Relate equilibrium mass to independent dwarf-galaxy properties

Investigate whether the per-galaxy equilibrium mass correlates with independent galaxy properties such as central density, core radius, or orbital pericenter in order to distinguish genuine astrophysical variation from a common origin.

Background

The method yields different effective equilibrium masses for the nine dwarf spheroidal galaxies. The paper emphasizes that these values are not necessarily samples of a single population parameter because the estimator measures the mass required for each observed density and mass profile to satisfy local static equilibrium.

A correlation with independent structural or orbital properties could clarify whether the galaxy-to-galaxy spread reflects real astrophysical variation, for example differences in tidal perturbations, or instead arises from a common systematic or methodological origin.

References

A natural extension of this work, which we defer to future study, is to test for a correlation between the per-galaxy equilibrium mass and independent galaxy properties (e.g., central density, core radius, or orbital pericenter, which sets the strength of Milky-Way tidal perturbation), which could help distinguish genuine astrophysical variation from a common origin.

— Hydrostatic Equilibrium Constraints on the Fuzzy Dark Matter Mass from Dwarf Spheroidals: Method, Systematics, and Robustness  (2610.21722 - Mitra et al., 15 Oct 2026) in Section 7, final paragraph