# Hydrodynamical simulations of galaxy clusters in dark energy cosmologies: I. general properties - Astrophysics > Cosmology and Nongalactic Astrophysics

Hydrodynamical simulations of galaxy clusters in dark energy cosmologies: I. general properties - Astrophysics > Cosmology and Nongalactic Astrophysics - Descarga este documento en PDF. Documentación en PDF para descargar gratis. Disponible también para leer online.

Abstract: We investigate the influence of dark energy on structure formation, withinfive different cosmological models, namely a concordance $\Lambda$CDM model,two models with dynamical dark energy, viewed as a quintessence scalar fieldusing a RP and a SUGRA potential form and two extended quintessence modelsEQp and EQn where the quintessence scalar field interacts non-minimally withgravity scalar-tensor theories. We adopted for all models the normalizationof the matter power spectrum $\sigma {8}$ to match the CMB data. In the modelswith dynamical dark energy and quintessence, we describe the equation of statewith $w 0\approx-0.9$, still within the range allowed by observations. For eachmodel, we have performed hydrodynamical simulations in a cosmological box of$300 \ { m{Mpc}} \ h^{-1}^{3}$ including baryons and allowing for coolingand star formation. The contemporary presence of evolving dark energy andbaryon physics allows us to investigate the interplay between the differentbackground cosmology and the evolution of the luminous matter. Since clusterbaryon fraction can be used to constrain other cosmological parameters such as$\Omega {m}$, we also analyse how dark energy influences the baryon content ofgalaxy clusters. We find that, in models with dynamical dark energy, theevolving cosmological background leads to different star formation rates anddifferent formation histories of galaxy clusters, but the baryon physics is notaffected in a relevant way. We investigate several proxies of the cluster massfunction based on X-ray observables like temperature, luminosity, $M {gas}$,and $Y {gas}$. We conclude that the X-ray temperature and $M {gas}$ functionsare better diagnostic to disentangle the growth of structures among differentdark energy models. Abridged

Autor: Cristiano De Boni, Klaus Dolag, Stefano Ettori, Lauro Moscardini, Valeria Pettorino, Carlo Baccigalupi

Fuente: https://arxiv.org/