The binary content of multiple populations in NGC 3201

Kamann, Sebastian; Giesers, Benjamin; Bastian, Nate; Brinchmann, Jarle; Göttgens, Fabian; Husser, Tim-Oliver; Latour, M.; Weilbacher, Peter M.; Wisotzki, L.

doi:10.1051/0004-6361/201936843

Cited by 27 publications

(18 citation statements)

References 33 publications

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“…To give a few examples, Deacon and Kraus [20] found a measurable difference in the wide-binary frequency between open clusters and moving groups. In the globular cluster NGC 3201, Kamann et al [21] measured a binary frequency of 23.1 ± 6.1% in the first population of stars and 8.2 ± 3.5% in the second-generation population that formed later in a more dynamically active environment.…”

Section: Statistical Trendsmentioning

confidence: 99%

Architecture of Hierarchical Stellar Systems and Their Formation

Tokovinin

2021

Universe

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Accumulation of new data on stellar hierarchical systems and the progress in numerical simulations of their formation open the door to genetic classification of these systems, where properties of a certain group (family) of objects are tentatively related to their formation mechanisms and early evolution. A short review of the structure and statistical trends of known stellar hierarchies is given. Like binaries, they can be formed by the disk and core fragmentation events happening sequentially or simultaneously and followed by the evolution of masses and orbits driven by continuing accretion of gas and dynamical interactions between stars. Several basic formation scenarios are proposed and associated qualitatively with the architecture of real systems, although quantitative predictions for these scenarios are still pending. The general trend of increasing orbit alignment with decreasing system size points to the critical role of the accretion-driven orbit migration, which also explains the typically comparable masses of stars belonging to the same system. The architecture of some hierarchies bears imprints of chaotic dynamical interactions. Characteristic features of each family are illustrated by several real systems.

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Section: Statistical Trendsmentioning

confidence: 99%

Architecture of Hierarchical Stellar Systems and Their Formation

Tokovinin

2021

Universe

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“…If at all, we see some stars with an excess metallicity. The binary content of multiple populations in NGC 3201 is investigated in detail in Kamann et al (2020).…”

Section: Ngc 3201mentioning

confidence: 99%

A stellar census in globular clusters with MUSE

Husser

Latour

Brinchmann

et al. 2020

A&A

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Aims. We use the spectra of more than 30 000 red giant branch (RGB) stars in 25 globular clusters (GC), obtained within the MUSE survey of Galactic globular clusters, to calibrate the Ca II triplet metallicity relation and derive metallicities for all individual stars. We investigate the overall metallicity distributions as well as those of the different populations within each cluster. Methods. The Ca II triplet in the near-infrared at 8498, 8542, and 8662 Å is visible in stars with spectral types between F and M and can be used to determine their metallicities. In this work, we calibrate the relation using average cluster metallicities from literature and MUSE spectra, and extend it below the horizontal branch – a cutoff that has traditionally been made to avoid a non-linear relation – using a quadratic function. In addition to the classic relation based on V − VHB, we also present calibrations based on absolute magnitude and luminosity. The obtained relations were used to calculate metallicities for all the stars in the sample and to derive metallicity distributions for different populations within a cluster, which have been separated using so-called “chromosome maps” based on HST photometry. Results. We show that despite the relatively low spectral resolution of MUSE (R = 1900 − 3700) we can derive single star metallicities with a mean statistical intra-cluster uncertainty of ∼0.12 dex. We present metallicity distributions for the RGB stars in 25 GCs and investigate the different metallicities of the populations P3 (and higher) in so-called metal-complex or Type II clusters, finding metallicity variations in all of them. We also detected unexpected metallicity variations in the Type I cluster NGC 2808 and confirm the Type II status of NGC 7078.

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“…On the other hand a range of Fe is not found by Cabrera-Ziri et al ( 2019) along the extended P1 sequence of NGC 2808. A recent analysis by Martins et al (2020) has also excluded binaries (see also Kamann et al 2020) and chromospheric activity as explanations for the observed extended P1 sequences.…”

Section: Pseudocolours and Chromosome Mapsmentioning

confidence: 99%