Remedy of some cosmological tensions via effective phantom-like behavior of interacting vacuum energy

Cosmology Intertwined: A Review of the Particle Physics, Astrophysics, and Cosmology Associated with the Cosmological Tensions and Anomalies

“…Among the variety of cosmological models (in alphabetical order) presented below, some of them have been proposed by many researchers to either alleviate or solve the S 8 tension C. Addressing Both the H0 and S8 Tensions Thus, looking for a cosmological model accommodating both the tensions is not a cup of tea. Nevertheless, curious minds never stop at any point and as a result it has been argued that in some extended cosmological models beyond ΛCDM, one can simultaneously tackle this problem [552][553][554][555][556][557][558][559]. However, even though we have a series of alternative possibilities beyond the standard ΛCDM model, we are still left with some vital issues that are usually overlooked while discussing the simultaneous solutions to both the tensions.…”

“…A cosmological scenario in which dark matter (DM) and DE share interactions other than gravitational leads to various interesting features [237,553,554,556,. In Ref.…”

“…In Ref. [553,554,556,824,[828][829][830][831][832], the authors have found that the IDE model can solve the tension with SH0ES within one standard deviation, leading to a preference for a non-zero DE-DM coupling at more than 5 standard deviations, while fixing the DE EoS to a cosmological constant. However, this category can be further extended into two classes [554]: (i) models with w DE < −1 in which energy flows from DE to DM, (ii) models with w DE > −1 in which energy flows from DM to DE.…”

“…For instance, one viable possibility to largely reduce the significance of the tension S 8 is to allow for DE-DM interactions in a scenario where the DE energy density can be transferred to the DM fluid via a coupling function proportional to the DE energy density itself (unlike the model able to address the H 0 tension, where the energy transfer is from the DM to the DE) [554,848] (see also [553,555,556]. Indeed, in this scenario, because of the additional energy flow from the DE to the DM over the cosmic history, a lower DM energy density with respect to the ΛCDM model is allowed at recombination without a sizable effect on the shape of the CMB anisotropy power spectra.…”

Cosmological direct detection of dark energy: non-linear structure formation signatures of dark energy scattering with visible matter

“…Dutta et al 2020;Calderón et al 2021;Bonilla et al 2021;Acquaviva et al 2021;Akarsu et al 2021;Sen et al 2021). 2 For examples of important works on theoretical and observational aspects of coupled DE, see for instance Wetterich (1995); Amendola (2000); Mangano et al (2003); Farrar & Peebles (2004); Barrow & Clifton (2006); Pettorino & Baccigalupi (2008); Valiviita et al (2008); Gavela et al (2009); Clemson et al (2012); Nunes & Barboza (2014); Benisty & Guendelman (2017); Kumar & Nunes (2017b); Yang et al (2017Yang et al ( , 2018a; Martinelli et al (2019); Kumar et al (2019); Yang et al (2019a,c); Benetti et al (2019); Di Valentino et al (2020); Lucca & Hooper (2020); Hogg et al (2020); Gómez-Valent et al (2020); Gao et al (2021); Zhang et al (2021); Benetti et al (2021); Kumar (2021); Lucca (2021a,b).…”