Observational constraints on Myrzakulov gravity. (arXiv:2012.06524v2 [gr-qc] UPDATED)
<a href="http://arxiv.org/find/gr-qc/1/au:+Anagnostopoulos_F/0/1/0/all/0/1">Fotios K. Anagnostopoulos</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Basilakos_S/0/1/0/all/0/1">Spyros Basilakos</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Saridakis_E/0/1/0/all/0/1">Emmanuel N. Saridakis</a>
We use data from Supernovae (SNIa) Pantheon sample, from Baryonic Acoustic
Oscillations (BAO), and from cosmic chronometers measurements of the Hubble
parameter (CC), alongside arguments from Big Bang Nucleosynthesis (BBN), in
order to extract constraints on Myrzakulov $F(R,T)$ gravity. This is a
connection-based theory belonging to the Riemann-Cartan subclass, that uses a
specific but non-special connection, which then leads to extra degrees of
freedom. Our analysis shows that both considered models lead to $sim 1 sigma$
compatibility in all cases. For the involved dimensionless parameter we find
that it is constrained to an interval around zero, however the corresponding
contours are slightly shifted towards positive values. Furthermore, we use the
obtained parameter chains so to reconstruct the corresponding Hubble function,
as well as the dark-energy equation-of-state parameter, as a function of
redshift. As we show, Model 1 is very close to $Lambda$CDM scenario, while
Model 2 resembles it at low redshifts, however at earlier times deviations are
allowed. Finally, applying the AIC, BIC and the combined DIC criteria, we
deduce that both models present a very efficient fitting behavior, and are
statistically equivalent with $Lambda$CDM cosmology, despite the fact that
Model 2 does not contain the latter as a limit.
We use data from Supernovae (SNIa) Pantheon sample, from Baryonic Acoustic
Oscillations (BAO), and from cosmic chronometers measurements of the Hubble
parameter (CC), alongside arguments from Big Bang Nucleosynthesis (BBN), in
order to extract constraints on Myrzakulov $F(R,T)$ gravity. This is a
connection-based theory belonging to the Riemann-Cartan subclass, that uses a
specific but non-special connection, which then leads to extra degrees of
freedom. Our analysis shows that both considered models lead to $sim 1 sigma$
compatibility in all cases. For the involved dimensionless parameter we find
that it is constrained to an interval around zero, however the corresponding
contours are slightly shifted towards positive values. Furthermore, we use the
obtained parameter chains so to reconstruct the corresponding Hubble function,
as well as the dark-energy equation-of-state parameter, as a function of
redshift. As we show, Model 1 is very close to $Lambda$CDM scenario, while
Model 2 resembles it at low redshifts, however at earlier times deviations are
allowed. Finally, applying the AIC, BIC and the combined DIC criteria, we
deduce that both models present a very efficient fitting behavior, and are
statistically equivalent with $Lambda$CDM cosmology, despite the fact that
Model 2 does not contain the latter as a limit.
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