CCD photometry of the Large Magellanic Cloud cluster NGC 1866 - Observational results

1989 ◽  
Vol 71 ◽  
pp. 25 ◽  
Author(s):  
E. Brocato ◽  
R. Buonanno ◽  
V. Castellani ◽  
A. R. Walker
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Ccd Photometry ◽  
Cloud Cluster

Cepheid Variables in the Large Magellanic Cloud Cluster NGC 1866. I. New BVRI CCD Photometry

2000 ◽  
Vol 129 (1) ◽  
pp. 111-121 ◽  
Author(s):  
Wolfgang P. Gieren ◽  
Matias Gomez ◽  
Jesper Storm ◽  
Thomas J. Moffett ◽  
L. Infante ◽  
...  
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Ccd Photometry ◽  
Cloud Cluster ◽  
Cepheid Variables

The Age of the Large Magellanic Cloud Cluster NGC 1651

1997 ◽  
Vol 483 (1) ◽  
pp. L41-L44 ◽  
Author(s):  
Jeremy R. Mould ◽  
Mingsheng Han ◽  
Peter B. Stetson ◽  
Brad Gibson ◽  
John A. Graham ◽  
...  
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Cloud Cluster

scholarly journals Theoretical fit of Cepheid light and radial velocity curves in the Large Magellanic Cloud cluster NGC 1866

2012 ◽  
Vol 428 (3) ◽  
pp. 2185-2197 ◽  
Author(s):  
M. Marconi ◽  
R. Molinaro ◽  
V. Ripepi ◽  
I. Musella ◽  
E. Brocato
Keyword(s):  
Radial Velocity ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Cloud Cluster

The distance to the Large Magellanic Cloud cluster NGC 1866 from its Cepheid members

1994 ◽  
Vol 433 ◽  
pp. L73 ◽  
Author(s):  
Wolfgang P. Gieren ◽  
Tom Richtler ◽  
Michael Hilker
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Cloud Cluster

scholarly journals Observational hints of a real age spread in the young LMC star cluster NGC 1971

2017 ◽  
Vol 470 (1) ◽  
pp. L77-L81 ◽  
Author(s):  
Andrés E. Piatti ◽  
Andrew Cole
Keyword(s):  
Main Sequence ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Star Cluster ◽  
Stellar Rotation ◽  
Cloud Cluster ◽  
Magnitude Diagram ◽  
Observational Errors ◽  
Age Range

Abstract We report that the serendipitous young Large Magellanic Cloud cluster NGC 1971 exhibits an extended main-sequence turn-off (eMSTO) possibly originated mostly by a real age spread. We used CT1 Washington photometry to produce a colour–magnitude diagram (CMD) with the fiducial cluster features. From its eMSTO, we estimated an age spread of ∼170 Myr (observed age range 100–280 Myr), once observational errors, stellar binarity, overall metallicity variations and stellar rotation effects were subtracted in quadrature from the observed age width.

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