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

Spitzer Infrared Spectrograph (IRS) Observations of Large Magellanic Cloud Planetary Nebula SMP 83

2004 ◽  
Vol 154 (1) ◽  
pp. 271-274 ◽  
Author(s):  
J. Bernard‐Salas ◽  
J. R. Houck ◽  
P. W. Morris ◽  
G. C. Sloan ◽  
S. R. Pottasch ◽  
...  
Keyword(s):  
Planetary Nebula ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

scholarly journals A More Complete Listing of LMC Planetary Nebulae

1984 ◽  
Vol 108 ◽  
pp. 231-232
Author(s):  
N. Sanduleak
Keyword(s):  
Planetary Nebula ◽  
Planetary Nebulae ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Plate Material ◽  
Schmidt Telescope ◽  
Complete Listing ◽  
Objective Prism

In an earlier paper by Sanduleak et al. (1978) a listing was given of 102 confirmed and probable planetary nebulae in the Large Magellanic Cloud detected on objective-prism plates taken with the Curtis Schmidt telescope at Cerro Tololo. Subsequently, deeper coverage was obtained on nitrogen-baked Kodak IIIa-J plates plus GG 455 filter exposed for 90 minutes. The thin prism was again used to provide a dispersion of about 1500 Å mm−1 at Hβ and the spectra were unwidened. An additional 25 planetary nebula candidates were found on this new plate material to show the requisite characteristics, i.e. they display (a) a stellar appearance, (b) [OIII] λλ5007, 4959 strongly in emission, and (c) no evidence of a continuum.

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.

scholarly journals SMC 1 or What's in a Name?

1999 ◽  
Vol 190 ◽  
pp. 17-18
Author(s):  
Hélène R. Dickel
Keyword(s):  
Planetary Nebula ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Web Documents

What's in a name? Everything! SMC 1 is a planetary nebula in the Large Magellanic Cloud! URLs of Web documents are given to aid astronomers in designating their astronomical sources so as to avoid confusion in the literature.

scholarly journals Constraining the thermally pulsing asymptotic giant branch phase with resolved stellar populations in the Large Magellanic Cloud

2020 ◽  
Vol 498 (3) ◽  
pp. 3283-3301 ◽  
Author(s):  
Giada Pastorelli ◽  
Paola Marigo ◽  
Léo Girardi ◽  
Bernhard Aringer ◽  
Yang Chen ◽  
...  
Keyword(s):  
Mass Loss Rate ◽  
Spectral Energy Distribution ◽  
Stellar Populations ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Asymptotic Giant Branch ◽  
Star Formation History ◽  
Spectral Energy ◽  
Agb Stars ◽  
The Third

ABSTRACT Reliable models of the thermally pulsing asymptotic giant branch (TP-AGB) phase are of critical importance across astrophysics, including our interpretation of the spectral energy distribution of galaxies, cosmic dust production, and enrichment of the interstellar medium. With the aim of improving sets of stellar isochrones that include a detailed description of the TP-AGB phase, we extend our recent calibration of the AGB population in the Small Magellanic Cloud (SMC) to the more metal-rich Large Magellanic Cloud (LMC). We model the LMC stellar populations with the trilegal code, using the spatially resolved star formation history derived from the VISTA survey. We characterize the efficiency of the third dredge-up by matching the star counts and the Ks-band luminosity functions of the AGB stars identified in the LMC. In line with previous findings, we confirm that, compared to the SMC, the third dredge-up in AGB stars of the LMC is somewhat less efficient, as a consequence of the higher metallicity. The predicted range of initial mass of C-rich stars is between Mi ≈ 1.7 and 3 M⊙ at Zi = 0.008. We show how the inclusion of new opacity data in the carbon star spectra will improve the performance of our models. We discuss the predicted lifetimes, integrated luminosities, and mass-loss rate distributions of the calibrated models. The results of our calibration are included in updated stellar isochrones publicly available.

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