English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Recently, in [1] we developed a parametric reconstruction method to ahomogeneous, isotropic and spatially flat Friedmann-Robertson-Walker (FRW)cosmological model filled of a fluid of dark energy (DE) with constant equationof state (EOS) parameter interacting with dark matter (DM). The reconstructionmethod is based on expansions of the general interaction term and the relevantcosmological variables in terms of Chebyshev polynomials which form a completeset orthonormal functions. In this article, we reconstruct the interactionfunction expanding it in terms of only the first four Chebyshev polynomials andobtain the best estimation for the coefficients of the expansion assuming threemodels: (a) a DE equation of the state parameter w=-1 (an interactingcosmological Lambda), (b) a DE equation of the state parameter w = constantwith a dark matter density parameter fixed, (c) a DE equation of the stateparameter w = constant with a free constant dark matter density parameter to beestimated. In all the cases, the preliminary reconstruction shows that in thebest scenario there exist the possibility of a crossing of the noninteractingline Q=0 in the recent past within the 1-sigma and 2-sigma errors from positivevalues at early times to negative values at late times. This means that, inthis reconstruction, there is an energy transfer from DE to DM at early timesand an energy transfer from DM to DE at late times. We conclude that this factis an indication of the possible existence of a crossing behavior in a generalinteraction coupling between dark components. Finally, we conclude that in thisscenario, the observations put strong constraints on the strength of theinteraction so that its magnitude can not solve the coincidence problem or atleast alleviate significantly.

Reconstruction of the interaction term between dark matter and dark energy using SNe Ia, BAO, CMB, H(z) and X-ray gas mass fraction