Galactic Accelerations from the GD-1 Stream Suggest a Tilted Dark Matter Halo

Abstract Cold dark matter halos are expected to be triaxial and often tilted relative to the stellar disk. Stellar streams provide a sensitive tracer of the Milky Way’s halo shape though models for the Galactic potential are typically limited to simple, symmetric functional forms. Here, we measure the Galactic acceleration field along the GD-1 stream using a direct differentiation of the stream’s track in phase space. Using a fully data-driven catalog of stream members from Gaia, Sloan Digital Sky Survey, LAMOST, and DESI, we map the stream in 6D phase space. We fit splines to the stream track and infer cylindrical acceleration components <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>a</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>R</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:mn>2.5</mml:mn> <mml:msubsup> <mml:mrow> <mml:mo>±</mml:mo> </mml:mrow> <mml:mrow> <mml:mn>0.1</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>0.2</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> , a z = −1.8 ± 0.1, and a ϕ = 0.2 ± 0.1 km s −1 Myr −1 at ( R , z , ϕ ) = (11.9 kpc, 7.3 kpc, 171 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover> <mml:mrow> <mml:mo>.</mml:mo> </mml:mrow> <mml:mrow> <mml:mtext>°</mml:mtext> </mml:mrow> </mml:mover> </mml:math> 1). We measure mass enclosed within 14 kpc of 1.4 ± 0.1 × 10 11 M ⊙ and z -axis density flattening of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>q</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>ρ</mml:mi> <mml:mo>,</mml:mo> <mml:mi>z</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:mn>0.81</mml:mn> <mml:msubsup> <mml:mrow> <mml:mo>±</mml:mo> </mml:mrow> <mml:mrow> <mml:mn>0.03</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>0.06</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> , both consistent with previous estimates. However, we find a 2 σ deviation from an axisymmetric acceleration field, which can be explained by a triaxial dark matter halo with axis ratios 1:0.75:0.70. The major axis of the halo is consistent with a tilt of 18° above the Galactic plane in the direction of the Sun. The magnitude and direction of the tilt are consistent with measurements of the stellar halo from Gaia and the Hectochelle in the Halo at High Resolution survey. A tilted triaxial halo has important consequences for orbit-integration-based studies of the Galaxy and can be further tested by deriving acceleration constraints from multiple streams.