Modified Dark Matter: Relating Dark Energy, Dark Matter and Baryonic Matter

Abstract

Modified dark matter (MDM) is a phenomenological model of dark matter, inspired by gravitational thermodynamics. For an accelerating Universe with positive cosmological constant ($\Lambda$), such phenomenological considerations lead to the emergence of a critical acceleration parameter related to $\Lambda$. Such a critical acceleration is an effective phenomenological manifestation of MDM, and it is found in correlations between dark matter and baryonic matter in galaxy rotation curves. The resulting MDM mass profiles, which are sensitive to $\Lambda$, are consistent with observational data at both the galactic and cluster scales. In particular, the same critical acceleration appears both in the galactic and cluster data fits based on MDM. Furthermore, using some robust qualitative arguments, MDM appears to work well on cosmological scales, even though quantitative studies are still lacking. Finally, we comment on certain non-local aspects of the quanta of modified dark matter, which may lead to novel non-particle phenomenology and which may explain why, so far, dark matter detection experiments have failed to detect dark matter particles.

References in corpus (24)

• Wilkinson Microwave Anisotropy Probe (WMAP) Three Year Results: Implications for Cosmology
• The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
• A direct empirical proof of the existence of dark matter
• Too big to fail? The puzzling darkness of massive Milky Way subhaloes
• Limits on the Macho Content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds
• Echoes of a Hidden Valley at Hadron Colliders
• The Radial Acceleration Relation in Rotationally Supported Galaxies
• Hundreds of Milky Way Satellites? Luminosity Bias in the Satellite Luminosity Function
• High-resolution mass models of dwarf galaxies from LITTLE THINGS
• One Law To Rule Them All: The Radial Acceleration Relation of Galaxies
• Is there a "too big to fail" problem in the field?
• Galaxies as simple dynamical systems: observational data disfavor dark matter and stochastic star formation
• The spatial distribution of the Milky Way and Andromeda satellite galaxies
• The baryon fraction of LambdaCDM haloes
• A Tale of Two Paradigms: the Mutual Incommensurability of LCDM and MOND
• Can MOND take a bullet? Analytical comparisons of three versions of MOND beyond spherical symmetry
• M31 Satellite Masses Compared to LCDM Subhaloes
• A thousand shadows of Andromeda: rotating planes of satellites in the Millennium-II cosmological simulation
• Gravitational polarization and the phenomenology of MOND
• An Alternative to Particle Dark Matter
• Quantum Gravity, Dynamical Phase Space and String Theory
• Rings and shells of "dark matter" as MOND artifacts
• Vast planes of satellites in a high resolution simulation of the Local Group: comparison to Andromeda
• Finslerian MOND vs. observations of Bullet Cluster 1E0657-558

Cited by in corpus (14)

• Phenomenological consequences of superfluid dark matter with baryon-phonon coupling
• Emergence of the mass discrepancy-acceleration relation from dark matter-baryon interactions
• Yet another test of Radial Acceleration Relation for galaxy clusters
• A first attempt to differentiate between modified gravity and modified inertia with galaxy rotation curves
• On de Sitter Spacetime and String Theory
• Baryon-Interacting Dark Matter: heating dark matter and the emergence of galaxy scaling relations
• Scaling relations for dark matter core density and radius from Chandra X-ray cluster sample
• Quantum gravity phenomenology at the dawn of the multi-messenger era -- A review
• Bound on the graviton mass from Chandra X-ray cluster sample
• Galaxy cluster hydrostatic masses using Tolman-Oppenheimer-Volkoff equation
• On Dark Energy and Quantum Gravity
• Entropy and Gravitation: From Black Hole Computers to Dark Energy and Dark Matter
• A Toy Model for the Dynamical Discrepancies on Galactic Scales
• The $\mu$-deformed Einstein field equations with $\mu$-dependent effective cosmological constant