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Determining the Milky Way Gravitational Potential Without Selection Functions

  • Authors: Taavet Kalda, Gregory M. Green

Taavet Kalda and Gregory M. Green 2026 The Astrophysical Journal Letters 1002 .

  • Provider: AAS Journals

Caption: Figure 3.

Recovery of the selection function and true spatial density of tracers by the “selection function” and “conditional” methods, respectively, in a two-dimensional slice through the xy plane (at z = 0). Top row: the recovered selection function (left), true selection function (middle), and residuals (right) for the “selection function” method. Bottom row: the recovered true spatial density of tracers (left), true spatial density of tracers (middle), and residuals (right) for the “conditional” method. Dust imprints fine angular structure on the selection function, necessitating much larger models (∼1.4 million parameters in this case) than are needed to capture the much smoother true spatial density of tracers (∼47,000 parameters). As seen in the top right panel, the selection function residuals appear as long radial spurs, illustrating the difficulty of recovering the angular structures in ﹩S\left({\boldsymbol{x}}\right)﹩.

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