An estimate of the dark matter density from galaxy clusters and supernovae data

Understand

In this paper, we discuss a model-independent way to obtain the present dark matter density parameter ($\Omega_{\rm{c,0}}$) by combining gas mass fraction measurements in galaxy clusters ($f_{gas}$), type Ia supernovae (SNe Ia) observations and measurements of the cosmic baryon abundance from observations of absorption systems at high redshifts.

• Our estimate is $\Omega_{\rm{c,0}} = 0.244 \pm 0.013$ ($1\sigma$).
• By considering the latest local measurement of the Hubble constant, we obtain $\Omega_{\rm{M,0}} = 0.285 \pm 0.013$ ($1\sigma$) for the total matter density parameter.
• We also investigate departures of the evolution of the dark matter density with respect to the usual $a^{-3}$ scaling, as usual in interacting models of dark matter and dark energy.