期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 513, 期 4, 页码 4968-4982出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stac1265
关键词
Galaxy: fundamental parameters; galaxies: dwarf; galaxies: evolution; galaxies: general; galaxies: kinematics and dynamics; Local Group
资金
- National Science Foundation (NSF) [AST-1815475, AST-1518257]
- National Science Foundation Graduate Research Fellowship
- Math and Physical Sciences (MPS) Ascend Postdoctoral Research Fellowship
- National Science Foundation Graduate Research Fellowship Program [DGE-1321846]
- National Science Foundation MPS-Ascend Postdoctoral Research Fellowship [AST-2138144]
- NSF CAREER award [AST-1752913]
- NSF [AST-1910346]
- National Aeronautics and Space Administration (NASA) [NNX17AG29G]
- Space Telescope Science Institute [HST-AR-15006, HST-AR-15809, HST-GO-15658, HST-GO-15901, HST-GO-15902, HST-AR-16159, HST-GO-16226]
- NASA [ATP 80NSSC20K0566, NAS5-26555]
- NSF CAREER [1945310]
- Large Synoptic Survey Telescope Corporation (LSSTC) Data Science Fellowship Program - LSSTC, NSF [1829740]
- Brinson Foundation
- Moore Foundation
- Direct For Computer & Info Scie & Enginr
- Office of Advanced Cyberinfrastructure (OAC) [1829740] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1945310] Funding Source: National Science Foundation
As the Milky Way and its satellite system become more important in cosmological studies, accurately estimating the mass of the Milky Way's dark matter halo is crucial. Utilizing data from stellar proper motions and simulations, a mass estimate of around 1-1.2 x 10(12) M-circle dot for the Milky Way's dark matter halo has been derived.
As the Milky Way and its satellite system become more entrenched in near field cosmology efforts, the need for an accurate mass estimate of the Milky Way's dark matter halo is increasingly critical. With the second and early third data releases of stellar proper motions from Gaia, several groups calculated full 6D phase-space information for the population of Milky Way satellite galaxies. Utilizing these data in comparison to subhalo properties drawn from the Phat ELVIS simulations, we constrain the Milky Way dark matter halo mass to be similar to 1-1.2 x 10(12) M-circle dot. We find that the kinematics of subhaloes drawn from more- or less-massive hosts (i.e. >1.2 x 10(12) M-circle dot or <10(12) M-circle dot) are inconsistent, at the 3 sigma confidence level, with the observed velocities of the Milky Way satellites. The preferred host halo mass for the Milky Way is largely insensitive to the exclusion of systems associated with the Large Magellanic Cloud, changes in galaxy formation thresholds, and variations in observational completeness. As more Milky Way satellites are discovered, their velocities (radial, tangential, and total) plus Galactocentric distances will provide further insight into the mass of the Milky Way dark matter halo.
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