Inflation model selection revisited
  We update the constraints on the power spectra of primordial curvature
perturbation and tensor perturbation including Planck data 2015 (P15) and
recently released BICEP2/Keck data (BK15), Baryon Acoustic Oscillation data and
the Type Ia supernovae data. We find that the upper limits of tensor-to-scalar
ratio are $0.061$, $0.064$ and $0.072$ at $95\%$ confidence level (CL) in the
$\Lambda$CDM+$r$, $\Lambda$CDM+$r$+$\alpha_s$ and
$\Lambda$CDM+$r$+$\alpha_s$+$\beta_s$ models respectively, where $\alpha_s$ and
$\beta_s$ are the running of scalar spectral index and running of running. The
inflation model with a concave potential is favored at more than $95\%$ CL. In
addition, parametrizing the slow-roll parameter $\epsilon\sim 1/N^p$, where $N$
is the e-folding number before the end of inflation and taken in the range of
$[50,60]$ and $[14,75]$ respectively, we conclude that the inflation model with
a monomial potential $V(\phi)\sim \phi^n$ is disfavored at more than $95\%$ CL,
and both the Starobinsky inflation model and brane inflation model are still
consistent with the data.
