Does Chaplygin gas have salvation?

TL;DR

This paper examines the viability of the generalized Chaplygin gas as a unification model for dark matter and dark energy, analyzing observational data, addressing theoretical issues, and comparing with the standard DM model.

Contribution

It provides observational constraints on the parameter nd explores modifications in gravity and scalar field formulations to resolve theoretical challenges.

Findings

Favours negative t 85% confidence level.

Negative orresponds to negative sound speed squared, problematic for structure formation.

Perturbation evolution differs from DM, affecting halo formation.

Abstract

We investigate the unification scenario provided by the generalised Chaplygin gas model (a perfect fluid characterized by an equation of state p = -A/\rho^{\alpha}). Our concerns lie with a possible tension existing between background kinematic tests and those related to the evolution of small perturbations. We analyse data from the observation of the differential age of the universe, type Ia supernovae, baryon acoustic oscillations and the position of the first peak of the angular spectrum of the cosmic background radiation. We show that these tests favour negative values of the parameter \alpha: we find \alpha = - 0.089^{+0.161}_{-0.128} at the 2\sigma\ level and that \alpha < 0 with 85% confidence. These would correspond to negative values of the square speed of sound which are unacceptable from the point of view of structure formation. We discuss a possible solution to this problem, when the generalised Chaplygin gas is framed in the modified theory of gravity proposed by Rastall. We show that a fluid description within this theory does not serve the purpose, but it is necessary to frame the generalised Chaplygin gas in a scalar field theory. Finally, we address the standard general relativistic unification picture provided by the generalised Chaplygin gas in the case \alpha = 0: this is usually considered to be undistinguishable from the standard \Lambda CDM model, but we show that the evolution of small perturbations, governed by the M\'esz\'aros equation, is indeed different and the formation of sub-horizon GCG matter halos may be importantly affected in comparison with the \Lambda CDM scenario.