Constraints on inflation revisited: An analysis including the latest
  local measurement of the Hubble constant
  We revisit the constraints on inflation models by using the current
cosmological observations involving the latest local measurement of the Hubble
constant ($H_{0} = 73.00\pm 1.75$ km s $^{-1}$ Mpc$^{-1}$). We constrain the
primordial power spectra of both scalar and tensor perturbations with the
observational data including the Planck 2015 CMB full data, the BICEP2 and Keck
Array CMB B-mode data, the BAO data, and the direct measurement of $H_0$. In
order to relieve the tension between the local determination of the Hubble
constant and the other astrophysical observations, we consider the additional
parameter $N_{\rm eff}$ in the cosmological model. We find that, for the
$\Lambda$CDM+$r$+$N_{\rm eff}$ model, the scale invariance is only excluded at
the 3.3$\sigma$ level, and $\Delta N_{\rm eff}>0$ is favored at the 1.6$\sigma$
level. Comparing the obtained 1$\sigma$ and 2$\sigma$ contours of $(n_s,r)$
with the theoretical predictions of selected inflation models, we find that
both the convex and concave potentials are favored at 2$\sigma$ level, the
natural inflation model is excluded at more than 2$\sigma$ level, the
Starobinsky $R^2$ inflation model is only favored at around 2$\sigma$ level,
and the spontaneously broken SUSY inflation model is now the most favored
model.
