http://arxiv.org/abs/1804.11348
We estimate the mass of the Milky Way (MW) within 21.1 kpc using the kinematics of halo globular clusters (GCs) determined by Gaia. The second Gaia data release (DR2) contained a catalogue of absolute proper motions (PMs) for a set of Galactic GCs and satellite galaxies measured using Gaia DR2 data. We select from the catalogue only halo GCs, identifying a total of 34 GCs spanning $2.0 < r < 21.1$ kpc, and use their 3D kinematics to estimate the anisotropy over this range to be $\beta = 0.48^{+0.15}{-0.20}$, in good agreement, though slightly lower than, a recent estimate for a sample of halo GCs using HST PM measurements further out in the halo. We then use the Gaia kinematics to estimate the mass of the MW inside the outermost GC to be $M(< 21.1 \mathrm{kpc}) = 0.22^{+0.04}{-0.03} 10^{12} \mathrm{M_\odot}$, which corresponds to a circular velocity of $v_\mathrm{circ}(21.1 \mathrm{kpc}) = 213^{+20}{-17}$ km/s. The implied virial mass is $M\mathrm{virial} = 1.41^{+1.99}{-0.52} 10^{12} \mathrm{M\odot}$. The error bars encompass the uncertainties on the anisotropy and on the density profile of the MW dark halo, and the shot noise inherent in the mass estimator we use. We get improved estimates when we combine the Gaia and HST samples to provide kinematics for 46 GCs out to 39.5 kpc: $\beta = 0.52^{+0.12}{-0.15}$, $M(< 39.5 \mathrm{kpc}) = 0.44^{+0.07}{-0.06} 10^{12} \mathrm{M_\odot}$, and $M_\mathrm{virial} = 1.67^{+0.79}{-0.50} 10^{12} \mathrm{M\odot}$. We show that these results are robust to potential substructure in the halo GC distribution. While a wide range of MW virial masses have been advocated in the literature, from below $10^{12} \mathrm{M_\odot}$ to above $2 \times 10^{12}\mathrm{M_\odot}$, these new data imply that an intermediate mass is most likely.
L. Watkins, R. Marel, S. Sohn, et. al.
Tue, 1 May 18
15/78
Comments: 16 pages, 8 figures, 3 tables, submitted to AAS Journals
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