
Keyword(s):  
Globular Cluster ◽  
Stellar Population ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

Velocities have been measured for 74 CH stars in the direction of the Large Magellanic Cloud (LMC). These have been used to study the kinematics of the oldest stellar population. Velocities of these objects appear to reflect two distinct subgroups - one associated with the old globular cluster population and a second with the LMC disk.

The Large Magellanic Cloud Globular Cluster NGC 1866: New Data, New Models, New Analysis

1999 ◽  
Vol 118 (6) ◽  
pp. 2839-2864 ◽  
Author(s):  
Vincenzo Testa ◽  
Francesco R. Ferraro ◽  
Alessandro Chieffi ◽  
Oscar Straniero ◽  
Marco Limongi ◽  
...  
Keyword(s):  
Globular Cluster ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
New Models

The age of the Large Magellanic Cloud globular cluster NGC 1651

1986 ◽  
Vol 304 ◽  
pp. 265 ◽  
Author(s):  
J. R. Mould ◽  
G. S. Da Costa ◽  
M. D. Crawford
Keyword(s):  
Globular Cluster ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

scholarly journals BLUE STRAGGLER EVOLUTION CAUGHT IN THE ACT IN THE LARGE MAGELLANIC CLOUD GLOBULAR CLUSTER HODGE 11

2013 ◽  
Vol 770 (1) ◽  
pp. L7 ◽  
Author(s):  
Chengyuan Li ◽  
Richard de Grijs ◽  
Licai Deng ◽  
Xiangkun Liu
Keyword(s):  
Globular Cluster ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Blue Straggler

Two kinematically different Large Magellanic Cloud old globular cluster populations unveiled from Gaia DR2 data sets

2019 ◽  
Vol 14 (S351) ◽  
pp. 139-142
Author(s):  
Andrés E. Piatti ◽  
Emilio J. Alfaro ◽  
Tristan Cantat-Gaudin
Keyword(s):  
Globular Cluster ◽  
Globular Clusters ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Data Sets ◽  
Spatial Distributions ◽  
Proper Motions ◽  
Structural Components ◽  
Absolute Value ◽  
Gaia Dr2

AbstractWe derive mean proper motions of 15 known Large Magellanic Cloud (LMC) old globular clusters (GCs) from the Gaia DR2 data sets. When these mean proper motions are gathered with existent radial velocities to compose the GCs’ velocity vectors, we found that the projection of the velocity vectors onto the LMC plane and those perpendicular to it tell us about two distinct kinematical GC populations. Such a distinction becomes clear if the GCs are split at a perpendicular velocity of 10 km/s (absolute value). The two different kinematics groups also exhibit different spatial distributions. Those with smaller vertical velocities are part of the LMC disk, while those with larger values are closely distributed like a spheroidal component. Since GCs in both kinematic-structural components share similar ages and metallicities, we speculate with the possibility that their origins could have occurred through a fast collapse that formed halo and disk concurrently.

On the structure of the ?red? globular cluster NGC 1806 in the large magellanic cloud

1982 ◽  
Vol 84 (1) ◽  
pp. 133-141 ◽  
Author(s):  
Edward H. Geyer ◽  
Ulrich Hopp
Keyword(s):  
Globular Cluster ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud
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