Differentiating dark interactions with perturbation. (arXiv:2101.08959v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Sinha_S/0/1/0/all/0/1">Srijita Sinha</a>
A cosmological model with an energy transfer between the dark matter (DM) and
dark energy (DE) can give rise to comparable energy densities at the present
epoch. The present work deals with the perturbation analysis, parameter
estimation and Bayesian evidence calculation of interacting models with
dynamical coupling parameter that determines the strength of the interaction.
We have considered two cases, where the interaction is a more recent phenomenon
and where the interaction is a phenomenon in the distant past. Moreover, we
have considered the quintessence DE equation of state with
Chevallier-Polarski-Linder (CPL) parametrisation and energy flow from DM to DE.
Using the current observational datasets like the cosmic microwave background
(CMB), baryon acoustic oscillation (BAO), Type Ia Supernovae (SNe Ia) and
redshift-space distortions (RSD), we have estimated the mean values of the
parameters. Using the perturbation analysis and Bayesian evidence calculation,
we have shown that interaction present as a brief early phenomenon is preferred
over a recent interaction.
A cosmological model with an energy transfer between the dark matter (DM) and
dark energy (DE) can give rise to comparable energy densities at the present
epoch. The present work deals with the perturbation analysis, parameter
estimation and Bayesian evidence calculation of interacting models with
dynamical coupling parameter that determines the strength of the interaction.
We have considered two cases, where the interaction is a more recent phenomenon
and where the interaction is a phenomenon in the distant past. Moreover, we
have considered the quintessence DE equation of state with
Chevallier-Polarski-Linder (CPL) parametrisation and energy flow from DM to DE.
Using the current observational datasets like the cosmic microwave background
(CMB), baryon acoustic oscillation (BAO), Type Ia Supernovae (SNe Ia) and
redshift-space distortions (RSD), we have estimated the mean values of the
parameters. Using the perturbation analysis and Bayesian evidence calculation,
we have shown that interaction present as a brief early phenomenon is preferred
over a recent interaction.
http://arxiv.org/icons/sfx.gif
