Probing Inflation with Large-Scale Structure Data: The Contribution of Information at Small Scales †
Abstract
:1. Introduction
- The nature of dark matter, which constitutes the bulk of the matter content.
- The component causing the accelerated expansion of the Universe. This may be a cosmological constant (, or some additional component known as dark energy, which may be dynamical, with a redshift-dependent equation of state (parametrized by some expression for w, e.g., or it may be a constant.
- Conditions in the very early Universe. The Theory of Inflation is well-established, and has been confirmed with remarkable precision by a succession of cosmic microwave background (CMB) probes. WMAP [1,2] provided conclusive evidence for inflation. Planck [3,4] conclusively excluded a scale-invariant primordial power spectrum. What is the form of this power spectrum beyond its main shape and amplitude? Does it contain features? If so, at which scales do they occur? What is the inflaton potential producing this power spectrum?
2. Primordial Physics
The Inflationary Potential
3. Method
- Simulated Planck CMB data alone (shown in red in the triangle plots);
- Joint Euclid Conservative galaxy clustering + Euclid Conservative cosmic shear + simulated Planck CMB data (shown in blue);
- Joint Euclid Realistic galaxy clustering + Euclid Realistic cosmic shear + simulated Planck CMB data (shown in green).
3.1. The Non-Linear Theoretical Uncertainty: ‘Conservative’ and ‘Realistic’ Setups
- Conservative galaxy clustering: We use a cut-off on large wavelengths at . This eliminates scales which are bigger than the bin width or which violate the small-angle approximation. On small wavelengths, we use a theoretical uncertainty with .
- Realistic galaxy clustering: The same formulation, but with
- Conservative cosmic shear: We include multipoles from up to a bin-dependent non-linear cut-off given by
- Realistic cosmic shear: the same, but with .
3.2. Fiducial Cosmology and WWI Models
4. Results
5. Conclusions
Funding
Institutional Review Board Statement
Informed Consent Statement
Data Availability Statement
Acknowledgments
Conflicts of Interest
Abbreviations
CMB | Cosmic microwave background |
CDM | cold dark matter |
MCMC | Markov chain Monte Carlo |
WMAP | Wilkinson Microwave Anisotropy Probe |
WWI | Wiggly Whipped Inflation |
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Model | |||||
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WWI: Featureless | 0 | 0 | – | – | |
WWI–A | |||||
WWI–B | |||||
WWI–C | |||||
WWI–D | |||||
WWIP: Featureless | 0 | – | – | – | |
WWIP: Planck-best-fit | – | – | |||
WWIP: Small-scale-feature | – | – |
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Debono, I. Probing Inflation with Large-Scale Structure Data: The Contribution of Information at Small Scales. Phys. Sci. Forum 2021, 2, 45. https://doi.org/10.3390/ECU2021-09371
Debono I. Probing Inflation with Large-Scale Structure Data: The Contribution of Information at Small Scales. Physical Sciences Forum. 2021; 2(1):45. https://doi.org/10.3390/ECU2021-09371
Chicago/Turabian StyleDebono, Ivan. 2021. "Probing Inflation with Large-Scale Structure Data: The Contribution of Information at Small Scales" Physical Sciences Forum 2, no. 1: 45. https://doi.org/10.3390/ECU2021-09371