Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 486, Issue 2, Pages 2679-2694Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stz973
Keywords
Galaxy: kinematics and dynamics; galaxies: dwarf; dark matter
Categories
Funding
- Texas A&M University Merit Fellowship
- European Union CO-FUND/Durham Junior Research Fellowship
- EU [609412]
- Texas AM University
- George P. and Cynthia Woods Institute for Fundamental Physics and Astronomy
- DOE [de-sc0010813]
- European Research Council (ERC) Advanced Investigator grant [GA 786910]
- FONDECYT Regular [1181264]
- Max Planck Society through a Partner Group grant
- Deutsche Forschungsgemeinschaft (DFG) Research Centre Sonderforschungsbereich
- Compute Canada Calcul Canada [PR85JE]
- Gauss Centre for Supercomputing
- UK Science and Technology Facilities Council (STFC) [ST/P000541/1]
- BIS National E-infrastructure capital grant [ST/K00042X/1]
- STFC capital grant [ST/H008519/1]
- STFC DiRAC Operations grant [ST/K003267/1]
- Durham University
- STFC [ST/K00042X/1, ST/T001550/1, ST/T001348/1, ST/T001569/1, ST/R001014/1, ST/M006948/1, ST/M007073/1, ST/P000541/1, ST/R001006/1, ST/M007006/1, ST/M007065/1, ST/S002529/1, ST/T001372/1, ST/R00689X/1, ST/H008519/1, ST/M007618/1, ST/R001049/1, ST/R000832/1] Funding Source: UKRI
Ask authors/readers for more resources
We analyse the orbital kinematics of the Milky Way (MW) satellite system utilizing the latest systemic proper motions for 38 satellites based on data from Gaia Data Release 2. Combining these data with distance and line-of-sight velocity measurements from the literature, we use a likelihood method to model the velocity anisotropy, beta, as a function of Galactocentric distance and compare the MW satellite system with those of simulated MW-mass haloes from the APOSTLE (A Project Of Simulating The Local Environment) and Auriga simulation suites. The anisotropy profile for the MW satellite system increases from beta similar to -2 at r similar to 20 kpc to beta similar to 0.5 at r similar to 200 kpc, indicating that satellites closer to the Galactic centre have tangentially biased motions while those farther out have radially biased motions. The motions of satellites around APOSTLE host galaxies are nearly isotropic at all radii, while the beta(r) profiles for satellite systems in the Auriga suite, whose host galaxies are substantially more massive in baryons than those in APOSTLE, are more consistent with that of the MW satellite system. This shape of the beta(r) profile may be attributed to the central stellar disc preferentially destroying satellites on radial orbits, or intrinsic processes from the formation of the MW system.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available