![]() ![]() P lanck collaboration, Planck 2018 results. P lanck collaboration, Planck 2015 results. WMAP collaboration, Nine-year Wilkinson Microwave Anisotropy Probe (WMAP) observations: final maps and results, Astrophys. ![]() ![]() Xu et al., Cosmological investigation of multi-frequency VLBI observations of ultra-compact structure in z ∼ 3 radio quasars, Eur. Zhu, Ultra-compact structure in intermediate-luminosity radio quasars: building a sample of standard cosmological rulers and improving the dark energy constraints up to z ∼ 3, Astron. Zhu, Cosmic equation of state from combined angular diameter distances: Does the tension with luminosity distances exist?, Phys. Zhu, A multi-wavelength study of the gravitational lens COSMOS J095930 023427, Res. S upernova C osmology P roject collaboration, Measurements of Ω and Λ from 42 high redshift supernovae, Astrophys. S upernova S earch T eam collaboration, Observational evidence from supernovae for an accelerating universe and a cosmological constant, Astron. Clowe et al., A direct empirical proof of the existence of dark matter, Astrophys. White, The evolution of large scale structure in a universe dominated by cold dark matter, Astrophys. Rees, Formation of galaxies and large scale structure with cold dark matter, Nature 311 (1984) 517. Therefore, one could expect more stringent constraints on the WMIP DM models, with the accumulation of more accurate cosmological observations in the near future. Those two cosmological observations lead to an almost paradoxical conclusion. After further considering the constraints from DM direct detection experiment, DM indirect detection experiment, and DM relic density, we find that the allowed parameter space of the scalar DM model will be completely excluded for the former cosmological observations, while it will increase for the latter ones. As for DM relic density, it will be magnified by \( \frac \) and γ DM = −0. Meanwhile, our numerical calculation also indicates that x f ≈ 20 is associated with DM freeze-out temperature, which is the same as the vanishing interaction scenario. In general, the coupling strength γ DE is close to 0 as the interaction between DE and WIMP DM is very weak, thus the effect of γ DE on the evolution of Y associated with DM energy density can be safely neglected. In this paper, we investigate the possibility of testing the weakly interacting massive particle (WIMP) dark matter (DM) models by applying the simplest phenomenological model which introduces an interaction term between dark energy (DE) and WIMP DM, i.e., Q = 3 γ DM Hρ DM. ![]()
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