Cosmology and Nongalactic Astrophysics · arXiv:1003.0456 v2 · submitted 1 Mar 2010
Cosmological Parameters Degeneracies and Non-Gaussian Halo Bias
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“Thus the $f_{\rm NL}$ constraint is remarkable robust to cosmological model uncertainties.”
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Abstract
We study the impact of the cosmological parameters uncertainties on the measurements of primordial non-Gaussianity through the large-scale non-Gaussian halo bias effect. While this is not expected to be an issue for the standard LCDM model, it may not be the case for more general models that modify the large-scale shape of the power spectrum. We consider the so-called local non-Gaussianity model and forecasts from planned surveys, alone and combined with a Planck CMB prior. In particular, we consider EUCLID- and LSST-like surveys and forecast the correlations among $f_{\rm NL}$ and the running of the spectral index αs, the dark energy equation of state w, the effective sound speed of dark energy perturbations c2s, the total mass of massive neutrinos Mν = ∑mν, and the number of extra relativistic degrees of freedom Nνrel. Neglecting CMB information on $f_{\rm NL}$ and scales k > 0.03h/Mpc, we find that, if $N_\nu^{\rm rel}$ is assumed to be known, the uncertainty on cosmological parameters increases the error on $f_{\rm NL}$ by 10 to 30% depending on the survey. Thus the $f_{\rm NL}$ constraint is remarkable robust to cosmological model uncertainties. On the other hand, if $N_\nu^{\rm rel}$ is simultaneously constrained from the data, the $f_{\rm NL}$ error increases by $\sim 80%$. Finally, future surveys which provide a large sample of galaxies or galaxy clusters over a volume comparable to the Hubble volume can measure primordial non-Gaussianity of the local form with a marginalized 1–σ error of the order $\Delta f_{\rm NL} \sim 2-5$, after combination with CMB priors for the remaining cosmological parameters. These results are competitive with CMB bispectrum constraints achievable with an ideal CMB experiment.
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abstract compiled · 2026-09-23 · no language-model review
How the main claim is stated: asserted 1.00
What the abstract itself states, as probabilities: claims first 0.02 · states limitation 0.76 · human participants 0.01 · controlled comparison 0.19 · randomized assignment 0.01 · states quantitative result 0.99 · compares with prior results 0.91 · mentions code or data availability 0.02
The abstract, sentence by sentence
This table labels the abstract only (arXiv listing abstract v2). The number is the probability the classifier gave the label.
| Sentence | Role | The authors' own work | States the main conclusion | Strength |
|---|---|---|---|---|
| We study the impact of the cosmological parameters uncertainties on the measurements of primordial non-Gaussianity through the large-scale non-Gaussian halo bias effect. | contribution 0.98 | 0.81 | 0.05 | asserted 0.80 |
| While this is not expected to be an issue for the standard LCDM model, it may not be the case for more general models that modify the large-scale shape of the power spectrum. | background 0.89 | 0.07 | 0.04 | hedged possibility 0.96 |
| We consider the so-called local non-Gaussianity model and forecasts from planned surveys, alone and combined with a Planck CMB prior. | method 0.90 | 0.75 | 0.03 | asserted 0.91 |
| In particular, we consider EUCLID- and LSST-like surveys and forecast the correlations among $f_{\rm NL}$ and the running of the spectral index $\alpha_s$, the dark energy equation of state $w$, the effective sound speed of dark energy perturbations $c^2_s$, the total mass of massive neutrinos $M_\nu=\sum m_\nu$, and the number of extra relativistic degrees of freedom $N_\nu^{rel}$. | method 0.81 | 0.80 | 0.04 | asserted 0.90 |
| Neglecting CMB information on $f_{\rm NL}$ and scales $k > 0.03 h$/Mpc, we find that, if $N_\nu^{\rm rel}$ is assumed to be known, the uncertainty on cosmological parameters increases the error on $f_{\rm NL}$ by 10 to 30% depending on the survey. | result 1.00 | 0.95 | 0.16 | asserted 1.00 |
| Thus the $f_{\rm NL}$ constraint is remarkable robust to cosmological model uncertainties. | interpretation 0.89 | 0.80 | 0.34 | asserted 1.00 |
| On the other hand, if $N_\nu^{\rm rel}$ is simultaneously constrained from the data, the $f_{\rm NL}$ error increases by $\sim 80%$. | result 1.00 | 0.91 | 0.14 | asserted 1.00 |
| Finally, future surveys which provide a large sample of galaxies or galaxy clusters over a volume comparable to the Hubble volume can measure primordial non-Gaussianity of the local form with a marginalized 1--$\sigma$ error of the order $\Delta f_{\rm NL} \sim 2-5$, after combination with CMB priors for the remaining cosmological parameters. | result 1.00 | 0.86 | 0.34 | asserted 0.76 |
| These results are competitive with CMB bispectrum constraints achievable with an ideal CMB experiment. | interpretation 0.87 | 0.70 | 0.16 | asserted 0.97 |
What kind of paper the classifier reports this is: simulation study 0.59 · evidence from simulation or computation 0.97
What was examined, and what was not
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- arXiv listing abstract v2
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Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 7,318 input tokens, $0.0003 reported.
Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. This record as JSON
Cited by 12 Pith papers
Reviewed papers on Pith that cite this one. The full citation record
- Primordial Non-Gaussianity from Biased Tracers: Likelihood Analysis of Real-Space Power Spectrum and Bispectrum astro-ph.CO · Oct 2020
- Exploring KSZ velocity reconstruction with $N$-body simulations and the halo model astro-ph.CO · Oct 2020
- Reconstructing the Inflationary Landscape with Cosmological Data astro-ph.CO · Jun 2018
- The Halo Bispectrum in N-body Simulations with non-Gaussian Initial Conditions astro-ph.CO · Nov 2011
- Optimal Constraints on Local Primordial Non-Gaussianity from the Two-Point Statistics of Large-Scale Structure astro-ph.CO · Apr 2011
- N-body simulations with generic non-Gaussian initial conditions II: Halo bias astro-ph.CO · Feb 2011
- Sloan Digital Sky Survey III Photometric Quasar Clustering: Probing the Initial Conditions of the Universe using the Largest Volume astro-ph.CO · Nov 2013
- Cosmological Parameter Estimation with Large Scale Structure Observations astro-ph.CO · Aug 2013
- Improved Primordial Non-Gaussianity Constraints from Measurements of Galaxy Clustering and the Integrated Sachs-Wolfe Effect astro-ph.CO · Mar 2013
- Prospects for constraining the shape of non-Gaussianity with the scale-dependent bias astro-ph.CO · Apr 2012
- Effects and Detectability of Quasi-Single Field Inflation in the Large-Scale Structure and Cosmic Microwave Background astro-ph.CO · Apr 2012
- Cosmology and Fundamental Physics with the Euclid Satellite astro-ph.CO · Jun 2016
How the literature uses it
18 arXiv papers cite this in 28 sentences
Papers citing it · 22 sentences without a confident label
Builds on it 1 paper
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This corresponds to the second example of [ref] , although with a lower (therefore more conservative) fiducial value for the linear bias.
Effects and Detectability of Quasi-Single Field Inflation in the Large-Scale Structure and Cosmic Microwave Background · Fisher matrix · 0.95
Uses its data or values 1 paper
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Future full-sky galaxy surveys might achieve an accuracy of $Δf^local_NL ∼1-5$ (68% CL) [ref] and Planck is expected to achieve $Δτ^local_NL ∼560$ (95% CL) [ref] .
Optimizing future experimental probes of inflation · Non-Gaussianity · 0.83
Cites it as support 1 paper
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This will cause to a simultaneous effect between cosmological parameters and primordial NG [ref] worth to study in detail.
Simultaneous effect of Modified Gravity and Primordial Non-Gaussianity in Large Scale Structure Observations · INTRODUCTION · 0.96
Cites it as background 3 papers
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There are several studies forecasting constraints on primordial non-Gaussianity through the scale-dependent galaxy bias (e.g., [ref] ).
Magnification effect on the detection of primordial non-Gaussianity from photometric surveys · Introduction · 0.94
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The detectability of the bias correction, both in galaxy and cluster surveys, has also been the subject of several works in recent years [ref] .
Effects and Detectability of Quasi-Single Field Inflation in the Large-Scale Structure and Cosmic Microwave Background · Introduction · 0.99
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In the remainder of the present work we shall therefore not address the interesting question of bias, see e.g. [ref] .
Cosmological Parameter Estimation with Large Scale Structure Observations · Number counts versus the real space power spectrum · 0.83
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