Beyond compactness:. A structural--dynamical--evolutionary manifold for the stellar-to-dynamical mass ratio in ultra-compact massive galaxies

March 30, 2026Open Access

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Key Points

This research aims to understand how compactness and star formation histories affect the stellar-to-dynamical mass ratio in ultra-compact massive galaxies (UCMGs).
Analyzed a homogeneous catalogue of 482 UCMGs with internal kinematics and stellar population properties.
Derived the compactness–mass relation while assuming a constant virial coefficient (K=5).
Corrected stellar masses for initial mass function variations and recomputed mass ratios using an empirical virial coefficient.
Tested the influence of stellar kinematics and population properties, particularly the degree of relicness (DoR).
Found an anti-correlation between compactness and IMF-corrected stellar-to-dynamical mass ratio using a constant virial coefficient.
Velocity dispersion was identified as the primary factor influencing the stellar-to-dynamical mass ratio, explaining 62% of the variance.
Increased variance explained to 63% when stellar age was included, indicating the importance of evolutionary factors.

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Explores factors influencing mass ratios in ultra-compact massive galaxies, suggesting new insights into galaxy formation.

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C. Spiniello (2026) studied this question.

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