The normal chemistry of multiple stellar populations in the dense globular cluster NGC 6093 (M 80)

Carretta, E.; Bragaglia, A.; Gratton, R.; D’Orazi, V.; Lucatello, S.; Sollima, A.; Momany, Y.; Catanzaro, G.; Leone, F.

doi:10.1051/0004-6361/201525951

Cited by 51 publications

(46 citation statements)

References 119 publications

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“…Wheeler et al 1989). This pattern is also Carretta et al (2009aCarretta et al ( ,b, 2010bCarretta et al ( ,c, 2011Carretta et al ( , 2013Carretta et al ( , 2014bCarretta et al ( , 2015, and asterisks are stars in NGC 2808 from . In each panel the error bars represent internal errors.…”

Section: Elements Up To Iron Peaksupporting

confidence: 49%

Chemical characterisation of the globular cluster NGC 5634 associated to the Sagittarius dwarf spheroidal galaxy

Carretta

Bragaglia

Lucatello

et al. 2017

A&A

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As part of our on-going project on the homogeneous chemical characterisation of multiple stellar populations in globular clusters (GCs), we studied NGC 5634, associated to the Sagittarius dwarf spheroidal galaxy, using high-resolution spectroscopy of red giant stars collected with VLT/FLAMES. We present here the radial velocity distribution of the 45 observed stars, 43 of which are cluster members, the detailed chemical abundance of 22 species for the seven stars observed with UVES-FLAMES, and the abundance of six elements for stars observed with GIRAFFE. On our homogeneous UVES metallicity scale, we derived a low-metallicity [Fe/H] = −1.867 ± 0.019 ± 0.065 dex (±statistical ±systematic error) with σ = 0.050 dex (7 stars). We found the normal anticorrelations between light elements (Na and O, Mg and Al), a signature of multiple populations typical of massive and old GCs. We confirm the associations of NGC 5634 to the Sgr dSph, from which the cluster was lost a few Gyr ago, on the basis of its velocity and position, and the abundance ratios of α and neutron capture elements.

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Section: Elements Up To Iron Peaksupporting

confidence: 49%

Chemical characterisation of the globular cluster NGC 5634 associated to the Sagittarius dwarf spheroidal galaxy

Carretta

Bragaglia

Lucatello

et al. 2017

A&A

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“…In the upper panel we indicate the separation between P and I, and I and E populations, according to Carretta et al (2009a). (Carretta et al 2009a(Carretta et al , 2010b(Carretta et al , 2011a(Carretta et al , 2013b(Carretta et al , 2014b(Carretta et al , 2015 In conclusion, with our study of 45 member stars in NGC 6139 conducted with FLAMES spectra, we determined for the first time its metallicity with high-resolution spectroscopy (the cluster has an intermediate metallicity, with [Fe/H] = −1.58 dex). We also measured the light elements O, Na, Mg, and Al involved in proton-capture reactions of H-burning at high temperatures; we detected the usual correlations and anticorrelations found in almost all GCs investigated so far.…”

Section: Light Element Anti-correlationsmentioning

confidence: 99%

NGC 6139: a normal massive globular cluster, or a first-generation dominated cluster? Clues from the light elements

Bragaglia¹,

Carretta²,

Sollima³

et al. 2015

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Information on globular clusters (GC) formation mechanisms can be gathered by studying the chemical signature of the multiple populations that compose these stellar systems. In particular, we investigate the anti-correlations among O, Na, Al, and Mg to explore the influence of cluster mass and environment on GCs in the Milky Way and in extragalactic systems. We present here the results obtained on NGC 6139, which, on the basis of its horizontal branch morphology, has been proposed to be dominated by first-generation stars. In our extensive study based on high-resolution spectroscopy, the first for this cluster, we found a metallicity of [Fe/H] = −1.579 ± 0.015 ± 0.058 (rms = 0.040 dex, 45 bona fide member stars) on the UVES scale defined by our group. The stars in NGC 6139 show a chemical pattern normal for GCs, with a rather extended Na-O (and Mg-Al) anti correlation. NGC 6139 behaves as expected from its mass and contains a large portion (about two thirds) of second-generation stars.

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“…To date, the largest homogeneous sample of GC stars with high resolution spectroscopy is that collected within the FLAMES Globular Cluster Na-O survey by Carretta et al 2015, and references therein). Fe, O, and Na abundances have been measured for these objects, allowing them to be classified into first and second generation stars.…”

Section: Introductionmentioning

confidence: 99%

The incidence of binaries in globular cluster stellar populations

Lucatello

Sollima

Gratton

et al. 2015

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Binary fraction and orbital characteristics provide indications on the conditions of star formation, as they shed light on the environment they were born in. Multiple systems are more common in low density environments than in higher density environments. In the current debate about the formation of globular clusters and their multiple populations, studying the binary incidence in the populations they host offers a crucial piece of information on the environment of their birth and their subsequent dynamical evolution. Through a multiyear observational campaign using FLAMES at VLT, we monitored the radial velocity of 968 red-giant-branch stars located around the half-light radii in a sample of ten Galactic globular clusters. We found a total of 21 radial velocity variables identified as bona fide binary stars, for a binary fraction of 2.2% ± 0.5%. When separating the sample into first generation and second generation stars, we find a binary fraction of 4.9% ± 1.3% and 1.2% ± 0.4%, respectively. Through simulations that take possible sources of bias into account in detecting radial velocity variations in the two populations, we show that the difference is significant and only marginally affected by these effects. This kind of different binary fraction strongly suggests different conditions in the environment of formation and evolution of first and second generations stars, with the latter being born in a much denser environment. Our result hence strongly supports the idea that the second generation forms in a dense subsystem at the center of the loosely distributed first generation, where (loose) binaries are efficiently destroyed.

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The normal chemistry of multiple stellar populations in the dense globular cluster NGC 6093 (M 80)

Cited by 51 publications

References 119 publications

Chemical characterisation of the globular cluster NGC 5634 associated to the Sagittarius dwarf spheroidal galaxy

Chemical characterisation of the globular cluster NGC 5634 associated to the Sagittarius dwarf spheroidal galaxy

NGC 6139: a normal massive globular cluster, or a first-generation dominated cluster? Clues from the light elements

The incidence of binaries in globular cluster stellar populations

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