We forecast the scientific capabilities to improve our understanding of cosmic inflation of CORE, a proposed CMB space satellite submitted in response to the ESA fifth call for a medium-size mission opportunity. The CORE satellite will map the CMB anisotropies in temperature and polarization in 19 frequency channels spanning the range 60-600 GHz. CORE will have an aggregate noise sensitivity of 1.7 μKċ arcmin and an angular resolution of 5' at 200 GHz. We explore the impact of telescope size and noise sensitivity on the inflation science return by making forecasts for several instrumental configurations. This study assumes that the lower and higher frequency channels suffice to remove foreground contaminations and complements other related studies of component separation and systematic effects, which will be reported in other papers of the series "Exploring Cosmic Origins with CORE." We forecast the capability to determine key inflationary parameters, to lower the detection limit for the tensor-to-scalar ratio down to the 10-3 level, to chart the landscape of single field slow-roll inflationary models, to constrain the epoch of reheating, thus connecting inflation to the standard radiation-matter dominated Big Bang era, to reconstruct the primordial power spectrum, to constrain the contribution from isocurvature perturbations to the 10-3 level, to improve constraints on the cosmic string tension to a level below the presumptive GUT scale, and to improve the current measurements of primordial non-Gaussianities down to the fNLlocal < 1 level. For all the models explored, CORE alone will improve significantly on the present constraints on the physics of inflation. Its capabilities will be further enhanced by combining with complementary future cosmological observations.
|Original language||English (US)|
|Journal||Journal of Cosmology and Astroparticle Physics|
|State||Published - Apr 5 2018|
Bibliographical noteFunding Information:
FA is supported by the National Taiwan University (NTU) under Project No. 103R4000 and by the NTU Leung Center for Cosmology and Particle Astrophysics (LeCosPA) under Project No. FI121. KK acknowledges support by the Magnus Ehrnrooth Foundation. JV acknowledges support by the Finnish Cultural Foundation. KK and JV work is supported in part by Academy of Finland grants 257989 and 295113. CJM is supported by an FCT Research Professorship, contract reference IF/00064/2012, funded by FCT/MCTES (Portugal) and POPH/FSE (EC). Partial support by ASI/INAF Agreement 2014-024-R.1 for the Planck LFI Activity of Phase E2. The calculations in this work were performed in CSC — the IT Center for Science Ltd. (Finland), IN2P3 Computer Center (France), HPC-cluster facilities of RWTH Aachen University (Germany), INAF-IASF Bologna HPC cluster (Italy), the Cambridge COSMOS SMP system (U.K.), part of the STFC DiRAC HPC Facility supported by BIS NeI capital grant ST/J005673/1 and STFC grants ST/H008586/1, ST/K00333X/1.
© 2018 IOP Publishing Ltd and Sissa Medialab.
- CMBR theory