The nuclear stellar disc (NSD) is a flattened high-density stellar structure that dominates the gravitational field of the Milky Way at Galactocentric radius 30 pc less than or similar to R less than or similar to 300 pc. We construct axisymmetric self-consistent equilibrium dynamical models of the NSD in which the distribution function is an analytic function of the action variables. We fit the models to the normalized kinematic distributions (line-of-sight velocities + VIRAC2 proper motions) of stars in the NSD survey of Fritz et al., taking the foreground contamination due to the Galactic Bar explicitly into account using an N-body model. The posterior marginalized probability distributions give a total mass of M-NSD = 10.5(-1.0)(+1.1) x 10(8) M-circle dot, roughly exponential radial and vertical scale lengths of R-disc = 88.6(-6.9)(+9.2) pc and H-disc = 28.4(-5.5)(+5.5) pc, respectively, and a velocity dispersion sigma similar or equal to 70 km s(-1) that decreases with radius. We find that the assumption that the NSD is axisymmetric provides a good representation of the data. We quantify contamination from the Galactic Bar in the sample, which is substantial in most observed fields. Our models provide the full 6D (position + velocity) distribution function of the NSD, which can be used to generate predictions for future surveys. We make the models publicly available as part of the software package AGAMA.

Self-consistent modelling of the Milky Way's nuclear stellar disc

Sormani M
;
2022-01-01

Abstract

The nuclear stellar disc (NSD) is a flattened high-density stellar structure that dominates the gravitational field of the Milky Way at Galactocentric radius 30 pc less than or similar to R less than or similar to 300 pc. We construct axisymmetric self-consistent equilibrium dynamical models of the NSD in which the distribution function is an analytic function of the action variables. We fit the models to the normalized kinematic distributions (line-of-sight velocities + VIRAC2 proper motions) of stars in the NSD survey of Fritz et al., taking the foreground contamination due to the Galactic Bar explicitly into account using an N-body model. The posterior marginalized probability distributions give a total mass of M-NSD = 10.5(-1.0)(+1.1) x 10(8) M-circle dot, roughly exponential radial and vertical scale lengths of R-disc = 88.6(-6.9)(+9.2) pc and H-disc = 28.4(-5.5)(+5.5) pc, respectively, and a velocity dispersion sigma similar or equal to 70 km s(-1) that decreases with radius. We find that the assumption that the NSD is axisymmetric provides a good representation of the data. We quantify contamination from the Galactic Bar in the sample, which is substantial in most observed fields. Our models provide the full 6D (position + velocity) distribution function of the NSD, which can be used to generate predictions for future surveys. We make the models publicly available as part of the software package AGAMA.
2022
2022
Galaxy: centre, Galaxy: kinematics and dynamics, Galaxy: structure
Sormani, M; Sanders, Jl; Fritz, Tk; Smith, Lc; Gerhard, O; Schodel, R; Magorrian, J; Neumayer, N; Nogueras-Lara, F; Feldmeier-Krause, A; Mastrobuono-Battisti, A; Schultheis, M; Shahzamanian, B; Vasiliev, E; Klessen, Rs; Lucas, P; Minniti, D
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11383/2171037
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