New observational constraints on interacting dark energy using galaxy clusters virial equilibrium states

Abstract

As the dark sector remains unknown in composition and interaction between dark energy and dark matter stand out as natural, observations of galaxy clusters out of equilibrium abound, opening a promising window on these questions. We continue here the exploration of dark sector interaction detection via clusters virial equilibrium state for all clusters configurations. The dynamics of clusters is evaluated with the Layzer-Irvine equation, a simple model of an interacting dark sector and some simplifying assumptions to obtain the time-dependent part of the virial dynamics. The clusters' data are concentrated in optical weak lensing and X-ray observations that evaluate, respectively, the clusters' mass profiles and temperatures. The global inconsistency of available X-ray data led us to constitute "gold" cluster samples. Through a Bayesian analysis, they are processed to obtain consistent interaction detected up to 3σ, in compounded interaction strength for 11 clusters at −0.027 ± 0.009 that translate in compounded universal equilibrium virial ratio of −0.61 +0.04 −0.03 . The level of detection and inconsistency of X-ray data call for caution, although future instruments promise a clearer detection soon.

Bounds from multi-messenger astronomy on the Super Heavy Dark Matter

“…More recently, dark sector interactions have been given more serious consideration, which viability has been scrutinized in Comelli et al [37]. Observational effects on galaxy clusters dynamics of such interactions have gathered credibility [38][39][40][41][42][43][44][45][46]. However, most of the current constraints tend to favour stable or long-lived, cold or warm, non-baryonic DM [47].…”

Logarithmic corrections to Newtonian gravity and large scale structure

“…These effects can be investigated using model of interacting dark matter and dark energy [24,25]. It is also possible to constrain the dark energy from the clustering of galaxies [29]. The cosmic expansion can also change the dynamics at the scale of galaxy clusters [30].…”