Precession of the Sagittarius stream
V. Belokurov, S.E. Koposov, N.W. Evans, J. Pe\~narrubia, M.J. Irwin,, M.C. Smith, G.F. Lewis, M. Gieles, M.I. Wilkinson, G. Gilmore, E.W., Olszewski, M.N. Niederste-Ostholt

TL;DR
This study maps the Sagittarius stream using stellar tracers, revealing new debris detections, precise distances, and velocities, which challenge existing models of the Milky Way's dark matter distribution and show differential precession in the stream.
Contribution
It provides new measurements of the Sgr stream's apo-centres, distances, and velocities, and highlights discrepancies with current disruption simulations and models of the Galactic halo.
Findings
Apo-centre distances: 47.8 kpc (leading), 102.5 kpc (trailing)
Angular difference between apo-centres: 93.2 degrees
Sgr debris shows differential precession in different tails
Abstract
Using a variety of stellar tracers -- blue horizontal branch stars, main-sequence turn-off stars and red giants -- we follow the path of the Sagittarius (Sgr) stream across the sky in Sloan Digital Sky Survey data. Our study presents new Sgr debris detections, accurate distances and line-of-sight velocities that together help to shed new light on the puzzle of the Sgr tails. For both the leading and the trailing tail, we trace the points of their maximal extent, or apo-centric distances, and find that they lie at = 47.8 0.5 kpc and = 102.5 2.5 kpc respectively. The angular difference between the apo-centres is 93.2 3.5 deg, which is smaller than predicted for logarithmic haloes. Such differential orbital precession can be made consistent with models of the Milky Way in which the dark matter density falls more quickly with radius. However, currently, no…
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