The Sagittarius Dwarf Galaxy: a Model for Evolution in a Triaxial Milky Way Halo

TL;DR

This paper introduces a new N-body model of the Sagittarius dwarf galaxy's tidal disruption within a triaxial Milky Way halo, successfully matching many observational constraints and revealing insights into the galaxy's debris streams and halo shape.

Contribution

The model incorporates a non-axisymmetric, triaxial dark matter halo to accurately reproduce the Sagittarius tidal streams and their properties, addressing previous conflicting observations.

Findings

Model fits most angular, distance, and velocity constraints of debris streams.

Reproduces metallicity gradients along tidal streams.

Suggests a nearly-oblate halo shape with specific axis ratios.

Abstract

We present a new N-body model for the tidal disruption of the Sagittarius (Sgr) dwarf that is capable of simultaneously satisfying the majority of angular position, distance, and radial velocity constraints imposed by current wide-field surveys of its dynamically young (< 3 Gyr) tidal debris streams. In particular, this model resolves the conflicting angular position and radial velocity constraints on the Sgr leading tidal stream that have been highlighted in recent years. While the model does not reproduce the apparent bifurcation observed in the leading debris stream, recent observational data suggest that this bifurcation may represent a constraint on the internal properties of the Sgr dwarf rather than the details of its orbit. The key element in the success of this model is the introduction of a non-axisymmetric component to the Galactic gravitational potential which can be described in terms of a triaxial dark matter halo whose minor/major axis ratio (c/a)_Phi = 0.72 and intermediate/major axis ratio (b/a)_Phi = 0.99 at radii 20 < r < 60 kpc. The minor/intermediate/major axes of this halo lie along the directions (l, b) = (7, 0), (0, 90), and (97, 0) respectively, corresponding to a nearly-oblate ellipsoid whose minor axis is contained within the Galactic disk plane. We demonstrate that with simple assumptions about the star formation history of Sgr, tidal stripping models naturally give rise to gradients in the metallicity distribution function (MDF) along the stellar debris streams similar to those observed in recent studies. (Abridged).