A Radial Velocity Survey for Large Magellanic Cloud Microlensed Sources

1999 ◽  
Vol 526 (1) ◽  
pp. 141-146 ◽  
Author(s):  
HongSheng Zhao
Keyword(s):  
Radial Velocity ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

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

scholarly journals The multiple system Sk-67°18 in the LMC

1995 ◽  
Vol 163 ◽  
pp. 251-253 ◽  
Author(s):  
V. S. Niemela ◽  
W. Seggewiss ◽  
A. F. J. Moffat
Keyword(s):  
Binary System ◽  
Radial Velocity ◽  
Spectral Type ◽  
Orbital Period ◽  
Large Magellanic Cloud ◽  
Primary Component ◽  
Magellanic Cloud ◽  
Bright Star ◽  
High Mass ◽  
Eclipsing Binary

The bright star Sk—67°18 (Brey 5) in the Large Magellanic Cloud (LMC) contains an eclipsing binary system. Our radial velocity study reveals that the orbital period is almost exactly two days. The spectra also show that the star's primary component is not of spectral type WN, but that the star is rather an Of+O type binary where the primary is probably of type O3f*. Furthermore, Sk—67°18 appears to be a high-mass multiple system.

scholarly journals THE ECLIPSING BINARY CEPHEID OGLE-LMC-CEP-0227 IN THE LARGE MAGELLANIC CLOUD: PULSATION MODELING OF LIGHT AND RADIAL VELOCITY CURVES

2013 ◽  
Vol 768 (1) ◽  
pp. L6 ◽  
Author(s):  
M. Marconi ◽  
R. Molinaro ◽  
G. Bono ◽  
G. Pietrzyński ◽  
W. Gieren ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Eclipsing Binary

scholarly journals The variable star population of NGC 1866

1991 ◽  
Vol 148 ◽  
pp. 384-385
Author(s):  
Douglas L. Welch ◽  
Patrick Côté ◽  
Mario Mateo ◽  
Barry F. Madore
Keyword(s):  
Radial Velocity ◽  
Variable Star ◽  
Large Magellanic Cloud ◽  
Variable Stars ◽  
Magellanic Cloud

We report the results of an extensive photometric and radial velocity study of the variable stars in the Large Magellanic Cloud (LMC) cluster NGC 1866. We find:

Dwarf galaxies: evidence of differential tidal effects in the Large Magellanic Cloud

2018 ◽  
Vol 14 (S344) ◽  
pp. 114-117
Author(s):  
Andrés E. Piatti ◽  
Dougal Mackey
Keyword(s):  
Gravitational Field ◽  
Radial Velocity ◽  
Globular Clusters ◽  
Surface Brightness ◽  
Dwarf Galaxies ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Tidal Effects ◽  
Radial Profiles ◽  
Stellar Density

AbstractWe built the most extended stellar density and/or surface brightness radial profiles for 13 old Large Magellanic Cloud (LMC) globular clusters (GCs). The studied GCs located farther than ~ 5 kpc from the LMC center would not seem to present any hint of extended stellar structures, while those closer than ~ 5 kpc do show extended structures. Such an excess of stars tightly depends on the position of the GCs, so that the closer the GC to the LMC center, the larger the excess of stars. Furthermore, the GC radii also show a remarkable trend with the position of the GC in the LMC disc. These outcomes can be fully interpreted in the light of the known GC radial velocity disc-like kinematics, from which GCs have been somehow mostly experiencing the influence of the LMC gravitational field at their respective mean distances from the LMC center.

scholarly journals Detached Binaries in the Large Magellanic Cloud

2005 ◽  
Vol 13 ◽  
pp. 462-462
Author(s):  
G. Michalska ◽  
A. Pigulski
Keyword(s):  
Radial Velocity ◽  
Variable Star ◽  
Good Accuracy ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Eclipsing Binaries ◽  
Light Curves ◽  
Distance Determination ◽  
Detached Binaries ◽  
Stellar Masses

Analysis of the radial-velocity and light curves of detached eclipsing binaries allows to derive stellar masses and radii and, in consequence, enables to find their distances. The method has been already applied to several LMC binaries, but in order to have the distance to the LMC determined with good accuracy, the parameters need to be known for a larger number of systems. As a first step we present results of the analysis of the photometry of over eighty detached binaries in the LMC selected from the OGLE-II catalog of 53 000 variable star candidates. If possible, we combine the OGLE-II data with the photometry from other projects (MACHO and EROS). As a result, we present the list of brightest eclipsing binaries in the LMC suitable for distance determination.

scholarly journals A kinematical catalogue of HII regions and superbubbles in the LMC

2012 ◽  
Vol 10 (H16) ◽  
pp. 621-621
Author(s):  
P. Ambrocio-Cruz ◽  
E. Le Coarer ◽  
M. Rosado ◽  
D. Russeil ◽  
P. Amram ◽  
...  
Keyword(s):  
Velocity Field ◽  
Radial Velocity ◽  
Gravitational Potential ◽  
Rotation Curve ◽  
Hii Regions ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

AbstractWe report the results of a kinematic Hα survey of the Large Magellanic Cloud (LMC) in the form of a kinematic and photometric catalogue of 210 HII regions, the radial velocity field of the ionized hydrogen in this galaxy, and the LMC Rotation Curve obtained from the velocity field. These data aim at understanding the LMC HII regions, bubbles and superbubbles in a global (galactic) scale so that we could have a 3D view and separate the rotation due to gravitational potential from other motions such as expansions.

Distance to SN 1987A and the LMC

1999 ◽  
Vol 190 ◽  
pp. 549-554
Author(s):  
Nino Panagia
Keyword(s):  
Angular Size ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Light Curves ◽  
Distance Modulus ◽  
Absolute Size ◽  
Sn 1987A

Using the new reductions of the IUE light curves by Sonneborn et al. (1997) and an extensive set of HST images of SN 1987A we have repeated and improved Panagia et al. (1991) analysis to obtain a better determination of the distance to the supernova. In this way we have derived an absolute size of the ringRabs= (6.23 ± 0.08) x 1017cm and an angular sizeR″ = 808 ± 17 mas, which give a distance to the supernovad(SN1987A) = 51.4 ± 1.2 kpc and a distance modulusm–M(SN1987A) = 18.55 ± 0.05. Allowing for a displacement of SN 1987A position relative to the LMC center, the distance to the barycenter of the Large Magellanic Cloud is also estimated to bed(LMC) = 52.0±1.3 kpc, which corresponds to a distance modulus ofm–M(LMC) = 18.58±0.05.

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