In a decaying dark matter plus semi-cosmographic dark energy cosmology constrained by DESI BAO and ShapeFit, the spherical collapse threshold stays close to the ΛCDM value while massive halo abundance shows pronounced deviations that enable joint constraints on DDM lifetime and dark energy parameter
Cluster Abundance Constraints on Quintessence Models
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abstract
The abundance of rich clusters is a strong constraint on the mass power spectrum. The current constraint can be expressed in the form $\sigma_8 \Omega_m^{\gamma} = 0.5 \pm 0.1$ where $\sigma_8$ is the $rms$ mass fluctuation on 8 $h^{-1}$ Mpc scales, $\Omega_m$ is the ratio of matter density to the critical density, and $\gamma$ is model-dependent. In this paper, we determine a general expression for $\gamma$ that applies to any models with a mixture of cold dark matter plus cosmological constant or quintessence (a time-evolving, spatially-inhomogeneous component with negative pressure) including dependence on the spectral index $n$, the Hubble constant $h$, and the equation-of-state of the quintessence component $w$. The cluster constraint is combined with COBE measurements to identify a spectrum of best-fitting models. The constraint from the evolution of rich clusters is also discussed.
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Spherical Collapse and Halo Formation in a Cosmology with Decaying Dark Matter and a Semi-Cosmographic Dark Energy
In a decaying dark matter plus semi-cosmographic dark energy cosmology constrained by DESI BAO and ShapeFit, the spherical collapse threshold stays close to the ΛCDM value while massive halo abundance shows pronounced deviations that enable joint constraints on DDM lifetime and dark energy parameter
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