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Warm Dark Matter Constraints Using Milky-Way Satellite Observations and Subhalo Evolution Modeling
Ariane Dekker, Shin'ichiro Ando, Camila A. Correa, Kenny C. Y. Ng
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Warm dark matter (WDM) can potentially explain small-scale observations that currently challenge the cold dark matter (CDM) model, as warm particles suppress structure formation due to free-streaming effects. Observing small-scale matter distribution provides a valuable way to distinguish between CDM and WDM. In this work, we use observations from the Dark Energy Survey and PanSTARRS1, which observe 270 Milky-Way satellites after completeness corrections. We test WDM models by comparing the number of satellites in the Milky Way with predictions derived from the Semi-Analytical SubHalo Inference ModelIng (SASHIMI) code, which we develop based on the extended Press-Schechter formalism and subhalos' tidal evolution prescription. We robustly rule out WDM with masses lighter than 4.4 keV at 95% confidence level for the Milky-Way halo mass of 10¹² M_⊙. The limits are a weak function of the (yet uncertain) Milky-Way halo mass, and vary as m_(WDM)>3.6-5.1 keV for (0.6-2.0) ×10¹² M_⊙. For the sterile neutrinos that form a subclass of WDM, we obtain the constraints of m_(νₛ)>11.6 keV for the Milky-Way halo mass of 10¹² M_⊙. These results based on SASHIMI do not rely on any assumptions of galaxy formation physics or are not limited by numerical resolution. The models, therefore, offer a robust and fast way to constrain the WDM models. By applying a satellite forming condition, however, we can rule out the WDM mass lighter than 9.0 keV for the Milky-Way halo mass of 10¹² M_⊙.
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