Inflation model selection revisited after a 1.91% measurement of the
  Hubble constant
  The recent local measurement of the Hubble constant based on the
distance-ladder method has reached a $1.91\%$ precision, but this result is in
tension with the early-universe measurements at the more than 4$\sigma$ level,
bringing a crisis to the contemporary cosmology. In addition to the end-to-end
test of the $\Lambda$CDM model in the late universe, it is also of great
interest to see how the local $H_0$ measurement affects the determination of
the primordial power spectra, and further to test the influences for the
inflation model selection. Here, we constrain the primordial power spectra of
scalar and tensor perturbations by using a series of observational data,
including the Planck 2015 cosmic microwave background (CMB) temperature and
polarization power spectra data, the Planck 2018 lensing power spectrum data,
the BICEP2/Keck Array CMB B-mode data, and also the prior of optical depth
$\tau=0.054\pm0.007$, as well as the late-universe measurements (baryon
acoustic oscillations and type Ia supernovae). In particular, we use the latest
$1.91\%$ measurement of the Hubble constant, $H_{0}=74.03\pm1.42$ km s$^{-1}$
Mpc$^{-1}$, in this cosmological test. We find that considering the latest
local $H_{0}$ measurement in the data combination will lead to a larger fit
value of $n_{\rm s}$. With the addition of the latest local measurement of
$H_{0}$, it is found that the natural inflation model is totally excluded at
the $2\sigma$ level, the Starobinsky $R^{2}$ inflation model is marginally
favored at around the $2\sigma$ level, and the spontaneously broken SUSY
inflation model is the most favored model.
