arXiv Analytics

Sign in

arXiv:1912.00995 [astro-ph.CO]AbstractReferencesReviewsResources

How much primordial tensor mode is allowed?

Moumita Aich, Yin-Zhe Ma, Wei-Ming Dai, Jun-Qing Xia

Published 2019-12-02Version 1

The presence of a significant amount of gravitational radiation in the early Universe affects the total energy density and hence the expansion rate in the early epoch. In this work, we develop a physical model to connect the parameter of relativistic degree of freedom $N_\mathrm{eff}$ with the amplitude and shape of primordial tensor power spectrum, and use the CMB temperature and polarization data from {\it Planck} and BICEP2/KECK Array, and the primordial deuterium measurement from damped Lyman-$\alpha$ (DLA) systems to constrain this model. We find that with this extra relation $\Delta N_{\rm eff}(r,n_{\rm t})$, the tensor-to-scalar ratio $r$ is constrained to be $r<0.07$ ($3\sigma$ C.L.) and the tilt of tensor power spectrum is $n_\mathrm{t}=-0.01\pm 0.31$ ($1\sigma$ C.L.) for {\it Planck}+BICEP2+KECK+[D/H] data. This achieves a much tighter constraint on the tensor spectrum and provides a stringent test for cosmic inflation models. In addition, the current constraint on $N_{\rm eff}=3.122 \pm 0.171$ excludes the possibility of fourth neutrino species at more than $5\sigma$ C.L.

Related articles: Most relevant | Search more
arXiv:1612.09253 [astro-ph.CO] (Published 2016-12-29)
Scale invariance of the primordial tensor power spectrum
arXiv:1810.04572 [astro-ph.CO] (Published 2018-10-10)
Eigen-reconstruction of Perturbations to the Primordial Tensor Power Spectrum
arXiv:1905.08200 [astro-ph.CO] (Published 2019-05-20)
Principal component analysis of the primordial tensor power spectrum