scholarly journals Surface Brightness and Stellar Populations at the Outer Edge of the Large Magellanic Cloud: No Stellar Halo Yet

2004 ◽  
Vol 614 (2) ◽  
pp. L109-L112 ◽  
Author(s):  
Carme Gallart ◽  
Peter B. Stetson ◽  
Eduardo Hardy ◽  
Frederic Pont ◽  
Robert Zinn
Keyword(s):  
Surface Brightness ◽  
Stellar Populations ◽  
Large Magellanic Cloud ◽  
Outer Edge ◽  
Magellanic Cloud ◽  
Stellar Halo

scholarly journals Exploring the Very Extended Low-surface-brightness Stellar Populations of the Large Magellanic Cloud with SMASH

2019 ◽  
Vol 874 (2) ◽  
pp. 118 ◽  
Author(s):  
David L. Nidever ◽  
Knut Olsen ◽  
Yumi Choi ◽  
Thomas J. L. de Boer ◽  
Robert D. Blum ◽  
...  
Keyword(s):  
Surface Brightness ◽  
Stellar Populations ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Low Surface Brightness

scholarly journals The VISCACHA survey – II. Structure of star clusters in the Magellanic Clouds periphery

2020 ◽  
Vol 498 (1) ◽  
pp. 205-222
Author(s):  
João F C Santos ◽  
Francisco F S Maia ◽  
Bruno Dias ◽  
Leandro de O Kerber ◽  
Andrés E Piatti ◽  
...  
Keyword(s):  
Surface Brightness ◽  
Structural Parameters ◽  
Star Clusters ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
The Core ◽  
Optical Images ◽  
Low Surface Brightness ◽  
Homogeneous Set ◽  
Stellar Density

ABSTRACT We provide a homogeneous set of structural parameters of 83 star clusters located at the periphery of the Small Magellanic Cloud (SMC) and the Large Magellanic Cloud (LMC). The clusters’ stellar density and surface brightness profiles were built from deep, AO assisted optical images, and uniform analysis techniques. The structural parameters were obtained from King and Elson et al. model fittings. Integrated magnitudes and masses (for a subsample) are also provided. The sample contains mostly low surface brightness clusters with distances between 4.5 and 6.5 kpc and between 1 and 6.5 kpc from the LMC and SMC centres, respectively. We analysed their spatial distribution and structural properties, comparing them with those of inner clusters. Half-light and Jacobi radii were estimated, allowing an evaluation of the Roche volume tidal filling. We found that: (i) for our sample of LMC clusters, the tidal radii are, on average, larger than those of inner clusters from previous studies; (ii) the core radii dispersion tends to be greater for LMC clusters located towards the southwest, with position angles of ∼200° and about ∼5° from the LMC centre, i.e. those LMC clusters nearer to the SMC; (iii) the core radius evolution for clusters with known age is similar to that of inner clusters; (iv) SMC clusters with galactocentric distances closer than 4 kpc are overfilling; (v) the recent Clouds collision did not leave marks on the LMC clusters’ structure that our analysis could reveal.

scholarly journals Equilibrium models of the Milky Way mass are biased high by the LMC

2020 ◽  
Vol 498 (4) ◽  
pp. 5574-5580 ◽  
Author(s):  
Denis Erkal ◽  
Vasily A Belokurov ◽  
Daniel L Parkin
Keyword(s):  
Milky Way ◽  
Large Magellanic Cloud ◽  
Substantial Effect ◽  
Magellanic Cloud ◽  
Equilibrium Models ◽  
Simple Modification ◽  
Bulk Motion ◽  
Stellar Halo ◽  
Large Satellite

ABSTRACT Recent measurements suggest that the Large Magellanic Cloud (LMC) may weigh as much as 25 per cent of the Milky Way (MW). In this work, we explore how such a large satellite affects mass estimates of the MW based on equilibrium modelling of the stellar halo or other tracers. In particular, we show that if the LMC is ignored, the MW mass within 200 kpc is overestimated by as much as 50 per cent. This bias is due to the bulk motion in the outskirts of the Galaxy’s halo and can be, at least in part, accounted for with a simple modification to the equilibrium modelling. Finally, we show that the LMC has a substantial effect on the orbit Leo I which acts to increase its present-day speed relative to the MW. We estimate that accounting for a $1.5\times 10^{11} \, \mathrm{M}_\odot$ LMC would lower the inferred MW mass to $\sim 10^{12} \, \mathrm{M}_\odot$.

Large Magellanic Cloud Planetary Nebula Morphology: Probing Stellar Populations and Evolution

2000 ◽  
Vol 534 (2) ◽  
pp. L167-L171 ◽  
Author(s):  
Letizia Stanghellini ◽  
Richard A. Shaw ◽  
Bruce Balick ◽  
J. Chris Blades
Keyword(s):  
Planetary Nebula ◽  
Stellar Populations ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

scholarly journals Exploring the nature and synchronicity of early cluster formation in the Large Magellanic Cloud – IV. Evidence for multiple populations in Hodge 11 and NGC 2210

2019 ◽  
Vol 486 (4) ◽  
pp. 5581-5599 ◽  
Author(s):  
Christina K Gilligan ◽  
Brian Chaboyer ◽  
Jeffrey D Cummings ◽  
Dougal Mackey ◽  
Roger E Cohen ◽  
...  
Keyword(s):  
Globular Clusters ◽  
Main Sequence ◽  
Hubble Space Telescope ◽  
Cluster Formation ◽  
Stellar Populations ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Wide Field ◽  
Horizontal Branch ◽  
Advanced Camera For Surveys

Abstract We present a multiple population search in two old Large Magellanic Cloud (LMC) Globular clusters, Hodge 11 and NGC 2210. This work uses data from the Advanced Camera for Surveys and Wide Field Camera 3 on the Hubble Space Telescope from programme GO-14164 in Cycle 23. Both of these clusters exhibit a broadened main sequence with the second population representing (20 ± ∼5) per cent for NGC 2210 and (30 ± ∼5) per cent for Hodge 11. In both clusters, the smaller population is redder than the primary population, suggesting CNO variations. Hodge 11 also displays a bluer second population in the horizontal branch, which is evidence for helium enhancement. However, even though NGC 2210 shows similarities to Hodge 11 in the main sequence, there does not appear to be a second population on NGC 2210’s horizontal branch. This is the first photometric evidence that ancient LMC Globular clusters exhibit multiple stellar populations.

scholarly journals Two Different Stellar Populations in the Large Magellanic Cloud?

1995 ◽  
Vol 164 ◽  
pp. 415-415
Author(s):  
JU. Frantsman ◽  
I. Shmeld
Keyword(s):  
Neutron Capture ◽  
Stellar Populations ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Agb Stars ◽  
Helium Burning ◽  
Stellar Interior ◽  
Processed Material ◽  
Evolutionary Scheme ◽  
Simple Picture

The evolution of stars on the AGB has been explained as episodic helium burning and neutron capture nucleosynthesis in the stellar interior, followed by the mixing of a portion of the processed material into the envelope of a star. The simple stellar evolutionary scheme M–MS–S–SC–N had been accepted. However in recent years extensive observations of AGB stars have shown that evolution of the AGB is more complicated than painted in such a simple picture.

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