Cosmological constraints on slow-roll inflation: an update. (arXiv:2110.01695v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Forconi_M/0/1/0/all/0/1">Matteo Forconi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giare_W/0/1/0/all/0/1">William Giar&#xe8;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valentino_E/0/1/0/all/0/1">Eleonora Di Valentino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Melchiorri_A/0/1/0/all/0/1">Alessandro Melchiorri</a>

In light of the most recent cosmological observations, we provide new updated
constraints on the slow-roll inflation in different extended scenarios beyond
the $Lambdarm{CDM}$ cosmological model. Along with the usual six parameters,
we simultaneously vary different combinations of additional parameters,
including the running of the scalar spectral index $alpha_s$, its running of
running $beta_s$, the tensor amplitude $r$ and the spatial curvature
$Omega_k$. From the Planck 2018 data, we find no evidence for a scalar running
or a running of running, while analyzing the Atacama Cosmology Telescope data
combined with WMAP 9-years observations data we find a preference for non-zero
$alpha_s$ and $beta_s$ at the level of 2.9$sigma$ and 2.7$sigma$,
respectively. Anyway, this preference is reduced when the tensor amplitude can
vary in the model or $beta_s$ is fixed to zero. The upper bound on $r$ is only
slightly affected by the additional parameters while the differences in the
datasets can remarkably change the compatibility among the different
inflationary models, sometimes leading to discordant conclusions.

In light of the most recent cosmological observations, we provide new updated
constraints on the slow-roll inflation in different extended scenarios beyond
the $Lambdarm{CDM}$ cosmological model. Along with the usual six parameters,
we simultaneously vary different combinations of additional parameters,
including the running of the scalar spectral index $alpha_s$, its running of
running $beta_s$, the tensor amplitude $r$ and the spatial curvature
$Omega_k$. From the Planck 2018 data, we find no evidence for a scalar running
or a running of running, while analyzing the Atacama Cosmology Telescope data
combined with WMAP 9-years observations data we find a preference for non-zero
$alpha_s$ and $beta_s$ at the level of 2.9$sigma$ and 2.7$sigma$,
respectively. Anyway, this preference is reduced when the tensor amplitude can
vary in the model or $beta_s$ is fixed to zero. The upper bound on $r$ is only
slightly affected by the additional parameters while the differences in the
datasets can remarkably change the compatibility among the different
inflationary models, sometimes leading to discordant conclusions.

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