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Exploring Early and Late Cosmology with Next Generation Surveys
Cosmology and Nongalactic Astrophysics · Submitted 21 Jan 2020
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The primordial power spectrum can be reconstructed at the subpercent level in a dozen wavenumber bins, while simultaneously fitting the sum of neutrino masses to 14 meV.
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The abstract, sentence by sentence
Perturbations from inflation evolve into large scale structure of the late universe, and encode abundant cosmic structure formation physics. We allow freedom in the primordial power spectrum, rather than assuming a power law scale dependence, to study its impact on cosmological parameter determination. Combining various generations of cosmic microwave background (CMB) data and galaxy redshift survey data, we investigate the constraints on reconstruction of the primordial curvature perturbation power spectrum and the late time cosmology, especially the sum of neutrino masses. We quantify how each successive generation, in CMB and galaxy surveys, provides significant improvements, often by factors of several. By using CMB polarization information over a broad range of angular scales, and galaxy redshift data in many bins of redshift, one can allow inflationary freedom and still constrain parameters comparably to assuming power law dependence. The primordial power spectrum can be reconstructed at the subpercent level in a dozen wavenumber bins, while simultaneously fitting the sum of neutrino masses to 14 meV.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Perturbations from inflation evolve into large scale structure of the late universe, and encode abundant cosmic structure formation physics. | background 1.00 | 0.05 | 0.03 | asserted 1.00 |
| s1 | We allow freedom in the primordial power spectrum, rather than assuming a power law scale dependence, to study its impact on cosmological parameter determination. | method 0.72 | 0.87 | 0.05 | asserted 0.85 |
| s2 | Combining various generations of cosmic microwave background (CMB) data and galaxy redshift survey data, we investigate the constraints on reconstruction of the primordial curvature perturbation power spectrum and the late time cosmology, especially the sum of neutrino masses. | contribution 0.52 | 0.92 | 0.12 | asserted 0.93 |
| s3 | We quantify how each successive generation, in CMB and galaxy surveys, provides significant improvements, often by factors of several. | result 0.94 | 0.87 | 0.12 | asserted 0.99 |
| s4 | By using CMB polarization information over a broad range of angular scales, and galaxy redshift data in many bins of redshift, one can allow inflationary freedom and still constrain parameters comparably to assuming power law dependence. | result 0.46 | 0.60 | 0.24 | hedged possibility 0.73 |
| s5 | The primordial power spectrum can be reconstructed at the subpercent level in a dozen wavenumber bins, while simultaneously fitting the sum of neutrino masses to 14 meV. | result 1.00 | 0.88 | 0.60 | asserted 0.97 |
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The paper
Original abstract
Perturbations from inflation evolve into large scale structure of the late universe, and encode abundant cosmic structure formation physics. We allow freedom in the primordial power spectrum, rather than assuming a power law scale dependence, to study its impact on cosmological parameter determination. Combining various generations of cosmic microwave background (CMB) data and galaxy redshift survey data, we investigate the constraints on reconstruction of the primordial curvature perturbation power spectrum and the late time cosmology, especially the sum of neutrino masses. We quantify how each successive generation, in CMB and galaxy surveys, provides significant improvements, often by factors of several. By using CMB polarization information over a broad range of angular scales, and galaxy redshift data in many bins of redshift, one can allow inflationary freedom and still constrain parameters comparably to assuming power law dependence. The primordial power spectrum can be reconstructed at the subpercent level in a dozen wavenumber bins, while simultaneously fitting the sum of neutrino masses to 14 meV.
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References
How the literature uses it
5 arXiv papers cite this in 6 sentences
Papers citing it · 3 sentences without a confident label
Cites it as support 2 papers
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Redshift-space maps at $z>2$ can radically improve constraints on inflation and dark energy [ref] , while at the same time relaxing assumptions such as a power-law primordial power spectrum [ref] .
A Spectroscopic Road Map for Cosmic Frontier: DESI, DESI-II, Stage-5 · Introduction · 0.97
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Models that push even further back, changing the primordial power spectrum beyond the power form, for example with oscillations or features, also have difficulty in substantially shifting $H_0$, e.g. [ref] (and will be tightly constrained by tomographic redshift surveys and future CMB experiments, e.g. [ref] ).
A Whole Cosmology View of the Hubble Constant · Early Universe Deviations · 0.98
Cites it as background 1 paper
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Several methods have been developed for model independent reconstruction of $P_ℛ(k)$ based on different inference methods, such as Bayesian inference, linear interpolation methods [ref] [ref] , combination of top hat functions [ref] , wavelet expansion of $P_ℛ(k)$ [ref] , smoothing splines [ref] , fixed wavenumber knots joined with cubic splines [ref] , the critical filter method [ref] , different spline techniques [ref] or placement of $N$ free knots in the ${k$, $P_ℛ}$ plane [ref] ; penalized likelihood, using function space generalization of the Fisher matrix formalism [ref] or a $P_ℛ(k)$ ansatz [ref] ; Principal Component Analysis, using expansion of a orthonormal set of basis functions [ref] ; and sparsity of the primordial power spectrum, using a sparsity-based linear inversion method [ref] .
Bayesian inference methodology for Primordial Power Spectrum reconstructions from Large Scale Structure · Introduction · 0.96
What it cites · 9 sentences without a confident label
Uses the method or tool of 6 papers
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For the CMB-S4 experiment we create a mock data set assuming Planck 2018 bestfit parameter values ($Ω_bh^2 = 0.02238$, $Ω_cdmh^2 = 0.1201$, $H_0 = 67.32$, $τ_reio = 0.0543$, $n_s=0.966$, $A_s=2.1 ×10^-9$, $∑=0.06$eV), and we use the mock likelihood class for this future survey introduced in [ref] (note that CMB-S4 experiment characteristics may have changed since then).
The promising future of a robust cosmological neutrino mass measurement · Next Generation Surveys · 0.98
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The matter density power spectrum $P_m$ is determined from the primordial curvature power spectrum through solution of the evolution equations within an appropriately modified version of the CLASS Boltzmann code [ref] (specifically, we generalize the initial conditions by introducing our binned PPS version in the code via the external_Pk mode feature and add a galaxy clustering likelihood module for the future data we use).
Localized correlated features in the CMB power spectrum and primordial bispectrum from a transient reduction in the speed of sound · Inflationary Freedom and Cosmology · 0.95
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The matter density power spectrum $P_m$ is determined from the primordial curvature power spectrum through solution of the evolution equations within an appropriately modified version of the CLASS Boltzmann code [ref] (specifically, we generalize the initial conditions by introducing our binned PPS version in the code via the external_Pk mode feature and add a galaxy clustering likelihood module for the future data we use).
The Cosmic Linear Anisotropy Solving System (CLASS) II: Approximation schemes · Inflationary Freedom and Cosmology · 0.95
Uses data or values from 1 paper
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We set $$ by adopting the fixed Planck 2018 [ref] values of $A_s=2.1 ×10^-9$ (which determines $(k_piv)$ according to our conventions), $n_s=0.966$, and $α_s=0$ for $k_piv=0.05 Mpc^-1$.
Planck 2018 results. VI. Cosmological parameters · Inflationary Freedom and Cosmology · 1.00
Cites as support 1 paper
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While no finite number of free variables gives complete freedom, this does give far more freedom than fixing to power law, and previous literature (e.g. [ref] ) has established that 20 bins give sufficient freedom for cases of most interest.
Inflationary Freedom and Cosmological Neutrino Constraints · Introduction · 0.99
Cites as background 29 papers
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Another research area seeks to reconstruct the primordial power spectrum from data (see, e.g., [ref] and many others).
The Simons Observatory: Science goals and forecasts · Introduction · 0.92
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Another research area seeks to reconstruct the primordial power spectrum from data (see, e.g., [ref] and many others).
Primordial power spectrum and cosmology from black-box galaxy surveys · Introduction · 0.92
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Another research area seeks to reconstruct the primordial power spectrum from data (see, e.g., [ref] and many others).
Planck 2018 results. X. Constraints on inflation · Introduction · 0.92
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