Unified dark matter: constraints from galaxies and clusters

TL;DR

This paper investigates the nonlinear behavior of unified dark matter models in galaxies and clusters, showing that pressure gradients significantly affect halo properties and constraining model parameters to match observations.

Contribution

It provides new constraints on the equation of state parameters of unified dark matter models based on nonlinear halo dynamics and pressure gradient effects.

Findings

Pressure gradients prevent flat rotation curves in unified dark matter models.

Constraints on the Chaplygin gas parameter alpha are very tight, requiring alpha to be near zero or very large.

Unified dark matter must have negligible pressure gradients at halo densities to mimic observed structures.

Abstract

Unified dark matter models are appealing in that they describe the dark sector in terms of a single component. They however face problems when attempting to account for structure formation: in the linear regime, density fluctuations can become Jeans stable and oscillate rather than collapse, though it is possible that this difficulty may be circumvented by invoking nonlinear clustering. Here we examine the behaviour in the fully nonlinear regime, of collapsed objects that should mimic standard dark matter haloes. It is shown that the pressure gradient associated with the unified dark matter fluid should be significant in the outer parts of galaxies and clusters, and its effects obervable. In this case, no flat or falling rotation curve is possible for any (barotropic) equation of state with associated sound speed decreasing with density (a necessary condition if the fluid is to behave as pressureless matter at high density). The associated density profile is therefore also incompatible with that inferred in the outer part of clusters. For the prototypical case of the generalised Chaplygin gas, it is shown that this limits the values of the equation of state index $\alpha$ that are compatible with observations to $\alpha \la 0.0001$ or $\alpha \ga 2$. This is in line from what is deduced from linear analysis. More generally, from the expected properties of dark matter haloes, constraints on the sound speed are derived. For the particular case of the generalised Chaplygin gas, this further constrains the index to $\alpha \la 10^{-9}$ or $\alpha \ga 6.7$. For a unified dark matter fluid to mimic dark halo properties, therefore, it needs to have an equation of state such that the pressure gradients are either minimal or which decrease fast enough so as to be negligible at densities characteristic of the outer parts of haloes.