Tully-Fisher relation, key to dark matter companion of baryonic matter

TL;DR

This paper models galaxy rotation curves and the Tully-Fisher relation by proposing a dark fluid companion, deriving its properties from gravitational effects and galaxy mass, offering a new perspective on dark matter distribution.

Contribution

It introduces a spherically symmetric spacetime model with a dark fluid companion that explains galaxy rotation curves and the Tully-Fisher relation, linking dark matter properties to observable baryonic matter.

Findings

Dark density proportional to the square root of galaxy mass

Dark matter density falls off as r^{-(2+α)} with α << 1

Formalism accounts for nonlinear, nonlocal dark matter effects

Abstract

Rotation curves of spiral galaxies \emph{i}) fall off much less steeply than the Keplerian curves do, and \emph{ii}) have asymptotic speeds almost proportional to the fourth root of the mass of the galaxy, the Tully-Fisher relation. These features alone are sufficient for assigning a dark companion to the galaxy in an unambiguous way. In regions outside a spherical system, we design a spherically symmetric spacetime to accommodate the peculiarities just mentioned. Gravitation emerges in excess of what the observable matter can produce. We attribute the excess gravitation to a hypothetical, dark, perfect fluid companion to the galaxy and resort to the Tully-Fisher relation to deduce its density and pressure. The dark density turns out to be proportional to the square root of the mass of the galaxy and to fall off as $r^{-(2+\alpha)}, \alpha\ll 1$. The dark equation of state is barrotropic. For the interior of the configuration, we require the continuity of the total force field at the boundary of the system. This enables us to determine the size and the distribution of the interior dark density and pressure in terms of the structure of the observable matter. The formalism is nonlocal and nonlinear, and the density and pressure of the dark matter at any spacetime point turn out to depend on certain integrals of the baryonic matter over all or parts of the system in a nonlinear manner.