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The Milky Way Stellar Halo Is Twisted and Doubly Broken: Insights from DESI DR2 Milky Way Survey Observation

  • Authors: Songting Li, Wenting Wang, Sergey E. Koposov, João A. S. Amarante, Alis J. Deason, Nathan R. Sandford, Ting S. Li, Gustavo E. Medina, Jiaxin Han, Monica Valluri, Oleg Y. Gnedin, Namitha Kizhuprakkat, Andrew P. Cooper, Leandro Beraldo e Silva, Carlos Frenk, Raymond G. Carlberg, Mika Lambert, Tian Qiu, Jessica Nicole Aguilar, Steven Ahlen, Davide Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Dick Joyce, Robert Kehoe, Anthony Kremin, Claire Lamman, Martin Landriau, Laurent Le Guillou, Ramon Miquel, Will Percival, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Ray Sharples, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Hu Zou

Songting Li et al 2026 The Astrophysical Journal 999 .

  • Provider: AAS Journals

Caption: Figure 15.

The black solid line refers to the selection-effect-free density profile based on a mock realization (ideal profile) of stars. The green line is the selection-effect-free best-fit model for the ideal profile perturbed with observational error. The green shaded region shows the statistical uncertainties of the best-fit model. The vertical dashed lines stand for the break radii of the original profile (black) and the recovered profile (green) after perturbation. Both profiles are renormalized to unity.

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