Long-period variables in the Large Magellanic Cloud. III - Evidence of a kinematic spheroidal population

1991 ◽  
Vol 101 ◽  
pp. 1304 ◽  
Author(s):  
Shaun M. G. Hughes ◽  
Peter R. Wood ◽  
Neill Reid
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Long Period ◽  
Long Period Variables

scholarly journals THE PROPERTIES OF LONG-PERIOD VARIABLES IN THE LARGE MAGELLANIC CLOUD FROM MACHO

2008 ◽  
Vol 136 (3) ◽  
pp. 1242-1258 ◽  
Author(s):  
Oliver J. Fraser ◽  
Suzanne L. Hawley ◽  
Kem H. Cook
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Long Period ◽  
Long Period Variables

scholarly journals Long-Period Variables in the Large Magellanic Cloud: Results from MACHO and 2MASS

2005 ◽  
Vol 129 (2) ◽  
pp. 768-775 ◽  
Author(s):  
Oliver J. Fraser ◽  
Suzanne L. Hawley ◽  
Kem H. Cook ◽  
Stefan C. Keller
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Long Period ◽  
Long Period Variables

scholarly journals Long period variables in the Large Magellanic Cloud from the EROS-2 survey

2011 ◽  
Vol 536 ◽  
pp. A60 ◽  
Author(s):  
M. Spano ◽  
N. Mowlavi ◽  
L. Eyer ◽  
G. Burki ◽  
J.-B. Marquette ◽  
...  
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Long Period ◽  
Long Period Variables

Investigating the Halo of the LMC

1990 ◽  
Vol 8 (04) ◽  
pp. 343-347 ◽  
Author(s):  
Shaun M. G. Hughes ◽  
Peter R. Wood ◽  
Neill Reid
Keyword(s):  
Molecular Clouds ◽  
Velocity Dispersion ◽  
Planetary Nebulae ◽  
Rotating Disk ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Long Period ◽  
Long Period Variables

Abstract Recent results have shown that Long-Period Variables (LPVs) with periods in the range 100 to 250 days have ages ~ 10 Gyr. We have studied the kinematics of a sample of such variables in the Large Magellanic Cloud (LMC). A comparison with the kinematics of other populations (H I gas, CO molecular clouds, planetary nebulae, CH stars and old clusters) indicates that all populations younger than the old LPVs are dominated by a single common rotating disk, with the kinematics of the old LPVs being the first to indicate the presence in the LMC of a spheroidal population, with little or no rotation and a velocity dispersion ~ 6 times larger than that of the H I gas.

scholarly journals Star Formation History of the Large Magellanic Cloud and Asymptotic Giant Branch Evolution Obtained from A Study of Long-Period Variables.

1989 ◽  
Vol 111 ◽  
pp. 269-269
Author(s):  
Shaun M.G. Hughes ◽  
P.R. Wood
Keyword(s):  
Star Formation ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Asymptotic Giant Branch ◽  
Star Formation History ◽  
Global Survey ◽  
Long Period ◽  
Formation History ◽  
Long Period Variables ◽  
History Of

AbstractA survey for Long-Period Variables has been made of the Bar and southern regions of the Large Magellanic Cloud. This has been combined with the results of Reid, Glass and Catchpole (1988) to present a global survey of the LMC. Periods are used as age indicators, giving the star formation history of the LMC from 1 to 10 Gyr, which indicates a major burst of star formation occurred approximately 4 Gyr ago.

scholarly journals Leavitt Variables: The Brightest Cepheids Variables and their Implications for the Distance Scale

1985 ◽  
Vol 82 ◽  
pp. 215-218
Author(s):  
Gerald R. Grieve ◽  
Barry F. Madore ◽  
Douglas L. Welch
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Log P ◽  
Linear Extrapolation ◽  
High Luminosity ◽  
Long Period ◽  
Long Period Variables ◽  
Cepheid Variables ◽  
External Galaxies ◽  
Low Amplitude

AbstractTwo low-amplitude variable supergiants in the Large Magellanic Cloud, S65-08 and S65-48 are each found to have periods of approximately 250 days. The cfptical data suggest that these stars are high-luminosity cepheid variables falling more than one magnitude brighter than any other known Cepheids in the LMC. Confirmation of the cepheid nature of these stars comes from their H-band magnitudes which place them accurately on a simple linear extrapolation of the narrower infrared Period-Luminosity relation. So it appears that the cepheid Period-Luminosity relation extends up to Mv ~ -8.5. To honour the astronomer who discovered the first of these highest-liminosity Cepheids, we have sub-classified the variables with log P > 1.8 as being “Leavitt variables”. As soon as these long-period variables are discovered in other external galaxies, reliable distances should be possible out to (m-M) ~30.

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