The Kinematics and Age of the Planetary Nebulae in the Large Magellanic Cloud

1986 ◽  
Vol 6 (4) ◽  
pp. 464-467 ◽  
Author(s):  
Stephen J. Meatheringham ◽  
Michael A. Dopita
Keyword(s):  
Rotation Curve ◽  
Velocity Dispersion ◽  
Transverse Velocity ◽  
Planetary Nebulae ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Upper Limit ◽  
Mass Estimate ◽  
Remnant Mass

AbstractAn HI survey of the Large Magellanic Cloud (LMC) has been reanalyzed to find the transverse velocity of the LMC, and derive an upper limit of 4.5 × 1011M⊙for the mass of our Galaxy out to 50 kpc. A rotation curve is derived for the LMC from the HI data giving a best mass estimate of (4.0±0.4)×109M⊙. Velocity observations of 97 planetary nebulae (PN) in the Large Cloud are used to compare the old and young components. Our results are found to be at odds with an earlier sample of 9 old clusters, which is interpreted as being due to the low number of objects in that sample. The w-component of velocity dispersion of the PN population is 35 km s-1and that of the HI 10 km s-1. If this difference is a result of stellar diffusion then the average age of the PN population is 1.3 × 109yr, implying a precursor mass of 1.8 M⊙and a remnant mass of 0.63 M⊙.

scholarly journals The Kinematics of the Planetary Nebulae in the Large Magellanic Cloud

1989 ◽  
Vol 131 ◽  
pp. 352-352
Author(s):  
Stephen J. Meatheringham ◽  
Michael A. Dopita ◽  
Holland. C. Ford ◽  
B. Louise Webster
Keyword(s):  
Vertical Velocity ◽  
Rotation Curve ◽  
Velocity Dispersion ◽  
Transverse Velocity ◽  
Planetary Nebulae ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Radial Velocities ◽  
Solar Neighbourhood ◽  
And Diffusion

The radial velocities of a total of 94 Planetary Nebulae (PN) in the Large Magellanic Cloud (LMC) have been determined. The kinematics of the population of planetary nebulae is compared with the H I data in the context of a re-analysis of the survey by Rohlfs et al. (1984), taking into account the transverse velocity of the LMC. We find that the best solution for this transverse velocity is 275±65 km s−1, and that the LMC is near perigalacticon. This is consistent with a maximum Galactic mass of order 4.5 × 1011M⊙ out to 51 kpc the rotation curve obtained after correction for this velocity implies a mass of (4.6 × 0.3) × 109 M⊙ within a radius of 3 degrees, or about 6 × 109 M⊙, total. The rotation solution for the PN population is essentially identical with that of the H I, but the vertical velocity dispersion of 19.1 km s−1 is much greater than the value of 5.4 km s−1 found for the H I. This increase in velocity dispersion is consistent with it being the result of orbital heating and diffusion operating in the LMC in a manner essentially identical with that found for the solar neighbourhood.

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 An Upper Limit on the Mass of a Central Black Hole in the Large Magellanic Cloud from the Stellar Rotation Field

2017 ◽  
Vol 846 (1) ◽  
pp. 14 ◽  
Author(s):  
H. Boyce ◽  
N. Lützgendorf ◽  
R. P. van der Marel ◽  
H. Baumgardt ◽  
M. Kissler-Patig ◽  
...  
Keyword(s):  
Black Hole ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Stellar Rotation ◽  
Central Black Hole ◽  
Upper Limit ◽  
Rotation Field

The Kinematics of the Planetary Nebulae in the Large Magellanic Cloud

1989 ◽  
pp. 352-352
Author(s):  
Stephen J. Meatheringham ◽  
Michael A. Dopita ◽  
Holland. C. Ford ◽  
B. Louise Webster
Keyword(s):  
Planetary Nebulae ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

scholarly journals Physical parameters and chemical abundances of Planetary Nebulae in the large Magellanic Cloud

1997 ◽  
Vol 180 ◽  
pp. 471-471 ◽  
Author(s):  
R. E. Carlos Reyes ◽  
J. E. Steiner ◽  
F. Elizalde
Keyword(s):  
Planetary Nebulae ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Physical Parameters ◽  
Chemical Abundances ◽  
The Difference

In the present work we have computed the physical parameters and chemical abundances for 45 planetary nebulae (PN) in the Large Magellanic Cloud (LMC) using the photoionization code CLOUDY, developed by Ferland (1993). CLOUDY is used as a subroutine in the code DIANA, developed by Elizalde & Steiner (1996), which minimises indices that measures the difference between the calculated and real nebula.

scholarly journals The 100 strongest radio point sources in the field of the Large Magellanic Cloud at 1.4 GHz

2009 ◽  
pp. 65-70 ◽  
Author(s):  
J.L. Payne ◽  
L.A. Tauber ◽  
M.D. Filipovic ◽  
E.J. Crawford ◽  
Horta de
Keyword(s):  
Spectral Index ◽  
Planetary Nebulae ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Point Sources ◽  
H Ii Regions ◽  
Short Spacing ◽  
Mosaic Image ◽  
Initial List ◽  
Compact Array

We present the 100 strongest 1.4 GHz point sources from a new mosaic image in the direction of the Large Magellanic Cloud (LMC). The observations making up the mosaic were made using Australia Telescope Compact Array (ATCA) over a ten year period and were combined with Parkes single dish data at 1.4 GHz to complete the image for short spacing. An initial list of co-identifications within 1000 at 0.843, 4.8 and 8.6 GHz consisted of 2682 sources. Elimination of extended objects and artifact noise allowed the creation of a refined list containing 1988 point sources. Most of these are presumed to be background objects seen through the LMC; a small portion may represent compact H ii regions, young SNRs and radio planetary nebulae. For the 1988 point sources we find a preliminary average spectral index (?) of -0.53 and present a 1.4 GHz image showing source location in the direction of the LMC.

The internal dynamics of the planetary nebulae in the Large Magellanic Cloud

1988 ◽  
Vol 327 ◽  
pp. 639 ◽  
Author(s):  
Michael A. Dopita ◽  
Stephen J. Meatheringham ◽  
B. Louise Webster ◽  
Holland C. Ford
Keyword(s):  
Planetary Nebulae ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Internal Dynamics

The kinematics of planetary nebulae in the outer fields of the Large Magellanic Cloud

1992 ◽  
Vol 394 ◽  
pp. 489 ◽  
Author(s):  
E. Vassiliadis ◽  
Stephen J. Meatheringham ◽  
Michael A. Dopita
Keyword(s):  
Planetary Nebulae ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud
Sign in / Sign up

Export Citation Format

Share Document