Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Quick Search
My eDoc
Session History
Support Wiki
Direct access to
document ID:

          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 742733.0, MPI für Astronomie / Publikationen_mpia
Triaxial orbit-based modelling of the Milky Way Nuclear Star Cluster
Authors:Feldmeier-Krause, A.; Zhu, L.; Neumayer, N.; van de Ven, G.; de Zeeuw, P. T.; Schödel, R.
Date of Publication (YYYY-MM-DD):2017
Title of Journal:Monthly Notices of the Royal Astronomical Society
Issue / Number:4
Start Page:4040
End Page:4052
Audience:Not Specified
Abstract / Description:We construct triaxial dynamical models for the Milky Way nuclear star cluster using Schwarzschild's orbit superposition technique. We fit the stellar kinematic maps presented in Feldmeier et al. The models are used to constrain the supermassive black hole mass M, dynamical mass-to-light ratio ϒ and the intrinsic shape of the cluster. Our best-fitting model has M = (3.0^{+1.1}_{-1.3}) × 106 M, ϒ = (0.90^{+0.76}_{-0.08}) M/L⊙, 4.5μm and a compression of the cluster along the line of sight. Our results are in agreement with the direct measurement of the supermassive black hole mass using the motion of stars on Keplerian orbits. The mass-to-light ratio is consistent with stellar population studies of other galaxies in the mid-infrared. It is possible that we underestimate M and overestimate the cluster's triaxiality due to observational effects. The spatially semiresolved kinematic data and extinction within the nuclear star cluster bias the observations to the near side of the cluster, and may appear as a compression of the nuclear star cluster along the line of sight. We derive a total dynamical mass for the Milky Way nuclear star cluster of MMWNSC = (2.1 ± 0.7) × 107 M within a sphere with radius r = 2 × reff = 8.4 pc. The best-fitting model is tangentially anisotropic in the central r = 0.5-2 pc of the nuclear star cluster, but close to isotropic at larger radii. Our triaxial models are able to recover complex kinematic substructures in the velocity map.
Free Keywords:Galaxy: center; kinematics and dynamics; Galaxy: centre; Galaxy: kinematics and dynamics
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0035-8711 %R 10.1093/mnras/stw3377
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.