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Author: Böker, Torsten ×

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    Erratum: "Resolved Nuclear Kinematics Link the Formation and Growth of Nuclear Star Clusters with the Evolution of Their Early and Late-type Hosts" (2021, ApJ, 921, 8)
    (London : Institute of Physics Publ., 2021) Pinna, Francesca; Neumayer, Nadine; Seth, Anil; Emsellem, Eric; Nguyen, Dieu D.; Böker, Torsten; Cappellari, Michele; McDermid, Richard M.; Voggel, Karina; Walcher, C. Jakob
    We have identified an error in Equations (D3) and (D4) in Appendix D of the published article. These equations result from the combination of Equations (16), (17), and (18) in Harborne et al. (2020). In the published article, the right-hand sides are swapped with each other. The corrected versions of the equations are (Formula Presented). All results shown and discussed in the published article were obtained using the correct version of the equations and do not need any modifications.
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    A Deep View into the Nucleus of the Sagittarius Dwarf Spheroidal Galaxy with MUSE. III. Discrete Multicomponent Population-dynamical Models Based on the Jeans Equations
    (London : Institute of Physics Publ., 2022) Kacharov, Nikolay; Alfaro-Cuello, Mayte; Neumayer, Nadine; Lützgendorf, Nora; Watkins, Laura L.; Mastrobuono-Battisti, Alessandra; Kamann, Sebastian; van de Ven, Glenn; Seth, Anil C.; Voggel, Karina T.; Georgiev, Iskren Y.; Leaman, Ryan; Bianchini, Paolo; Böker, Torsten; Mieske, Steffen
    We present comprehensive multicomponent dynamical models of M54 (NGC 6715), the nuclear star cluster of the Sagittarius (Sgr) dwarf galaxy, which is undergoing a tidal disruption in the Milky Way halo. Previous papers in this series used a large MUSE mosaic data set to identify multiple stellar populations in the system and study their kinematic differences. Here, we use Jeans-based dynamical models that fit the population properties (mean age and metallicity), spatial distributions, and kinematics simultaneously. They provide a solid physical explanation for our previous findings. Population-dynamical models deliver a comprehensive view of the whole system, and allow us to disentangle the different stellar populations. We explore their dynamical interplay and confirm our previous findings about the build-up of Sgr’s nuclear cluster via contributions from globular cluster stars, Sgr inner field stars, and in situ star formation. We explore various parameterizations of the gravitational potential and show the importance of a radially varying mass-to-light ratio for the proper treatment of the mass profile. We find a total dynamical mass within M54's tidal radius (∼75 pc) of 1.60 ± 0.07 × 106 M ⊙ in excellent agreement with N-body simulations. Metal-poor globular cluster stars contribute about 65% of the total mass or 1.04 ± 0.05 × 106 M ⊙. Metal-rich stars can be further divided into young and intermediate-age populations, which contribute 0.32 ± 0.02 × 106 M ⊙ (20%) and 0.24 ± 0.02 × 106 M ⊙ (15%), respectively. Our population-dynamical models successfully distinguish the different stellar populations in Sgr’s nucleus because of their different spatial distributions, ages, metallicities, and kinematic features.