Milky Way total Mass derived by Rotation Curve and Globular Cluster kinematics from Gaia EDR3

Abstract

Using action-based distribution function for the dynamical model of the Milky Way we have estimated its total mass and its density profile. Constraints are coming from the globular cluster proper motions from Gaia EDR3, from the rotation curve based on Gaia DR2 data, and from the vertical force data. We use Bayesian Markov chain Monte Carlo method to explore the parameters, for which the globular cluster distribution function and the Galactic potential are fully constrained. Numerical simulations are used to study the uncertainties on the potential constraint if considering a possible massive Large Magellanic Could (LMC). We found that a massive LMC (1.5$\times 10^{11}$ M${}_{\odot }$) will affect the MW mass measurement at large radius, which includes both the Milky Way and the LMC. We also use the FIRE2 Latte cosmological hydrodynamic simulations to make mock data set from a Milky-Way like galaxy that includes many unrelaxed substructures. We test the effect of these unrelaxed substructures on the final results, and found that the measured rotation curve fluctuated around input value within 5 percent. By keeping a large freedom in choosing a priori mass profile for both baryonic and dark matter leads a total mass of the MW that ranges from $5.36_{-0.68}^{+0.81}\times 10^{11}$ M${}_{\odot }$ to $7.84_{-1.97}^{+3.08}\times 10^{11}$ M$\odot$. This includes the contribution of a putative massive LMC and significantly narrows the MW total mass range published earlier. Such total mass leads to dark matter density at solar position of $0.34_{-0.02}^{+0.02}$ GeV cm${}^{-3}$.

21 pages, 18 Figures, 2 Tables, proof-corrected version, to be published in MNRAS

References in corpus (30)

• galpy: A Python Library for Galactic Dynamics
• Too big to fail? The puzzling darkness of massive Milky Way subhaloes
• The mass distribution and gravitational potential of the Milky Way
• The redshift dependence of the structure of massive LCDM halos
• Evidence for Two Early Accretion Events That Built the Milky Way Stellar Halo
• Gaia EDR3 view on Galactic globular clusters
• The Local Dark Matter Density
• On the frequency, intensity and duration of starburst episodes triggered by galaxy interactions and mergers
• "Skinny Milky Way, Please", says Sagittarius
• On the Shoulders of Giants: Properties of the Stellar Halo and the Milky Way Mass Distribution
• Constraining the Galaxy's dark halo with RAVE stars
• Globular Cluster Streams as Galactic High-Precision Scales - The Poster Child Palomar 5
• Kinematics of the stellar halo and the mass distribution of the Milky Way using BHB stars
• The shape of the inner Milky Way halo from observations of the Pal 5 and GD-1 stellar streams
• The total stellar halo mass of the Milky Way
• All-Sky Dynamical Response of the Galactic Halo to the Large Magellanic Cloud
• The local high velocity tail and the Galactic escape speed
• Detection of the Milky Way reflex motion due to the Large Magellanic Cloud infall
• Dipping Our Toes in the Water: First Models of GD-1 as a Stream
• Action-based distribution functions for spheroidal galaxy components
• A Milky Way with a massive, centrally concentrated thick disc: new Galactic mass models for orbit computations
• The Rotation Curve, Mass Distribution and Dark Matter Content of the Milky Way from Classical Cepheids
• Toward a Complete Understanding of the Magellanic Stream Formation
• The effects of dynamical substructure on Milky Way mass estimates from the high velocity tail of the local stellar halo
• The Milky Way Tomography with SDSS. V. Mapping the Dark Matter Halo
• Characterizing stellar halo populations II: The age gradient in blue horizontal-branch stars
• Subhalo statistics of galactic halos: beyond the resolution limit
• Modelling the Milky Way's globular cluster system
• Which Milky Way masses are consistent with the slightly declining 5-25 kpc rotation curve?
• Chemical abundances of giant stars in the Crater stellar system

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• Detection of the Keplerian decline in the Milky Way rotation curve
• Measuring the Milky Way mass distribution in the presence of the LMC
• Mapping the Milky Way Disk with Gaia DR3: 3D extended kinematic maps and rotation curve to $\approx 30$ kpc
• Strong constraints on the gravitational law from $Gaia$ DR3 wide binaries
• Self-consistent models of our Galaxy
• Exploring dark matter spike distribution around the Galactic centre with stellar orbits
• Milky Way Mass with K Giants and BHB Stars Using LAMOST, SDSS/SEGUE, and Gaia: 3D Spherical Jeans Equation and Tracer Mass Estimator
• A self-consistent dynamical model of the Milky Way disc adjusted to Gaia data
• Implications of the Milky Way travel velocity for dynamical mass estimates of the Local Group
• Hydrodynamical structure formation in Milgromian cosmology
• Constructing the Milky Way Stellar Halo in the Galactic Center by Direct Orbit Integration
• The Escape Velocity Profile of the Milky Way from Gaia DR3
• How Close Dark Matter Halos and MOND Are to Each Other: Three-Dimensional Tests Based on Gaia DR2
• Bar-driven dispersal of Galactic substructure
• First spiral arm detection using dynamical mass measurements of the Milky Way disk
• On the anti-correlation between pericentric distance and inner dark matter density of Milky Way's dwarf spheroidal galaxies
• A Pristine-UNIONS view on the Galaxy: Kinematics of the distant spur feature of the Sagittarius stream traced by Blue Horizontal Branch stars
• Dark Matter Freeze-In and Small-Scale Observables: Novel Mass Bounds and Viable Particle Candidates
• Prospects for probing small-scale dark matter models with pulsars around Sagittarius A*
• The outskirts of M33: Tidally induced distortions versus signatures of gas accretion
• Exploring Milky Way rotation curves with Gaia DR3: a comparison between $\Lambda$CDM, MOND, and General Relativistic approaches
• Milky Way Mass Through Escape Velocity Curve from LAMOST K Giants
• Quantifying the Milky Way, LMC and their interaction using all-sky kinematics of outer halo stars
• Impact of merger histories on the timing argument estimate of the Local Group mass