An Empirical Response Law for Galaxy and Dwarf Dynamics
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2026
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| _version_ | 1866901830445826048 |
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| author | Macke, Eugen |
| author_facet | Macke, Eugen |
| contents | <p>A compact empirical response framework is introduced to organize late-time weak-field dynamics5<br>across rotation-supported galaxies and pressure-supported dwarfs. The method is based on radius-6<br>local inversion of co-located tuples of enclosed baryonic mass, characteristic radius, and observed7<br>circular velocity, yielding an empirical response coefficient that can be compared across systems and8<br>dynamical regimes.9<br>Within the rotation-supported calibration domain, the inferred coefficients populate a tight inverse-10<br>mass ridge over approximately five decades in enclosed baryonic mass, including an independent halo-11<br>scale galaxy–galaxy lensing and satellite-kinematics cross-check at ∼ 200 kpc. The ridge exhibits finite12<br>but structured scatter rather than exact constancy. Extending the same tuple-plane diagnostic to13<br>pressure-supported dwarfs evaluated at their half-light radius increases the dynamic range to more14<br>than eight decades in mass and reveals systematic regime-dependent deviations.15<br>Unlike a universal single-valued radial acceleration relation, the primary empirical benchmark16<br>adopted here is the stability and structured scatter of the tuple-plane ridge across radii, tracers,17<br>and dynamical states. The formulation is explicitly empirical and agnostic with respect to microscopic18<br>interpretation and defines falsification criteria based on slope stability, normalization drift, radial co-19<br>herence, and cross-channel consistency.</p> |
| format | Recurso digital |
| id | zenodo_https___doi_org_10_5281_zenodo_19388493 |
| institution | Zenodo |
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| publishDate | 2026 |
| publisher | Zenodo |
| record_format | zenodo |
| spellingShingle | An Empirical Response Law for Galaxy and Dwarf Dynamics Macke, Eugen galaxy rotation RAR dwarf dynamics galaxy dynamics <p>A compact empirical response framework is introduced to organize late-time weak-field dynamics5<br>across rotation-supported galaxies and pressure-supported dwarfs. The method is based on radius-6<br>local inversion of co-located tuples of enclosed baryonic mass, characteristic radius, and observed7<br>circular velocity, yielding an empirical response coefficient that can be compared across systems and8<br>dynamical regimes.9<br>Within the rotation-supported calibration domain, the inferred coefficients populate a tight inverse-10<br>mass ridge over approximately five decades in enclosed baryonic mass, including an independent halo-11<br>scale galaxy–galaxy lensing and satellite-kinematics cross-check at ∼ 200 kpc. The ridge exhibits finite12<br>but structured scatter rather than exact constancy. Extending the same tuple-plane diagnostic to13<br>pressure-supported dwarfs evaluated at their half-light radius increases the dynamic range to more14<br>than eight decades in mass and reveals systematic regime-dependent deviations.15<br>Unlike a universal single-valued radial acceleration relation, the primary empirical benchmark16<br>adopted here is the stability and structured scatter of the tuple-plane ridge across radii, tracers,17<br>and dynamical states. The formulation is explicitly empirical and agnostic with respect to microscopic18<br>interpretation and defines falsification criteria based on slope stability, normalization drift, radial co-19<br>herence, and cross-channel consistency.</p> |
| title | An Empirical Response Law for Galaxy and Dwarf Dynamics |
| topic | galaxy rotation RAR dwarf dynamics galaxy dynamics |
| url | https://doi.org/10.5281/zenodo.19388493 |