The local high-velocity tail and the Galactic escape speed
May 21, 201913 pages
Published in:
- Mon.Not.Roy.Astron.Soc. 485 (2019) 3, 3514-3526
- Published: May 21, 2019
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Abstract: (Oxford University Press)
We model the fastest moving (||) local (D ≲ 3 kpc) halo stars using cosmological simulations and six-dimensional Gaia data. Our approach is to use our knowledge of the assembly history and phase-space distribution of halo stars to constrain the form of the high-velocity tail of the stellar halo. Using simple analytical models and cosmological simulations, we find that the shape of the high-velocity tail is strongly dependent on the velocity anisotropy and number density profile of the halo stars – highly eccentric orbits and/or shallow density profiles have more extended high-velocity tails. The halo stars in the solar vicinity are known to have a strongly radial velocity anisotropy, and it has recently been shown the origin of these highly eccentric orbits is the early accretion of a massive (||) dwarf satellite. We use this knowledge to construct a prior on the shape of the high-velocity tail. Moreover, we use the simulations to define an appropriate outer boundary of 2r_200, beyond which stars can escape. After applying our methodology to the Gaia data, we find a local (r_0 = 8.3 kpc) escape speed of ||. We use our measurement of the escape velocity to estimate the total Milky Way mass, and dark halo concentration: ||, ||. Our estimated mass agrees with recent results in the literature that seem to be converging on a Milky Way mass of ||.- Galaxy: fundamental parameters
- Galaxy: kinematics and dynamics
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