Bayesian Comparison of the Cosmic Duality Scenarios. (arXiv:2005.04131v3 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Silva_W/0/1/0/all/0/1">W. J. C. da Silva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holanda_R/0/1/0/all/0/1">R. F. L. Holanda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silva_R/0/1/0/all/0/1">R. Silva</a>
The cosmic distance duality relation (CDDR), $D_{rm L}(1+z)^{-2}/D_{rm
A}=eta=1$, with $D_{rm L}$ and $D_{rm A}$, being the luminosity and angular
diameter distances, respectively, is a crucial premise in cosmological
scenarios. Many investigations try to test CDDR through observational
approaches, even some of these ones also consider a deformed CDDR, i.e.,
$eta=eta(z)$. In this paper, we use type Ia supernovae luminosity distances
and galaxy cluster measurements (their angular diameter distances and gas mass
fractions) in order to perform a Bayesian model comparison between $ eta(z) $
functions. We show that the data here used are unable to pinpoint, with a high
degree of Bayesian evidence, which $eta(z)$ function best captures the
evolution of CDDR.
The cosmic distance duality relation (CDDR), $D_{rm L}(1+z)^{-2}/D_{rm
A}=eta=1$, with $D_{rm L}$ and $D_{rm A}$, being the luminosity and angular
diameter distances, respectively, is a crucial premise in cosmological
scenarios. Many investigations try to test CDDR through observational
approaches, even some of these ones also consider a deformed CDDR, i.e.,
$eta=eta(z)$. In this paper, we use type Ia supernovae luminosity distances
and galaxy cluster measurements (their angular diameter distances and gas mass
fractions) in order to perform a Bayesian model comparison between $ eta(z) $
functions. We show that the data here used are unable to pinpoint, with a high
degree of Bayesian evidence, which $eta(z)$ function best captures the
evolution of CDDR.
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