Dark Matter Halos In The N-body Simulations For Interacting Dark Energy Models:Formation History,Density Profile,Spin And Shape

The interacting dark energy(IDE)model,which considers the interactions between dark energy and dark matter,is regarded as one of well-motivated and promising nonstandard cosmological scenarios.It provides a natural mechanism to alleviate the coincidence problem,and with appropriate interacting parameters it can also relieve the H0 tension to some extent.Previous studies have put preliminary constraints to IDE models by cosmic microwave background,baryon acoustic oscillations,type la supernova and Hubble parameter observations,but these data are not yet enough to distinguish IDE models from the standard cosmological constant-cold dark matter(ACDM)model effectively.Because the non-linear evolution of large-scale structures contains rich cosmological probes,it is expected that the non-linear structures can provide tighter constraints to IDE models.In this work,based on a set of state-of-art,fully self-consistent N-body simulations for IDE models,we systematically investigate the formation histories and properties of dark matter halos in IDE models,and analyse the differences with their ACDM counterparts.Our results do not support the model of dark matter decaying to be dark energy,IDEl,in which the cosmic structure formation is markedly slowed down,and the dark matter halos have systematically lower mass,shallower internal potential,higher spin and anisotropy.Moreover,we find that within the considered parameter range,the halo concentration parameter of IDE is proportional to that of ACDM,and the ratio depends on the IDE interacting parameter and is independent of halo mass.This can act as a powerful probe to constrain IDE models.Our results concretely demonstrate how the interactions between dark energy and dark matter affect the structure formation,and therefore the constraints from non-linear structures are indispensable.