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Testing ΛCDM with Dwarf Galaxy Morphology
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DOI：10.3847/1538-4357/aba51f.png)
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Abstract
En 中文
The leading tensions to the collisionless cold dark matter (CDM) paradigm are the small-scale controversies, discrepancies between observations at the dwarf-galactic scale, and their simulational counterparts. In this work we consider methods to infer 3D morphological information on Local Group dwarf spheroidals and test the fitness of CDM+hydrodynamics simulations to the observed galaxy shapes. We find that the subpopulation of dwarf galaxies with mass-to-light ratio greater than or similar to 100M(circle dot)/L-circle dot reflects an oblate morphology. This is discrepant with the dwarf galaxies with mass-to-light ratios less than or similar to 100M(circle dot)/L-circle dot, which reflect prolate morphologies, as well as simulations of CDM-sourced bright isolated galaxies that are explicitly prolate. Although more simulations and data are called for if evidence of oblate pressure-supported stellar distributions persists in observed galaxies while being absent from simulations, we argue that an underlying oblate non-CDM dark matter halo may be required and present this as motivation for future studies.
Keywords:
MILKY-WAY SATELLITES
LOCAL GROUP
MATTER
KINEMATICS
FORNAX