Constraining the Milky Way Halo Potential with the GD-1 stellar stream

Abstract

We use ESA/Gaia astrometry together with SEGUE and LAMOST measurements of the GD-1 stellar stream to explore the improvement on the Galactic gravitational potential that these new data provide. Assuming a realistic universal model for the dark matter halo together with reasonable models of the baryonic components, we find that the orbital solutions for GD-1 require the circular velocity at the Solar radius to be $V_{\mathrm{circ}}(R_{\odot })=244\pm 4\mathrm{km}{\mathrm{s}}^{-1}$, and also that the density flattening of the dark halo is $q_{\rho }=0.82_{-0.13}^{+0.25}$. The corresponding Galactic mass within 20kpc was estimated to be $M_{\mathrm{MW}}(<20kpc)=2.5\pm 0.2\times 10^{11}{M}_{\odot }$. Moreover, Gaia's excellent proper motions also allowed us to constrain the velocity dispersion of the GD-1 stream in the direction tangential to the line of sight to be $<2.30\mathrm{km}{\mathrm{s}}^{-1}$ (95 % confidence limit), confirming the extremely cold dynamical nature of this system.

12 pages, 8 Figures, 2 Tables, accepted by MNRAS

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