Light‐Element Abundance Patterns in the Orion Association. I.Hubble Space TelescopeObservations of Boron in G Dwarfs

2000 ◽  
Vol 543 (2) ◽  
pp. 850-860 ◽  
Author(s):  
Katia Cunha ◽  
Verne V. Smith ◽  
Etienne Parizot ◽  
David L. Lambert
Keyword(s):  
Light Element ◽  
Element Abundance ◽  
Abundance Patterns ◽  
Orion Association ◽  
Light Element Abundance

scholarly journals Multiple populations in integrated light spectroscopy of intermediate-age clusters

2019 ◽  
Vol 489 (1) ◽  
pp. L80-L85 ◽  
Author(s):  
Nate Bastian ◽  
Christopher Usher ◽  
Sebastian Kamann ◽  
Carmela Lardo ◽  
Søren S Larsen ◽  
...  
Keyword(s):  
Globular Clusters ◽  
Light Element ◽  
Large Magellanic Cloud ◽  
Element Abundance ◽  
Multiple Populations ◽  
Individual Stars ◽  
Abundance Patterns ◽  
Nearby Galaxies ◽  
Massive Clusters ◽  
Light Element Abundance

ABSTRACT The presence of star-to-star light-element abundance variations (also known as multiple populations, MPs) appears to be ubiquitous within old and massive clusters in the Milky Way and all studied nearby galaxies. Most previous studies have focused on resolved images or spectroscopy of individual stars, although there has been significant effort in the past few years to look for multiple population signatures in integrated light spectroscopy. If proven feasible, integrated light studies offer a potential way to vastly open parameter space, as clusters out to 10s of Mpc can be studied. We use the Na D lines in the integrated spectra of two clusters with similar ages (2–3 Gyr) but very different masses: NGC 1978 (∼3 × 105 M⊙) in the Large Magellanic Cloud and G114 (1.7 × 107 M⊙) in NGC 1316. For NGC 1978, our findings agree with resolved studies of individual stars that did not find evidence for Na spreads. However, for G114, we find clear evidence for the presence of multiple populations. The fact that the same anomalous abundance patterns are found in both the intermediate age and ancient globular clusters lends further support to the notion that young massive clusters are effectively the same as the ancient globular clusters, only separated in age.

scholarly journals Light element abundance inhomogeneities in globular clusters: probing star formation and evolution in the early Milky Way

1994 ◽  
Vol 72 (11-12) ◽  
pp. 772-781 ◽  
Author(s):  
Michael M. Briley ◽  
Roger A. Bell ◽  
James E. Hesser ◽  
Graeme H. Smith
Keyword(s):  
Star Formation ◽  
Globular Clusters ◽  
Main Sequence ◽  
Light Element ◽  
Star Formation History ◽  
Element Abundance ◽  
Chemical Compositions ◽  
Original Material ◽  
Abundance Patterns ◽  
Red Giant

Abundance patterns of the elements C, N, and O are sensitive probes of stellar nucleosynthesis processes and, in addition, O abundances are an important input for stellar age determinations. Understanding the nature of the observed distribution of these elements is key to constraining protogalactic star formation history. Patterns deduced from low-resolution spectroscopy of the CN, CH, NH, and CO molecules for low-mass stars in their core-hydrogen or first shell-hydrogen burning phases in the oldest ensembles known, the Galactic globular star clusters, are reviewed. New results for faint stars in NGC 104 (47 Tuc, C0021-723) reveal that the bimodal, anticorrelated pattern of CN and CH strengths found among luminous evolved stars is also present in stars nearing the end of their main-sequence lifetimes. In the absence of known mechanisms to mix newly synthesized elements from the interior to the observable surface layers of such unevolved stars, those particular inhomogeneities imply that the original material from which the stars formed some 15 billion years ago was chemically inhomogeneous in the C and N elements. However, in other clusters, observations of abundance ratios and C isotope ratios suggest that alterations to surface chemical compositions are produced as stars evolve from the main sequence through the red giant branch. Thus, the current observed distributions of C, N, and O among the brightest stars (those also observed most often) may not reflect the true distribution from which the protocluster cloud formed. The picture that is emerging of the C, N, and O abundance patterns within globular clusters may be one which requires a complicated combination of stellar evolutionary and primordial effects for its explanation.

scholarly journals Integrated spectroscopy of extragalactic Globular Clusters

2019 ◽  
Vol 14 (S351) ◽  
pp. 155-160
Author(s):  
Charli M. Sakari
Keyword(s):  
Globular Clusters ◽  
Milky Way ◽  
Light Element ◽  
Element Abundance ◽  
Future Perspectives ◽  
Host Galaxies ◽  
Chemical Abundances ◽  
Essential Information ◽  
Light Element Abundance ◽  
Detailed Chemical

AbstractIntegrated light (IL) spectroscopy enables studies of stellar populations beyond the Milky Way and its nearest satellites. In this paper, I will review how IL spectroscopy reveals essential information about globular clusters and the assembly histories of their host galaxies, concentrating particularly on the metallicities and detailed chemical abundances of the GCs in M31. I will also briefly mention the effects of multiple populations on IL spectra, and how observations of distant globular clusters help constrain the source(s) of light-element abundance variations. I will end with future perspectives, emphasizing how IL spectroscopy can bridge the gap between Galactic and extragalactic astronomy.

scholarly journals LIGHT-ELEMENT ABUNDANCE VARIATIONS AT LOW METALLICITY: THE GLOBULAR CLUSTER NGC 5466

2010 ◽  
Vol 140 (4) ◽  
pp. 1119-1127 ◽  
Author(s):  
Matthew Shetrone ◽  
Sarah L. Martell ◽  
Rachel Wilkerson ◽  
Joshua Adams ◽  
Michael H. Siegel ◽  
...  
Keyword(s):  
Globular Cluster ◽  
Light Element ◽  
Element Abundance ◽  
Low Metallicity ◽  
Light Element Abundance

scholarly journals The light element abundance distribution in NGC 5128 from planetary nebulae

2012 ◽  
Vol 544 ◽  
pp. A70 ◽  
Author(s):  
J. R. Walsh ◽  
G. H. Jacoby ◽  
R. F. Peletier ◽  
N. A. Walton
Keyword(s):  
Light Element ◽  
Planetary Nebulae ◽  
Element Abundance ◽  
Abundance Distribution ◽  
Light Element Abundance
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