Inferences for f(R) Models from Late-Time Megamaser Observational Data

In this work, we study three widely used models of f® gravity, namely HuSawicki, Starobinsky and ArcTanh along with the standard cosmology model ($\mathrm{\Lambda }$CDM). For this, we employ the megamaser angular diameter distance and velocity measurements from the Megamaser Cosmology Project, which provide a purely geometric determination of the Hubble constant. We constrain the parameters using the Markov Chain Monte Carlo method. Our results show that values of the Hubble Constant, $H_0$, obtained for all four models are in concordance with its value obtained from other late-time observational data such as SNe Ia. The constraints on $H_0$ in all the models under study are restrictive and the marginalized estimates lie close to 73 $\mathrm{k}\mathrm{m}{\mathrm{s}}^{-1}\mathrm{M}\mathrm{p}{\mathrm{c}}^{-1}$. The marginalized estimates of the deviation parameter, b, for the three f® gravity models lie close to zero. This late-time dataset, thus predicts that f® models mimic $\mathrm{\Lambda }$CDM. However, the matter density, ${\mathrm{\Omega }}_m$, remains weakly constrained for all the models with its marginalized estimate close to 0.5. Further, comparison of the four models (f® models and $\mathrm{\Lambda }$CDM) using information criteria such as Akaike Information Criterion and Bayesian Information Criterion shows that within current uncertainties, the dataset finds f® models statistically indistinguishable from $\mathrm{\Lambda }$CDM. This is consistent with the fact that the favoured value of b for each of the f® models lies close to zero.